Author name code: magain
ADS astronomy entries on 2022-09-14
author:"Magain, Pierre" 
------------------------------------------------------------------------  

Title: COSMOGRAIL. XIX. Time delays in 18 strongly lensed quasars
    from 15 years of optical monitoring
Authors: Millon, M.; Courbin, F.; Bonvin, V.; Paic, E.; Meylan, G.;
   Tewes, M.; Sluse, D.; Magain, P.; Chan, J. H. H.; Galan, A.; Joseph,
   R.; Lemon, C.; Tihhonova, O.; Anderson, R. I.; Marmier, M.; Chazelas,
   B.; Lendl, M.; Triaud, A. H. M. J.; Wyttenbach, A.
Bibcode: 2020A&A...640A.105M
Altcode: 2020arXiv200205736M
  We present the results of 15 years of monitoring lensed quasars, which
  was conducted by the COSMOGRAIL programme at the Leonhard Euler 1.2
  m Swiss Telescope. The decade-long light curves of 23 lensed systems
  are presented for the first time. We complement our data set with
  other monitoring data available in the literature to measure the time
  delays in 18 systems, among which nine reach a relative precision
  better than 15% for at least one time delay. To achieve this, we
  developed an automated version of the curve-shifting toolbox PyCS
  to ensure robust estimation of the time delay in the presence of
  microlensing, while accounting for the errors due to the imperfect
  representation of microlensing. We also re-analysed the previously
  published time delays of RX J1131-1231 and HE 0435-1223, by adding
  six and two new seasons of monitoring, respectively, and confirming
  the previous time-delay measurements. When the time delay measurement
  is possible, we corrected the light curves of the lensed images from
  their time delay and present the difference curves to highlight the
  microlensing signal contained in the data. To date, this is the largest
  sample of decade-long lens monitoring data, which is useful to measure
  H<SUB>0</SUB> and the size of quasar accretion discs with microlensing
  as well as to study quasar variability. <P />All light curves presented
  in this paper are only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/640/A105">http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/640/A105</A>

Title: VizieR Online Data Catalog: R-band light curves of 23 lensed
    QSOs (Millon+, 2020)
Authors: Millon, M.; Courbin, F.; Bonvin, V.; Paic, E.; Meylan, G.;
   Tewes, M.; Sluse, D.; Magain, P.; Chan, J. H. H.; Galan, A.; Joseph,
   R.; Lemon, C.; Tihhonova, O.; Anderson, R. I.; Marmier, M.; Chazelas,
   B.; Lendl, M.; Triaud, A. H. M. J.; Wyttenbach, A.
Bibcode: 2020yCat..36400105M
Altcode:
  R-band cosmograil light curves of lensed quasars taken at the Euler 1.2m
  Swiss telescope with the EulerCAM and EulerC2 instrument. Additional
  data taken at the SMARTS 1.3m telescope with the ANDICAM optical/
  infrared camera are also included for SDSS J0924+0219 (MacLeod et
  al., 2015ApJ...806..258M, Cat. J/ApJ/806/258). <P />For HE 0435-1223
  and RX J1131-1231, data taken at the 1.5m telescope at the Maidanak
  Observatory, the Mercator Belgian telescope and at the SMARTS 1.3
  m telescope are included (Courbin et al. 2011A&amp;A...536A..53C,
  Cat, J/A+A/536/A53, Tewes et al. 2013A&amp;A...553A.120T,
  2013A&amp;A...556A..22T, Cat. J/A+A/556/A22). For SDSS J1515+1511,
  we had the data from Shalyapin &amp; Goicoechea (2017ApJ...836...14S)
  from the Liverpool Telescope. <P />(5 data files).

Title: COSMOGRAIL. XVII. Time delays for the quadruply imaged quasar
    PG 1115+080
Authors: Bonvin, V.; Chan, J. H. H.; Millon, M.; Rojas, K.; Courbin,
   F.; Chen, G. C. -F.; Fassnacht, C. D.; Paic, E.; Tewes, M.; Chao,
   D. C. -Y.; Chijani, M.; Gilman, D.; Gilmore, K.; Williams, P.;
   Buckley-Geer, E.; Frieman, J.; Marshall, P. J.; Suyu, S. H.; Treu,
   T.; Hempel, A.; Kim, S.; Lachaume, R.; Rabus, M.; Anguita, T.; Meylan,
   G.; Motta, V.; Magain, P.
Bibcode: 2018A&A...616A.183B
Altcode: 2018arXiv180409183B
  We present time-delay estimates for the quadruply imaged quasar PG
  1115+080. Our results are based on almost daily observations for
  seven months at the ESO MPIA 2.2 m telescope at La Silla Observatory,
  reaching a signal-to-noise ratio of about 1000 per quasar image. In
  addition, we re-analyze existing light curves from the literature
  that we complete with an additional three seasons of monitoring with
  the Mercator telescope at La Palma Observatory. When exploring the
  possible source of bias we considered the so-called microlensing
  time delay, a potential source of systematic error so far never
  directly accounted for in previous time-delay publications. In
  15 yr of data on PG 1115+080, we find no strong evidence of
  microlensing time delay. Therefore not accounting for this effect,
  our time-delay estimates on the individual data sets are in good
  agreement with each other and with the literature. Combining the
  data sets, we obtain the most precise time-delay estimates to date
  on PG 1115+080, with Δt(AB) = 8.3<SUP>+1.5</SUP><SUB>-1.6</SUB>
  days (18.7% precision), Δt(AC) = 9.9<SUP>+1.1</SUP><SUB>-1.1</SUB>
  days (11.1%) and Δt(BC) = 18.8<SUP>+1.6</SUP><SUB>-1.6</SUB> days
  (8.5%). Turning these time delays into cosmological constraints
  is done in a companion paper that makes use of ground-based
  Adaptive Optics (AO) with the Keck telescope. <P />Lightcurve
  data points are only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/616/A183">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/616/A183</A>

Title: A cosmology-independent calibration of Type Ia supernovae data
Authors: Hauret, C.; Magain, P.; Biernaux, J.
Bibcode: 2018MNRAS.479.3996H
Altcode: 2018arXiv180610900H; 2018MNRAS.tmp.1635H
  Recently, the common methodology used to transform Type Ia
  supernovae (SNe Ia) into genuine standard candles has been suffering
  criticism. Indeed, it assumes a particular cosmological model [namely
  the flat Λ cold dark matter (ΛCDM)] to calibrate the standardization
  corrections parameters, i.e. the dependence of the supernova peak
  absolute magnitude on its colour, post-maximum decline rate and host
  galaxy mass. As a result, this assumption could make the data compliant
  to the assumed cosmology and thus nullify all works previously conducted
  on model comparison. In this work, we verify the viability of these
  hypotheses by developing a cosmology-independent approach to standardize
  SNe Ia data from the recent JLA compilation. Our resulting corrections
  turn out to be very close to the ΛCDM-based corrections. Therefore,
  even if a ΛCDM-based calibration is questionable from a theoretical
  point of view, the potential compliance of SNe Ia data does not happen
  in practice for the JLA compilation. Previous works of model comparison
  based on these data do not have to be called into question. However,
  as this cosmology-independent standardization method has the same
  degree of complexity than the model-dependent one, it is worth using
  it in future works, especially if smaller samples are considered,
  such as the superluminous Type Ic supernovae.

Title: VizieR Online Data Catalog: R-band light curves of PG 1115+080
    (Bonvin+, 2018)
Authors: Bonvin, V.; Chan, J. H. H.; Millon, M.; Rojas, K.; Courbin,
   F.; Chen, G. C. -F.; Fassnacht, C. D.; Paic, E.; Tewes, M.; Chao,
   D. C. -Y.; Chijani, M.; Gilman, D.; Gilmore, K.; Williams, P.;
   Buckley-Geer, E.; Frieman, J.; Marshall, P. J.; Suyu, S. H.; Treu,
   T.; Hempel, A.; Kim, S.; Lachaume, R.; Rabus, M.; Anguita, T.; Meylan,
   G.; Motta, V.; Magain, P.
Bibcode: 2018yCat..36160183B
Altcode:
  We have been monitoring the quadruply lensed quasar PG1115+080 for 8
  months in the R band (~600-720nm) using the MPIA/ESO 2.2m telescope. The
  resulting R-band light curves of the quadruply lensed quasar PG1115+080,
  is displayed in Fig. 2 of the paper. <P />(1 data file).

Title: High-precision multiwavelength eclipse photometry of the
    ultra-hot gas giant exoplanet WASP-103 b
Authors: Delrez, L.; Madhusudhan, N.; Lendl, M.; Gillon, M.; Anderson,
   D. R.; Neveu-VanMalle, M.; Bouchy, F.; Burdanov, A.; Collier-Cameron,
   A.; Demory, B. -O.; Hellier, C.; Jehin, E.; Magain, P.; Maxted,
   P. F. L.; Queloz, D.; Smalley, B.; Triaud, A. H. M. J.
Bibcode: 2018MNRAS.474.2334D
Altcode: 2017arXiv171102566D
  We present 16 occultation and three transit light curves for the
  ultra-short period hot Jupiter WASP-103b, in addition to five new radial
  velocity measurements. We combine these observations with archival
  data and perform a global analysis of the resulting extensive data
  set, accounting for the contamination from a nearby star. We detect
  the thermal emission of the planet in both the z<SUP>΄</SUP> and
  K<SUB>S</SUB> bands, the measured occultation depths being 699±110
  ppm (6.4σ) and 3567_{-350}^{+400} ppm (10.2σ), respectively. We use
  these two measurements, together with recently published HST/WFC3 data,
  to derive joint constraints on the properties of WASP-103b's dayside
  atmosphere. On one hand, we find that the z<SUP>΄</SUP> band and
  WFC3 data are best fit by an isothermal atmosphere at 2900 K or an
  atmosphere with a low H<SUB>2</SUB>O abundance. On the other hand,
  we find an unexpected excess in the K<SUB>S</SUB> band measured flux
  compared to these models, which requires confirmation with additional
  observations before any interpretation can be given. From our global
  data analysis, we also derive a broad-band optical transmission spectrum
  that shows a minimum around 700 nm and increasing values towards both
  shorter and longer wavelengths. This is in agreement with a previous
  study based on a large fraction of the archival transit light curves
  used in our analysis. The unusual profile of this transmission spectrum
  is poorly matched by theoretical spectra and is not confirmed by more
  recent observations at higher spectral resolution. Additional data,
  in both emission and transmission, are required to better constrain
  the atmospheric properties of WASP-103b.

Title: Analysis of luminosity distributions of strong lensing
galaxies: subtraction of diffuse lensed signal
Authors: Biernaux, J.; Magain, P.; Hauret, C.
Bibcode: 2017A&A...604A..46B
Altcode: 2017arXiv170502282B
  Context. Strong gravitational lensing gives access to the total mass
  distribution of galaxies. It can unveil a great deal of information
  about the lenses' dark matter content when combined with the study of
  the lenses' light profile. However, gravitational lensing galaxies,
  by definition, appear surrounded by lensed signal, both point-like and
  diffuse, that is irrelevant to the lens flux. Therefore, the observer is
  most often restricted to studying the innermost portions of the galaxy,
  where classical fitting methods show some instabilities. <BR /> Aims: We
  aim at subtracting that lensed signal and at characterising some lenses'
  light profile by computing their shape parameters (half-light radius,
  ellipticity, and position angle). Our objective is to evaluate the total
  integrated flux in an aperture the size of the Einstein ring in order
  to obtain a robust estimate of the quantity of ordinary (luminous)
  matter in each system. <BR /> Methods: We are expanding the work we
  started in a previous paper that consisted in subtracting point-like
  lensed images and in independently measuring each shape parameter. We
  improve it by designing a subtraction of the diffuse lensed signal,
  based only on one simple hypothesis of symmetry. We apply it to the
  cases where it proves to be necessary. This extra step improves our
  study of the shape parameters and we refine it even more by upgrading
  our half-light radius measurement method. We also calculate the impact
  of our specific image processing on the error bars. <BR /> Results:
  The diffuse lensed signal subtraction makes it possible to study a
  larger portion of relevant galactic flux, as the radius of the fitting
  region increases by on average 17%. We retrieve new half-light radii
  values that are on average 11% smaller than in our previous work,
  although the uncertainties overlap in most cases. This shows that not
  taking the diffuse lensed signal into account may lead to a significant
  overestimate of the half-light radius. We are also able to measure
  the flux within the Einstein radius and to compute secure error bars
  to all of our results.

Title: Cosmological Time, Entropy and Infinity
Authors: Hauret, Clémentine; Magain, Pierre; Biernaux, Judith
Bibcode: 2017Entrp..19..357H
Altcode:
  Time is a parameter playing a central role in our most fundamental
  modelling of natural laws. Relativity theory shows that the comparison
  of times measured by different clocks depends on their relative
  motion and on the strength of the gravitational field in which they
  are embedded. In standard cosmology, the time parameter is the one
  measured by fundamental clocks (i.e., clocks at rest with respect
  to the expanding space). This proper time is assumed to flow at a
  constant rate throughout the whole history of the universe. We make
  the alternative hypothesis that the rate at which the cosmological time
  flows depends on the dynamical state of the universe. In thermodynamics,
  the arrow of time is strongly related to the second law, which states
  that the entropy of an isolated system will always increase with time
  or, at best, stay constant. Hence, we assume that the time measured
  by fundamental clocks is proportional to the entropy of the region
  of the universe that is causally connected to them. Under that simple
  assumption, we find it possible to build toy cosmological models that
  present an acceleration of their expansion without any need for dark
  energy while being spatially closed and finite, avoiding the need to
  deal with infinite values.

Title: A seven-planet resonant chain in TRAPPIST-1
Authors: Luger, Rodrigo; Sestovic, Marko; Kruse, Ethan; Grimm, Simon
   L.; Demory, Brice-Olivier; Agol, Eric; Bolmont, Emeline; Fabrycky,
   Daniel; Fernandes, Catarina S.; Van Grootel, Valérie; Burgasser,
   Adam; Gillon, Michaël; Ingalls, James G.; Jehin, Emmanuël; Raymond,
   Sean N.; Selsis, Franck; Triaud, Amaury H. M. J.; Barclay, Thomas;
   Barentsen, Geert; Howell, Steve B.; Delrez, Laetitia; de Wit, Julien;
   Foreman-Mackey, Daniel; Holdsworth, Daniel L.; Leconte, Jérémy;
   Lederer, Susan; Turbet, Martin; Almleaky, Yaseen; Benkhaldoun, Zouhair;
   Magain, Pierre; Morris, Brett M.; Heng, Kevin; Queloz, Didier
Bibcode: 2017NatAs...1E.129L
Altcode: 2017NatAs...1..129L; 2017arXiv170304166L
  The TRAPPIST-1 system is the first transiting planet system found
  orbiting an ultracool dwarf star<SUP> 1 </SUP>. At least seven planets
  similar in radius to Earth were previously found to transit this host
  star<SUP> 2 </SUP>. Subsequently, TRAPPIST-1 was observed as part of
  the K2 mission and, with these new data, we report the measurement
  of an 18.77 day orbital period for the outermost transiting planet,
  TRAPPIST-1 h, which was previously unconstrained. This value matches
  our theoretical expectations based on Laplace relations<SUP> 3 </SUP>
  and places TRAPPIST-1 h as the seventh member of a complex chain, with
  three-body resonances linking every member. We find that TRAPPIST-1 h
  has a radius of 0.752 R <SUB>⊕</SUB> and an equilibrium temperature of
  173 K. We have also measured the rotational period of the star to be
  3.3 days and detected a number of flares consistent with a low-activity,
  middle-aged, late M dwarf.

Title: Seven temperate terrestrial planets around the nearby ultracool
    dwarf star TRAPPIST-1
Authors: Gillon, Michaël; Triaud, Amaury H. M. J.; Demory,
   Brice-Olivier; Jehin, Emmanuël; Agol, Eric; Deck, Katherine M.;
   Lederer, Susan M.; de Wit, Julien; Burdanov, Artem; Ingalls, James
   G.; Bolmont, Emeline; Leconte, Jeremy; Raymond, Sean N.; Selsis,
   Franck; Turbet, Martin; Barkaoui, Khalid; Burgasser, Adam; Burleigh,
   Matthew R.; Carey, Sean J.; Chaushev, Aleksander; Copperwheat, Chris
   M.; Delrez, Laetitia; Fernandes, Catarina S.; Holdsworth, Daniel L.;
   Kotze, Enrico J.; Van Grootel, Valérie; Almleaky, Yaseen; Benkhaldoun,
   Zouhair; Magain, Pierre; Queloz, Didier
Bibcode: 2017Natur.542..456G
Altcode: 2017arXiv170301424G
  One aim of modern astronomy is to detect temperate,
  Earth-like exoplanets that are well suited for atmospheric
  characterization. Recently, three Earth-sized planets were detected
  that transit (that is, pass in front of) a star with a mass just eight
  per cent that of the Sun, located 12 parsecs away. The transiting
  configuration of these planets, combined with the Jupiter-like size of
  their host star—named TRAPPIST-1—makes possible in-depth studies of
  their atmospheric properties with present-day and future astronomical
  facilities. Here we report the results of a photometric monitoring
  campaign of that star from the ground and space. Our observations
  reveal that at least seven planets with sizes and masses similar to
  those of Earth revolve around TRAPPIST-1. The six inner planets form
  a near-resonant chain, such that their orbital periods (1.51, 2.42,
  4.04, 6.06, 9.1 and 12.35 days) are near-ratios of small integers. This
  architecture suggests that the planets formed farther from the star
  and migrated inwards. Moreover, the seven planets have equilibrium
  temperatures low enough to make possible the presence of liquid water
  on their surfaces.

Title: Red worlds: Spitzer exploration of a compact system of
    temperate terrestrial planets transiting a nearby Jupiter-sized star
Authors: Gillon, Michael; Burdanov, Artem; Delrez, Laetitia; Jehin,
   Emmanuel; Magain, Pierre; Van Grootel, Valerie; Bolmont, Emeline;
   Leconte, Jeremy; Raymond, Sean; Selsis, Franck; Demory, Brice-Olivier;
   Queloz, Didier; Triaud, Amaury; de Wit, Julien; Burgasser, Adam;
   Carey, Sean; Ingalls, Jim; Lederer, Sue; Agol, Eric; Deck, Katherine
Bibcode: 2016sptz.prop13067G
Altcode:
  The recently detected TRAPPIST-1 planetary system represents a unique
  opportunity to extend the nascent field of comparative exoplanetology
  into the realm of temperate terrestrial worlds. It is composed of at
  least three Earth-sized planets similar in sizes and irradiations to
  Earth and Venus transiting an ultra-cool dwarf star only 39 light-years
  away. Thanks to the Jupiter-size and infrared brightness of their host
  star, the planets are amenable for detailed atmospheric characterization
  with JWST, including for biosignatures detection. Our Spitzer
  Exploration Science Program aims to prepare and optimize the detailed
  study of this fascinating planetary system through the two following
  complementary sub-programs: (1) a 480 hrs continuous monitoring of
  the star to explore its full inner system up to its ice line in a
  search for any other transiting object(s) (planet, moon, Trojan) with a
  sensitivity high enough to detect any body as small as Ganymede, and (2)
  the observation of ~130 transits of the planets (520 hrs). This second
  part has two goals. First, to measure precisely the planets' masses
  and eccentricities through the Transit Timing Variations method, to
  constrain strongly their compositions and energy budgets. Secondly, to
  measure with an extremely high precision the planets' effective radii at
  4.5 microns to assess, when combined with future HST/WFC3 observations,
  the presence of an atmosphere around them. The two complementary parts
  of this program will make it a long-lasting legacy of Spitzer to the
  fields of comparative exoplanetology and astrobiology, by providing
  the necessary measurements on the inner system of TRAPPIST-1 (complete
  census, masses, eccentricities, first insights on atmospheres) required
  to initiate and optimize the detailed atmospheric characterization
  of its different components with JWST and other future facilities. <P
  />Data from program 13175 can also be found in this program.

Title: Variable time flow as an alternative to dark energy
Authors: Magain, Pierre; Hauret, Clémentine
Bibcode: 2016arXiv160606169M
Altcode:
  Time is a parameter playing a central role in our most fundamental
  modelling of natural laws. Relativity theory shows that the comparison
  of times measured by different clocks depends on their relative
  motions and on the strength of the gravitational field in which they
  are embedded. In standard cosmology, the time parameter is the one
  measured by fundamental clocks, i.e. clocks at rest with respect to the
  expanding space. This proper time is assumed to flow at a constant rate
  throughout the whole history of the Universe. We make the alternative
  hypothesis that the rate at which cosmological time flows depends on the
  global geometric curvature the Universe. Using a simple one-parameter
  model for the relation between proper time and curvature, we build
  a cosmological model that fits the Type Ia Supernovae data (the best
  cosmological standard candles) without the need for dark energy nor
  probably exotic dark matter.

Title: Temperate Earth-sized planets transiting a nearby ultracool
    dwarf star
Authors: Gillon, Michaël; Jehin, Emmanuël; Lederer, Susan M.; Delrez,
   Laetitia; de Wit, Julien; Burdanov, Artem; Van Grootel, Valérie;
   Burgasser, Adam J.; Triaud, Amaury H. M. J.; Opitom, Cyrielle; Demory,
   Brice-Olivier; Sahu, Devendra K.; Bardalez Gagliuffi, Daniella;
   Magain, Pierre; Queloz, Didier
Bibcode: 2016Natur.533..221G
Altcode: 2016arXiv160507211G
  Star-like objects with effective temperatures of less than
  2,700 kelvin are referred to as ‘ultracool dwarfs’. This
  heterogeneous group includes stars of extremely low mass as well
  as brown dwarfs (substellar objects not massive enough to sustain
  hydrogen fusion), and represents about 15 per cent of the population
  of astronomical objects near the Sun. Core-accretion theory predicts
  that, given the small masses of these ultracool dwarfs, and the
  small sizes of their protoplanetary disks, there should be a large
  but hitherto undetected population of terrestrial planets orbiting
  them—ranging from metal-rich Mercury-sized planets to more hospitable
  volatile-rich Earth-sized planets. Here we report observations of
  three short-period Earth-sized planets transiting an ultracool dwarf
  star only 12 parsecs away. The inner two planets receive four times
  and two times the irradiation of Earth, respectively, placing them
  close to the inner edge of the habitable zone of the star. Our data
  suggest that 11 orbits remain possible for the third planet, the most
  likely resulting in irradiation significantly less than that received
  by Earth. The infrared brightness of the host star, combined with its
  Jupiter-like size, offers the possibility of thoroughly characterizing
  the components of this nearby planetary system.

Title: Long-term activity and outburst of comet C/2013 A1 (Siding
    Spring) from narrow-band photometry and long-slit spectroscopy
Authors: Opitom, C.; Guilbert-Lepoutre, A.; Jehin, E.; Manfroid,
   J.; Hutsemékers, D.; Gillon, M.; Magain, P.; Roberts-Borsani, G.;
   Witasse, O.
Bibcode: 2016A&A...589A...8O
Altcode: 2015arXiv151007514O
  We present a unique data set of more than one year's worth of regular
  observations of comet C/2013 A1(Siding Spring) taken with TRAPPIST,
  along with low-resolution spectra obtained with the ESO/VLT FORS 2
  instrument. The comet made a close approach to Mars on October 19,
  2014, and was then observed by many space-borne and ground-based
  telescopes. We followed the evolution of the OH, NH, CN, C<SUB>3</SUB>,
  and C<SUB>2</SUB> production rates as well as the Afρ parameter,
  a proxy for the dust production. We detected an outburst two weeks
  after perihelion, with gas and dust production rates increased by a
  factor of five within a few days. By modelling the shape of the CN
  and C<SUB>2</SUB> radial profiles, we determined that the outburst
  happened on November 10 around 15:30 UT (±5 h) and measured a gas
  expansion velocity of 1.1 ± 0.2 km s<SUP>-1</SUP>. We used a thermal
  evolution model to reproduce the activity pattern and outburst. Our
  results are consistent with the progressive formation of a dust
  mantle explaining the shallow dependence of gas production rates,
  which may be partially blown off during the outburst. We studied the
  evolution of gas composition, using various ratios such as CN/OH,
  C<SUB>2</SUB>/OH, or C<SUB>3</SUB>/OH, which showed little or no
  variation with heliocentric distance, including at the time of the
  outburst. This indicates a relative level of homogeneity of the nucleus
  composition. <P />Based on observations obtained at the ESO/VLT in
  the framework of program 93.C-0619.

Title: Two Birds One Stone: Simultaneous Atmospheric Pre-Screening
    of Two Temperate Earth-Sized Exoplanets During Their Double Transit
Authors: de Wit, Julien; Burdanov, Artem; Burgasser, Adam J.; Delrez,
   Laetitia; Demory, Brice-Olivier; Gillon, Michael; Jehin, Emmanuel;
   Lederer, Susan; Lewis, Nikole; Magain, Pierre; Queloz, Didier; Triaud,
   Amaury; Van Grootel, Valerie
Bibcode: 2016hst..prop14500D
Altcode:
  We have detected three temperate Earth-sized planets transiting an
  ultra-cool dwarf star only 12 pc away, TRAPPIST-1. This discovery sparks
  the era of detailed characterization and habitability assessment of
  Earth-sized exoplanets. It also opens a new chapter for exoplanetology:
  comparative planetology in the realm of temperate terrestrial
  planets. <P />TRAPPIST-1's system is currently the subject of an
  intense, worldwide follow-up effort that spans the electromagnetic
  spectrum from the UV to radio. Being uniquely suited for NIR and
  UV high-precision observations, HST has a key role to play in this
  follow-up effort. <P />Updated ephemerids resulting from two Spitzer
  DDTs show that TRAPPIST-1 b and c will transit simultaneously on May
  4th, 2016 at 9h10 UT providing a unique and rare opportunity to study
  for the first time, and simultaneously, the atmospheres of temperate
  Earth-sized planets outside of the Solar System. We propose a 4-orbit
  pre-screening program with WFC3 to definitely test the H/He-dominated
  atmospheric scenario for these planets and determine the relative
  inclination of both planets, bringing invaluable constraints on the
  dynamical history of the system.

Title: On the eclipsing binary nature of a nearby ultracool dwarf
Authors: Gillon, Michael; Jehin, Emmanuel; de Wit, Julien; Demory,
   Brice-Olivier; Burgasser, Adam; Van Grootel, Valerie; Lederer, Susan;
   Triaud, Amaury; Delrez, Laetitia; Burdanov, Artem; Queloz, Didier;
   Magain, Pierre
Bibcode: 2016sptz.prop12130G
Altcode:
  The eclipsing binary nature of a nearby ultracool dwarf has just been
  revealed. The aim of this DDT is to investigate this nearby system
  further through high-precision infrared time-series photometry.

Title: On the eclipsing binary nature of a nearby ultracool dwarf
Authors: Gillon, Michael; de Wit, Julien; Jehin, Emmanuel; Burdanov,
   Artem; Van Grootel, valerie. vangrootel@ulg. ac. be; Delrez, Laetitia;
   Magain, Pierre; Burgasser, Adam; Demory, Brice-Olivier; Triaud,
   Amaury; Queloz, Didier; Lederer, Sue
Bibcode: 2016sptz.prop12126G
Altcode:
  The eclipsing binary nature of a nearby ultracool dwarf has just been
  revealed. The aim of this DDT is to investigate this nearby system
  further through high-precision infrared time-series photometry.

Title: Analysis of luminosity distributions and the shape parameters
    of strong gravitational lensing elliptical galaxies
Authors: Biernaux, J.; Magain, P.; Sluse, D.; Chantry, V.
Bibcode: 2016A&A...585A..84B
Altcode: 2015arXiv151009118B
  Context. The luminosity profiles of galaxies acting as strong
  gravitational lenses can be tricky to study. Indeed, strong
  gravitational lensing images display several lensed components, both
  point-like and diffuse, around the lensing galaxy. Those objects limit
  the study of the galaxy luminosity to its inner parts. Therefore, the
  usual fitting methods perform rather badly on such images. Previous
  studies of strong lenses luminosity profiles using software such as
  GALFIT or IMFITFITS and various PSF-determining methods have resulted
  in somewhat discrepant results. <BR /> Aims: The present work aims at
  investigating the causes of those discrepancies, as well as at designing
  more robust techniques for studying the morphology of early-type
  lensing galaxies with the ability to subtract a lensed signal from
  their luminosity profiles. <BR /> Methods: We design a new method
  to independently measure each shape parameter, namely, the position
  angle, ellipticity, and half-light radius of the galaxy. Our half-light
  radius measurement method is based on an innovative scheme for computing
  isophotes that is well suited to measuring the morphological properties
  of gravititational lensing galaxies. Its robustness regarding various
  specific aspects of gravitational lensing image processing is analysed
  and tested against GALFIT. It is then applied to a sample of systems
  from the CASTLES database. <BR /> Results: Simulations show that, when
  restricted to small, inner parts of the lensing galaxy, the technique
  presented here is more trustworthy than GALFIT. It gives more robust
  results than GALFIT, which shows instabilities regarding the fitting
  region, the value of the Sérsic index, and the signal-to-noise
  ratio. It is therefore better suited than GALFIT for gravitational
  lensing galaxies. It is also able to study lensing galaxies that are
  not much larger than the PSF. New values for the half-light radius
  of the objects in our sample are presented and compared to previous
  works. <P />Table 6 is only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/585/A84">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/585/A84</A>

Title: TRAPPIST photometry and imaging monitoring of comet C/2013 R1
(Lovejoy): Implications for the origin of daughter species
Authors: Opitom, C.; Jehin, E.; Manfroid, J.; Hutsemékers, D.;
   Gillon, M.; Magain, P.
Bibcode: 2015A&A...584A.121O
Altcode: 2015arXiv150701520O
  We report the results of the narrow-band photometry and imaging
  monitoring of comet C/2013 R1 (Lovejoy) with the robotic telescope
  TRAPPIST (La Silla observatory). We gathered around 400 images
  over 8 months pre- and post-perihelion between September 12, 2013
  and July 6, 2014. We followed the evolution of the OH, NH, CN,
  C<SUB>3</SUB>, and C<SUB>2</SUB> production rates computed with the
  Haser model, as well as the evolution of the dust production. All
  five gas species display an asymmetry about perihelion, since the
  rate of brightening is steeper than the rate of fading. The study
  of the coma morphology reveals gas and dust jets that indicate one
  or several active zone(s) on the nucleus. The dust, C<SUB>2</SUB>,
  and C<SUB>3</SUB> morphologies present some similarities, while
  the CN morphology is different. OH and NH are enhanced in the tail
  direction. The study of the evolution of the comet activity shows
  that the OH, NH, and C<SUB>2</SUB> production rate evolution with the
  heliocentric distance is correlated to the dust evolution. The CN and,
  to a lesser extent, the C<SUB>3</SUB> do not display such a correlation
  with the dust. This evidence and the comparison with parent species
  production rates indicate that C<SUB>2</SUB> and C<SUB>3</SUB>,
  on one hand, and OH and NH, on the other, could be - at least
  partially - released from organic - rich grains and icy grains. On
  the contrary, all evidences point to HCN being the main parent of CN
  in this comet. <P />Appendix A is available in electronic form at <A
  href="http://www.aanda.org/10.1051/0004-6361/201526427/olm">http://www.aanda.org</A>

Title: Five years of comet narrow band photometry and imaging with
    TRAPPIST
Authors: Opitom, Cyrielle; Jehin, Emmanuel; Manfroid, Jean;
   Hutsemékers, Damien; Gillon, Michaël; Magain, Pierre
Bibcode: 2015DPS....4750602O
Altcode:
  TRAPPIST is a 60-cm robotic telescope in La Silla Observatory [1]
  mainly dedicated to the study of exoplanets and comets. The telescope
  is equipped with a set of narrow band cometary filters designed by the
  NASA for the Hale-Bopp observing campaign [2]. Since its installation in
  2010, we gathered a high quality and homogeneous data set of more than
  30 bright comets observed with narrow band filters. Some comets were
  only observed for a few days but others have been observed weekly during
  several months on both sides of perihelion. From the images, we derived
  OH, NH, CN, C<SUB>2</SUB>, and C<SUB>3</SUB> production rates using a
  Haser [3] model in addition to the Afρ parameter as a proxy for the
  dust production. We computed production rates ratios and the dust color
  for each comet to study their composition and followed the evolution
  of these ratios and colors with the heliocentric distance.The TRAPPIST
  data set, rich of more than 10000 images obtained and reduced in an
  homogeneous way, allows us to address several fundamental questions
  such as the pristine or evolutionary origin of composition differences
  among comets. The evolution of comet activity with the heliocentric
  distance, the differences between species, and from comet to comet, will
  be discussed. Finally, the first results about the one year campaign on
  comet C/2013 US10 (Catalina) and our recent work on the re-determination
  of Haser scalelengths will be presented.[1] Jehin et al., The Messenger,
  145, 2-6, 2011[2] Farnham et al., Icarus, 147, 180-204, 2000[3] Haser,
  Bulletin de l’Académie Royal des Sciences de Belgique,63, 739, 1957

Title: VizieR Online Data Catalog: Shape parameters of lensing
    galaxies (Biernaux+, 2016)
Authors: Biernaux, J.; Magain, P.; Sluse, D.; Chantry, V.
Bibcode: 2015yCat..35850084B
Altcode:
  In the paper we explain procedures designed to measure the position
  angle, the ellipticity and the half-light radius of lensing galaxies,
  that rely on an innovative scheme to compute isophotes. Table 6
  details frame per frame the characteristics of the masks used in this
  work. Those values are in fact the shape parameters of the galaxies,
  before correcting from the effect of the PSF. The relative coordinates
  of the galaxy center, with regards to a reference lensed image, and the
  size of the region of interest are given as well. The reference lensed
  image can be found in Fig. 2 in the paper and is the one labelled A
  (or A1 in some cases). <P />(2 data files).

Title: On the nature of cosmological time
Authors: Magain, Pierre; Hauret, Clémentine
Bibcode: 2015arXiv150502052M
Altcode:
  Time is a parameter playing a central role in our most fundamental
  modeling of natural laws. Relativity theory shows that the comparison
  of times measured by different clocks depends on their relative
  motions and on the strength of the gravitational field in which they
  are embedded. In standard cosmology, the time parameter is the one
  measured by fundamental clocks, i.e. clocks at rest with respect to the
  expanding space. This proper time is assumed to flow at a constant rate
  throughout the whole history of the Universe. We make the alternative
  hypothesis that the rate at which cosmological time flows depends on the
  dynamical state of the Universe. In thermodynamics, the arrow of time
  is strongly related to the second law, which states that the entropy
  of an isolated system will always increase with time or, at best,
  stay constant. Hence, we assume that time measured by fundamental
  clocks is proportional to the entropy of the region of the Universe
  that is causally connected to them. Under that simple assumption, we
  build a cosmological model that explains the Type Ia Supernovae data
  (the best cosmological standard candles) without the need for exotic
  dark matter nor dark energy.

Title: TRAPPIST monitoring of comet C/2012 F6 (Lemmon)
Authors: Opitom, C.; Jehin, E.; Manfroid, J.; Hutsemékers, D.;
   Gillon, M.; Magain, P.
Bibcode: 2015A&A...574A..38O
Altcode:
  We report the results of the long-term narrowband photometry and
  imaging monitoring of comet C/2012 F6 (Lemmon) with the robotic
  TRAPPIST telescope (La Silla Observatory). Observations covered 52
  nights pre- and post-perihelion between December 11, 2012, and June 11,
  2013 (perihelion: 24 March, 2013). We followed the evolution of the OH,
  NH, CN, C<SUB>3</SUB>, and C<SUB>2</SUB> production rates computed with
  the Haser model as well as the evolution of the A(θ)fρ parameter
  as a proxy for the dust production. All five gas species display
  similar slopes for the heliocentric dependence. An asymmetry about
  perihelion is observed, the rate of brightening being steeper than the
  rate of fading. The chemical composition of the comet's coma changes
  slightly along the orbit: the relative abundance of C<SUB>2</SUB>
  to CN increases with the heliocentric distance (r) below -1.4 au
  and decreases with r beyond 1.4 au while the C<SUB>3</SUB>-to-CN
  ratio is constant during our observations. The behavior of the dust
  is different from that of the gas, the slope of the heliocentric
  dependence becoming steeper in early February, correlated to a change
  in the visual lightcurve slope. However, the dust color does not
  vary during the observations. The application of several enhancement
  techniques on the images revealed structures in the CN, C<SUB>3</SUB>,
  and C<SUB>2</SUB> images. These features imply the existence of one or
  several active zone(s) on the comet nucleus. The shape of the structures
  is similar in these three filters and changes from a roughly hourglass
  shape in December and January to a corkscrew shape in February and
  March. The structures in the continuum filters (sampling the dust)
  are not correlated to those observed for the gas. During several full
  nights in February, we observed changes in the CN and C<SUB>2</SUB>
  structures that repeated periodically because of the nucleus rotation,
  our derived rotational period being of 9.52 ± 0.05 h. <P />Full
  Tables 2, 4, 6 are only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/574/A38">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/574/A38</A>

Title: A global analysis of Spitzer and new HARPS data confirms the
    loneliness and metal-richness of GJ 436 b
Authors: Lanotte, A. A.; Gillon, M.; Demory, B. -O.; Fortney, J. J.;
   Astudillo, N.; Bonfils, X.; Magain, P.; Delfosse, X.; Forveille, T.;
   Lovis, C.; Mayor, M.; Neves, V.; Pepe, F.; Queloz, D.; Santos, N.;
   Udry, S.
Bibcode: 2014A&A...572A..73L
Altcode: 2014arXiv1409.4038L
  Context. GJ 436b is one of the few transiting warm Neptunes for
  which a detailed characterisation of the atmosphere is possible,
  whereas its non-negligible orbital eccentricity calls for further
  investigation. Independent analyses of several individual datasets
  obtained with Spitzer have led to contradicting results attributed to
  the different techniques used to treat the instrumental effects. <BR
  /> Aims: We aim at investigating these previous controversial results
  and developing our knowledge of the system based on the full Spitzer
  photometry dataset combined with new Doppler measurements obtained
  with the HARPS spectrograph. We also want to search for additional
  planets. <BR /> Methods: We optimise aperture photometry techniques
  and the photometric deconvolution algorithm DECPHOT to improve the
  data reduction of the Spitzer photometry spanning wavelengths from
  3-24 μm. Adding the high-precision HARPS radial velocity data, we
  undertake a Bayesian global analysis of the system considering both
  instrumental and stellar effects on the flux variation. <BR /> Results:
  We present a refined radius estimate of R<SUB>P</SUB> = 4.10 ± 0.16
  R<SUB>⊕</SUB> , mass M<SUB>P</SUB> = 25.4 ± 2.1 M<SUB>⊕</SUB>,
  and eccentricity e = 0.162 ± 0.004 for <ASTROBJ>GJ 436b</ASTROBJ>. Our
  measured transit depths remain constant in time and wavelength, in
  disagreement with the results of previous studies. In addition, we find
  that the post-occultation flare-like structure at 3.6 μm that led to
  divergent results on the occultation depth measurement is spurious. We
  obtain occultation depths at 3.6, 5.8, and 8.0 μm that are shallower
  than in previous works, in particular at 3.6 μm. However, these
  depths still appear consistent with a metal-rich atmosphere depleted in
  methane and enhanced in CO/CO<SUB>2</SUB>, although perhaps less than
  previously thought. We could not detect a significant orbital modulation
  in the 8 μm phase curve. We find no evidence of a potential planetary
  companion, stellar activity, or a stellar spin-orbit misalignment. <BR
  /> Conclusions: Recent theoretical models invoking high-metallicity
  atmospheres for warm Neptunes are a reasonable match to our results,
  but we encourage new modelling efforts based on our revised data. Future
  observations covering a wide wavelength range of GJ 436b and other
  Neptune-class exoplanets will further illuminate their atmosphere
  properties, whilst future accurate radial velocity measurements might
  explain the eccentricity. <P />Based on observations made with the HARPS
  spectrograph on the 3.6 m ESO telescope at the ESO La Silla Observatory,
  Chile.Table 2 and Figs. 5-7 are available in electronic form at <A
  href="http://www.aanda.org/10.1051/0004-6361/201424373/olm">http://www.aanda.org</A>

Title: VizieR Online Data Catalog: TRAPPIST monitoring of comet
    C/2012 F6 (Lemmon) (Opitom+, 2015)
Authors: Opitom, C.; Jehin, E.; Manfroid, J.; Hutsemekers, D.; Gillon,
   M.; Magain, P.
Bibcode: 2014yCat..35740038O
Altcode: 2014yCat..35749038O
  Observational circumstances, OH, NH, CN, C<SUB>3 and C</SUB>2 production
  and A(θ)f<SUB>{rho}</SUB> values of comet C/2012 F6 (Lemmon) obtained
  using the TRAPPIST telescope <P />(3 data files).

Title: Search for a habitable terrestrial planet transiting the
    nearby red dwarf GJ 1214
Authors: Gillon, M.; Demory, B. -O.; Madhusudhan, N.; Deming, D.;
   Seager, S.; Zsom, A.; Knutson, H. A.; Lanotte, A. A.; Bonfils, X.;
   Désert, J. -M.; Delrez, L.; Jehin, E.; Fraine, J. D.; Magain, P.;
   Triaud, A. H. M. J.
Bibcode: 2014A&A...563A..21G
Altcode: 2013arXiv1307.6722G
  High-precision eclipse spectrophotometry of transiting terrestrial
  exoplanets represents a promising path for the first atmospheric
  characterizations of habitable worlds and the search for life outside
  our solar system. The detection of terrestrial planets transiting nearby
  late-type M-dwarfs could make this approach applicable within the
  next decade, with soon-to-come general facilities. In this context,
  we previously identified GJ 1214 as a high-priority target for a
  transit search, as the transit probability of a habitable planet
  orbiting this nearby M4.5 dwarf would be significantly enhanced by
  the transiting nature of GJ 1214 b, the super-Earth already known
  to orbit the star. Based on this observation, we have set up an
  ambitious high-precision photometric monitoring of GJ 1214 with the
  Spitzer Space Telescope to probe the inner part of its habitable zone
  in search of a transiting planet as small as Mars. We present here
  the results of this transit search. Unfortunately, we did not detect
  any other transiting planets. Assuming that GJ 1214 hosts a habitable
  planet larger than Mars that has an orbital period smaller than 20.9
  days, our global analysis of the whole Spitzer dataset leads to an a
  posteriori no-transit probability of ~98%. Our analysis allows us to
  significantly improve the characterization of GJ 1214 b, to measure its
  occultation depth to be 70 ± 35 ppm at 4.5 μm, and to constrain it
  to be smaller than 205 ppm (3σ upper limit) at 3.6 μm. In agreement
  with the many transmission measurements published so far for GJ 1214 b,
  these emission measurements are consistent with both a metal-rich and a
  cloudy hydrogen-rich atmosphere. <P />The photometric time series used
  in this work are only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/563/A21">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/563/A21</A>

Title: VizieR Online Data Catalog: GJ 1214 Trappist and Spitzer
    light curves (Gillon+, 2014)
Authors: Gillon, M.; Deming, D.; Madhusudhan, N.; Deming, D.; Seager,
   S.; Zsom, A.; Knutson, H. A.; Lanotte, A. A.; Bonfils, X.; Desert,
   J. -M.; Delrez, L.; Jehin, E.; Fraine, J. D.; Magain, P.; Triaud,
   A. H. M. J.
Bibcode: 2014yCat..35630021G
Altcode: 2014yCat..35639021G
  Files trappist.dat, spitzer1.dat, and spitzer2.dat contain the
  photometric time-series presented in the paper and obtained by the
  TRAPPIST and Spitzer telescopes. <P />(3 data files).

Title: TRAPPIST (TRAnsiting Planets and PlanetesImals Small Telescope)
Authors: Jehin, E.; Gillon, M.; Opitom, C.; Manfroid, J.; Hutsemékers,
   D.; Magain, P.
Bibcode: 2013EPSC....8..968J
Altcode:
  TRAPPIST is a 60-cm robotic telescope that has been installed in June
  2010 at the ESO La Silla Observatory [1]. Operated from Liège (Belgium)
  it is devoted to the detection and characterisation of exoplanets and
  to the study of comets and other small bodies in the Solar System. We
  describe here the hardware and the goals of the project and give an
  overview of the comet production rates monitoring after three years
  of operations.

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses. XIV. Time delay of the doubly lensed quasar SDSS J1001+5027
Authors: Rathna Kumar, S.; Tewes, M.; Stalin, C. S.; Courbin, F.;
   Asfandiyarov, I.; Meylan, G.; Eulaers, E.; Prabhu, T. P.; Magain,
   P.; Van Winckel, H.; Ehgamberdiev, Sh.
Bibcode: 2013A&A...557A..44R
Altcode: 2013arXiv1306.5105R
  This paper presents optical R-band light curves and the time delay of
  the doubly imaged gravitationally lensed quasar SDSS J1001+5027 at a
  redshift of 1.838. We have observed this target for more than six years,
  between March 2005 and July 2011, using the 1.2-m Mercator Telescope,
  the 1.5-m telescope of the Maidanak Observatory, and the 2-m Himalayan
  Chandra Telescope. Our resulting light curves are composed of 443
  independent epochs, and show strong intrinsic quasar variability, with
  an amplitude of the order of 0.2 magnitudes. From this data, we measure
  the time delay using five different methods, all relying on distinct
  approaches. One of these techniques is a new development presented in
  this paper. All our time-delay measurements are perfectly compatible. By
  combining them, we conclude that image A is leading B by 119.3 ±
  3.3 days (1σ, 2.8% uncertainty), including systematic errors. It has
  been shown recently that such accurate time-delay measurements offer a
  highly complementary probe of dark energy and spatial curvature, as they
  independently constrain the Hubble constant. The next mandatory step
  towards using SDSS J1001+5027 in this context will be the measurement
  of the velocity dispersion of the lensing galaxy, in combination with
  deep Hubble Space Telescope imaging. <P />Based on observations made
  with the 2.0-m Himalayan Chandra Telescope (Hanle, India), the 1.5-m
  AZT-22 telescope (Maidanak Observatory, Uzbekistan), and the 1.2-m
  Mercator Telescope. Mercator is operated on the island of La Palma
  by the Flemish Community, at the Spanish Observatorio del Roque de
  los Muchachos of the Instituto de Astrofísica de Canarias.Light
  curves are only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/557/A44">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/557/A44</A>

Title: TRAPPIST monitoring of comet C/2012 F6 (Lemmon)
Authors: Opitom, C.; Jehin, E.; Manfroid, J.; Hutsemékers, D.;
   Gillon, M.; Magain, P.
Bibcode: 2013EPSC....8..764O
Altcode:
  Comet C/2012 F6 is a long-period comet that reached perihelion on March
  23, 2012. The unexpected brightness of this comet since December 2012
  allowed us to obtain narrowband photometry and to study its chemical
  composition as well as its rotation.

Title: Herschel imaging and spectroscopy of the nebula around the
    luminous blue variable star WRAY 15-751
Authors: Vamvatira-Nakou, C.; Hutsemékers, D.; Royer, P.; Nazé,
   Y.; Magain, P.; Exter, K.; Waelkens, C.; Groenewegen, M. A. T.
Bibcode: 2013A&A...557A..20V
Altcode: 2013arXiv1307.0759V
  We have obtained far-infrared Herschel-PACS imaging and spectroscopic
  observations of the nebular environment of the luminous blue variable
  (LBV) WRAY 15-751. The far-infrared images clearly show that the main,
  dusty nebula is a shell of radius 0.5 pc and width 0.35 pc extending
  outside the Hα nebula. Furthermore, these images reveal a second,
  bigger and fainter dust nebula that is observed for the first time. Both
  nebulae lie in an empty cavity, very likely the remnant of the O-star
  wind bubble formed when the star was on the main sequence. The kinematic
  ages of the nebulae are calculated to be about 2 × 10<SUP>4</SUP> and
  8 × 10<SUP>4</SUP> years, and we estimated that each nebula contains
  ~0.05 M<SUB>⊙</SUB> of dust. Modeling of the inner nebula indicates
  a Fe-rich dust. The far-infrared spectrum of the main nebula revealed
  forbidden emission lines coming from ionized and neutral gas. Our
  study shows that the main nebula consists of a shell of ionized
  gas surrounded by a thin photodissociation region illuminated by an
  "average" early-B star. We derive the abundance ratios N/O = 1.0 ±
  0.4 and C/O = 0.4 ± 0.2, which indicate a mild N/O enrichment. From
  both the ionized and neutral gas components we estimate that the inner
  shell contains 1.7 ± 0.6 M<SUB>⊙</SUB> of gas. Assuming a similar
  dust-to-gas ratio for the outer nebula, the total mass ejected by WRAY
  15-751 amounts to 4 ± 2 M<SUB>⊙</SUB>. The measured abundances,
  masses and kinematic ages of the nebulae were used to constrain
  the evolution of the star and the epoch at which the nebulae were
  ejected. Our results point to an ejection of the nebulae during the
  red super-giant (RSG) evolutionary phase of an ~40 M<SUB>⊙</SUB>
  star. The multiple shells around the star suggest that the mass-loss
  was not a continuous ejection but rather a series of episodes of
  extreme mass-loss. Our measurements are compatible with the recent
  evolutionary tracks computed for an ~40 M<SUB>⊙</SUB> star with
  little rotation. They support the O-BSG-RSG-YSG-LBV filiation and the
  idea that high-luminosity and low-luminosity LBVs follow different
  evolutionary paths. <P />Herschel is an ESA space observatory with
  science instruments provided by European-led Principal Investigator
  consortia and with important participation from NASA.Based in part
  on observations collected at the European Southern Observatory, La
  Silla, Chile.

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses. XIII. Time delays and 9-yr optical monitoring of the lensed
    quasar RX J1131-1231
Authors: Tewes, M.; Courbin, F.; Meylan, G.; Kochanek, C. S.; Eulaers,
   E.; Cantale, N.; Mosquera, A. M.; Magain, P.; Van Winckel, H.; Sluse,
   D.; Cataldi, G.; Vörös, D.; Dye, S.
Bibcode: 2013A&A...556A..22T
Altcode: 2012arXiv1208.6009T
  We present the results from nine years of optically monitoring the
  gravitationally lensed z<SUB>QSO</SUB> = 0.658 quasar RX J1131-1231. The
  R-band light curves of the four individual images of the quasar
  were obtained using deconvolution photometry for a total of 707
  epochs. Several sharp quasar variability features strongly constrain the
  time delays between the quasar images. Using three different numerical
  techniques, we measured these delays for all possible pairs of quasar
  images while always processing the four light curves simultaneously. For
  all three methods, the delays between the three close images A, B,
  and C are compatible with being 0, while we measured the delay of
  image D to be 91 days, with a fractional uncertainty of 1.5% (1σ),
  including systematic errors. Our analysis of random and systematic
  errors accounts in a realistic way for the observed quasar variability,
  fluctuating microlensing magnification over a broad range of temporal
  scales, noise properties, and seasonal gaps. Finally, we find that our
  time-delay measurement methods yield compatible results when applied
  to subsets of the data. <P />Based on observations made with the 1.2-m
  Swiss Euler telescope (La Silla, Chile), the 1.3-m SMARTS telescope (Las
  Campanas, Chile), and the 1.2-m Mercator Telescope. Mercator is operated
  on the island of La Palma by the Flemish Community, at the Spanish
  Observatorio del Roque de los Muchachos of the Instituto de Astrofísica
  de Canarias.Light curves are available at the CDS via anonymous ftp to
  <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/556/A22">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/556/A22</A>

Title: Fast-evolving weather for the coolest of our two new substellar
    neighbours
Authors: Gillon, M.; Triaud, A. H. M. J.; Jehin, E.; Delrez, L.;
   Opitom, C.; Magain, P.; Lendl, M.; Queloz, D.
Bibcode: 2013A&A...555L...5G
Altcode: 2013arXiv1304.0481G
  We present the results of intense photometric monitoring in the
  near-infrared (~0.9 μm) with the TRAPPIST robotic telescope of
  the newly discovered binary brown dwarf WISE J104915.57-531906.1,
  the third closest system to the Sun at a distance of only 2 pc. Our
  twelve nights of time-series photometry reveal a quasi-periodic (P =
  4.87 ± 0.01h) variability with a maximum peak-peak amplitude of ~11%
  and strong night-to-night evolution. We attribute this variability
  to the rotational modulation of fast-evolving weather patterns in
  the atmosphere of the coolest component (~T1-type) of the binary. No
  periodic signal is detected for the hottest component (~L8-type). For
  both brown dwarfs, our data allow us to firmly discard any unique
  transit during our observations for planets ≥2 R<SUB>⊕</SUB>. For
  orbital periods smaller than ~9.5 h, transiting planets are excluded
  down to an Earth-size.

Title: SPECULOOS: Search for habitable Planets EClipsing ULtra-cOOl
    Stars
Authors: Gillon, Michaël; Jehin, Emmanuël; Delrez, Laetitia; Magain,
   Pierre; Opitom, Cyrielle; Sohy, Sandrine
Bibcode: 2013prpl.conf2K066G
Altcode:
  The 1000 nearest ultra-cool stars (spectral type M6 and latter)
  represent a unique opportunity for the search for life outside our
  solar system. Due to their small luminosity, their habitable zone is
  30-100 times closer than for the Sun, the corresponding orbital periods
  ranging from one to a few days. Thanks to this proximity, the transits
  of a habitable planet are much more probable and frequent than for
  an Earth-Sun analog, while their tiny size (about 1 Jupiter radius)
  leads to transits deep enough for a ground-based detection, even for
  sub-Earth size planets. Furthermore, a habitable planet transiting
  one of these nearby ultra-cool stars would be amenable for a thorough
  atmospheric characterization, including the detection of possible
  biosignatures, notably with the near-to-come JWST. Motivated by these
  reasons, we have set up the concept of a ground-based survey optimized
  for detecting planets of Earth-size and below transiting the nearest
  Southern ultra-cool stars. We present here this concept and its status.

Title: VizieR Online Data Catalog: The doubly lensed quasar SDSS
    J1001+5027 (Rathna Kumar+, 2013)
Authors: Rathna, Kumar S.; Tewes, M.; Stalin, C. S.; Courbin, F.;
   Asfandiyarov, I.; Meylan, G.; Eulaers, E.; Prabhu, T. P.; Magain,
   P.; van Winckel, H.; Ehgamberdiev, Sh.
Bibcode: 2013yCat..35570044R
Altcode: 2013yCat..35579044R
  These data are R-band light curves of the doubly lensed quasar SDSS
  J1001+5027, as displayed in Fig. 4 of the paper. They cover 6.5 years,
  from March 2005 to July 2011. <P />The light curves are obtained using
  deconvolution photometry of images from 3 different telescopes, for
  a total of 443 epochs. Several quasar variability features strongly
  constrain the time delay between the quasar images. <P />(1 data file).

Title: VizieR Online Data Catalog: R-band light curves of RX
    J1131-1231 (Tewes+, 2013)
Authors: Tewes, M.; Courbin, F.; Meylan, G.; Kochanek, C. S.; Eulaers,
   E.; Cantale, N.; Mosquera, A. M.; Magain, P.; van Winckel, H.; Sluse,
   D.; Cataldi, G.; Voros, D.; Dye, S.
Bibcode: 2013yCat..35560022T
Altcode: 2013yCat..35569022T
  We have been monitoring the quadruply lensed quasar RX J1131-1231 since
  December 2003 with different telescopes in the R band (~600-720nm). The
  resulting R-band light curves of the quadruply lensed quasar RX
  J1131-1231, is displayed in Fig. 4 of the paper. <P />The light
  curves are obtained using deconvolution photometry of images from 3
  different telescopes (the ESO Euler 1.2m, the CTIO SMARTS 1.3m and
  the Mercator 1.2m), for a total of 707 epochs. Several sharp quasar
  variability features strongly constrain the time delays between the
  quasar images. <P />(1 data file).

Title: The Nebula around the Luminous Blue Variable WRAY 15-751 as
    seen by Herschel
Authors: Vamvatira-Nakou, C.; Hutsemekers, D.; Royer, P.; Naze, Y.;
   Magain, P.; Exter, K.; Waelkens, C.; Groenewegen, M.
Bibcode: 2013msao.confE.188V
Altcode:
  To understand the evolution of massive stars it is crucial to study the
  nebulae associated to Luminous Blue Variables which can reveal the star
  mass-loss history. We obtained far-infrared Herschel PACS imaging and
  spectroscopic observations of the nebula associated with the Luminous
  Blue Variable star WRAY 15-751. These images revealed a second nebula,
  bigger and cooler, lying in an empty cavity that probably delineates
  the remnant of the O-star bubble formed when the star was on the Main
  Sequence. The dust mass and temperature were derived from the modeling
  of the far-infrared SED. The analysis of the emission line spectrum
  revealed that the main nebula consists of a region of photoionised
  gas surrounded by a thin photodissociation region. Both regions are
  mixed with dust. The calculated C, N, O abundances, together with the
  estimated mass-loss rate, show that the nebula was ejected from the
  star during a Red Supergiant phase. This is compatible with the latest
  evolutionary tracks for a ~40 Mo star with little rotation.

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses. XII. Time delays of the doubly lensed quasars SDSS J1206+4332
    and HS 2209+1914
Authors: Eulaers, E.; Tewes, M.; Magain, P.; Courbin, F.; Asfandiyarov,
   I.; Ehgamberdiev, Sh.; Rathna Kumar, S.; Stalin, C. S.; Prabhu, T. P.;
   Meylan, G.; Van Winckel, H.
Bibcode: 2013A&A...553A.121E
Altcode: 2013arXiv1304.4474E
  <BR /> Aims: Within the framework of the COSMOGRAIL collaboration we
  present 7- and 8.5-year-long light curves and time-delay estimates
  for two gravitationally lensed quasars: SDSS J1206+4332 and HS
  2209+1914. <BR /> Methods: We monitored these doubly lensed quasars in
  the R-band using four telescopes: the Mercator, Maidanak, Himalayan
  Chandra, and Euler telescopes, together spanning a period of 7 to
  8.5 observing seasons from mid-2004 to mid-2011. The photometry of
  the quasar images was obtained through simultaneous deconvolution of
  these data. The time delays were determined from these resulting light
  curves using four very different techniques: a dispersion method, a
  spline fit, a regression difference technique, and a numerical model
  fit. This minimizes the bias that might be introduced by the use of
  a single method. <BR /> Results: The time delay for SDSS J1206+4332
  is Δt<SUB>AB</SUB> = 111.3 ± 3 days with A leading B, confirming a
  previously published result within the error bars. For HS 2209+1914
  we present a new time delay of Δt<SUB>BA</SUB> = 20.0 ± 5 days with
  B leading A. <BR /> Conclusions: The combination of data from up to
  four telescopes have led to well-sampled and nearly 9-season-long
  light curves, which were necessary to obtain these results,
  especially for the compact doubly lensed quasar HS 2209+1914. <P
  />Based on observations made with the 1.2-m Swiss Euler telescope
  (La Silla, Chile), the 1.5-m AZT-22 telescope (Maidanak Observatory,
  Uzbekistan), the 2.0-m HCT telescope (Hanle, India), and the 1.2-m
  Mercator Telescope. Mercator is operated on the island of La Palma by
  the Flemish Community, at the Spanish Observatorio del Roque de los
  Muchachos of the Instituto de Astrofísica de Canarias.Numerical values
  of light curves are only available at the CDS via anonymous ftp to
  <A href="http://cdsarc.u-strasbg.fr">cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/553/A121">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/553/A121</A>
  and at <A href="http://www.cosmograil.org">http://www.cosmograil.org</A>

Title: VizieR Online Data Catalog: 2 lensed quasars light curves
    (Eulaers+, 2013)
Authors: Eulaers, E.; Tewes, M.; Magain, P.; Courbin, F.; Asfandiyarov,
   I.; Ehgamberdiev, Sh.; Rathna, Kumar S.; Stalin, C. S.; Prabhu, T. P.;
   Meylan, G.; van Winckel, H.
Bibcode: 2013yCat..35530121E
Altcode: 2013yCat..35539121E
  Within the framework of the COSMOGRAIL collaboration we present 7-
  and 8.5-year-long light curves and time-delay estimates for two
  gravitationally lensed quasars: SDSS J1206+4332 and HS 2209+1914. <P
  />We monitored these doubly lensed quasars in the R-band using four
  telescopes: the Mercator, Maidanak, Himalayan Chandra, and Euler
  Telescopes, together spanning a period of 7 to 8.5 observing seasons
  from mid-2004 to mid-2011. The photometry of the quasar images was
  obtained through simultaneous deconvolution of these data. The time
  delays were determined from these resulting light curves using four very
  different techniques: a dispersion method, a spline fit, a regression
  difference technique, and a numerical model fit. This minimizes the
  bias that might be introduced by the use of a single method. <P />(2
  data files).

Title: TRAPPIST-UCDTS: A prototype search for habitable planets
    transiting ultra-cool stars
Authors: Gillon, M.; Jehin, E.; Fumel, A.; Magain, P.; Queloz, D.
Bibcode: 2013EPJWC..4703001G
Altcode:
  The ∼1000 nearest ultra-cool stars (spectral type M6 and latter)
  represent a unique opportunity for the search for life outside solar
  system. Due to their small luminosity, their habitable zone is 30-100
  times closer than for the Sun, the corresponding orbital periods
  ranging from one to a few days. Thanks to this proximity, the transits
  of a habitable planet are much more probable and frequent than for an
  Earth-Sun analog, while their tiny size (∼1 Jupiter radius) leads to
  transits deep enough for a ground-based detection, even for sub-Earth
  size planets. Furthermore, a habitable planet transiting one of these
  nearby ultra-cool star would be amenable for a thorough atmospheric
  characterization, including the detection of possible biosignatures,
  notably with the near-to-come JWST. Motivated by these reasons, we have
  set up the concept of a ground-based survey optimized for detecting
  planets of Earth-size and below transiting the nearest Southern
  ultra-cool stars. To assess thoroughly the actual potential of this
  future survey, we are currently conducting a prototype mini-survey using
  the TRAPPIST robotic 60cm telescope located at La Silla ESO Observatory
  (Chile). We summarize here the preliminary results of this mini-survey
  that fully validate our concept.

Title: Gravitational lensing evidence against extended dark matter
    halos
Authors: Magain, Pierre; Chantry, Virginie
Bibcode: 2013arXiv1303.6896M
Altcode:
  It is generally thought that galaxies are embedded in dark matter
  halos extending well beyond their luminous matter. The existence of
  these galactic halos is mainly derived from the larger than expected
  velocities of stars and gas in the outskirts of spiral galaxies. Much
  less is known about dark matter around early-type (elliptical or
  lenticular) galaxies. We use gravitational lensing to derive the masses
  of early-type galaxies deflecting light of background quasars. This
  provides a robust measurement of the total mass within the Einstein
  ring, a circle whose diameter is comparable to the separation of the
  different quasar images. We find that the mass-to-light ratio of the
  lensing galaxies does not depend on radius, from inner galactic regions
  out to several half-light radii. Moreover, its value does not exceed the
  value predicted by stellar population models by more than a factor two,
  which may be explained by baryonic dark matter alone, without any need
  for exotic matter. Our results thus suggest that, if dark matter is
  present in early-type galaxies, its amount does not exceed the amount
  of luminous matter and its density follows that of luminous matter, in
  sharp contrast to what is found from rotation curves of spiral galaxies.

Title: COSMOGRAIL: Time delays in lensed quasars from Himalayan
    Chandra Telescope
Authors: Rathna Kumar, S.; Stalin, C. S.; Tewes, M.; Courbin, F.;
   Asfandiyarov, I.; Ibrahimov, M.; Eulaers, E.; Meylan, G.; Prabhu,
   T. P.; Magain, P.
Bibcode: 2013ASInC...9...87R
Altcode:
  Estimating H_0 to an accuracy of few percent is an important
  challenge today as it will offer key insights into various questions
  in cosmology. By measuring time delays between the photometric
  variations in lensed quasar images and subsequent modelling of the
  mass distribution in the lensing galaxy, it is possible to constrain
  H_0 in a way well complementary to traditional techniques. Time delays
  are difficult to measure due to the long time span needed to monitor
  the sources and photometry is challenging due to the small angular
  separation between the lensed quasar images. These issues are addressed
  by the COSMOGRAIL (COSmological MOnitoring of GRAvItational Lenses)
  collaboration, which uses several telescopes in both the hemispheres
  to monitor a large sample of gravitationally lensed quasars. As part
  of this collaboration, 6 sources are being monitored using the 2 m
  Himalayan Chandra Telescope (HCT) in Hanle, India. We present here
  the preliminary estimates of time delays in these sources.

Title: COSMOGRAIL: Measuring Time Delays of Gravitationally Lensed
    Quasars to Constrain Cosmology
Authors: Tewes, M.; Courbin, F.; Meylan, G.; Kochanek, C. S.; Eulaers,
   E.; Cantale, N.; Mosquera, A. M.; Asfandiyarov, I.; Magain, P.; van
   Winckel, H.; Sluse, D.; Keerthi, R. K. S.; Stalin, C. S.; Prabhu,
   T. P.; Saha, P.; Dye, S.
Bibcode: 2012Msngr.150...49T
Altcode:
  COSMOGRAIL is a long-term programme for the photometric monitoring
  of gravitationally lensed quasars. It makes use of several
  medium-size telescopes to derive long and well-sampled light curves
  of lensed quasars, in order to measure the time delays between
  the quasar images. These delays directly relate to the Hubble
  constant H<SUB>0</SUB>, without any need for secondary distance
  calibrations. COSMOGRAIL was initiated in 2004, and has now secured
  almost a decade of data, resulting in cosmological constraints that
  are very complementary to other cosmological probes.

Title: An expanding universe without dark matter and dark energy
Authors: Magain, Pierre
Bibcode: 2012arXiv1212.1110M
Altcode:
  Assuming that observers located inside the Universe measure a time flow
  which is different from the time appearing in the Friedmann-Lemaitre
  equation, and determining this time flow such that the Universe always
  appears flat to these observers, we derive a simple cosmological model
  which allows to explain the velocity dispersions of galaxies in galaxy
  clusters without introducing dark matter. It also solves the horizon
  problem without recourse to inflation. Moreover, it explains the present
  acceleration of the expansion without any resort to dark energy and
  provides a good fit to the observations of distant supernovae. Depending
  on the present value of the matter-energy density, we calculate an
  age of the Universe between 15.4 and 16.5 billion years, significantly
  larger than the 13.7 billion years of the standard Lambda-CDM model. Our
  model has a slower expansion rate in the early epochs, thus leaving
  more time for the formation of structures such as stars and galaxies.

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2012MPC..81457..12J
Altcode:
  No abstract at ADS

Title: Debris disks as seen by Herschel/DUNES
Authors: Löhne, T.; Eiroa, C.; Augereau, J. -C.; Ertel, S.; Marshall,
   J. P.; Mora, A.; Absil, O.; Stapelfeldt, K.; Thébault, P.; Bayo, A.;
   del Burgo, C.; Danchi, W.; Krivov, A. V.; Lebreton, J.; Letawe, G.;
   Magain, P.; Maldonado, J.; Montesinos, B.; Pilbratt, G. L.; White,
   G. J.; Wolf, S.
Bibcode: 2012AN....333..441L
Altcode:
  The far-infrared excesses produced by debris disks are common features
  of stellar systems. These disks are thought to contain solids ranging
  from micron-sized dust to planetesimals. Naturally, their formation
  and evolution are linked to those of potential planets. With this
  motivation, the Herschel open time key programme DUNES (DUst around
  NEarby Stars) aims at further characterising known debris disks and
  discovering new ones in the regime explored by the Herschel space
  observatory. On the one hand, in their survey of 133 nearby FGK stars,
  DUNES discovered a class of extremely cold and faint debris disks,
  different from well-known disks such as the one around Vega in that
  their inferred typical grain sizes are rather large, indicating
  low dynamical excitation and low collision rates. On the other
  hand, for the more massive disk around the sun-like star HD 207129,
  well-resolved PACS images confirmed the ring-liked structure seen in
  HST images and provided valuable information for an in-depth study and
  benchmark for models. Employing both models for power-law fitting and
  collisional evolution we found the disk around HD 207129 to feature
  low collision rates and large grains, as well. Transport by means
  of Poynting-Robertson drag likely plays a role in replenishing the
  dust seen closer to the star, inside of the ring. The inner edge is
  therefore rather smooth and the contribution from the extended halo of
  barely bound grains is small. Both slowly self-stirring and planetary
  perturbations could potentially have formed and shaped this disk. <P
  />Herschel is an ESA space observatory with science instruments provided
  by European-led Principal Investigator consortia and with important
  participation from NASA.

Title: The TRAPPIST survey of southern transiting planets. I. Thirty
    eclipses of the ultra-short period planet WASP-43 b
Authors: Gillon, M.; Triaud, A. H. M. J.; Fortney, J. J.; Demory,
   B. -O.; Jehin, E.; Lendl, M.; Magain, P.; Kabath, P.; Queloz, D.;
   Alonso, R.; Anderson, D. R.; Collier Cameron, A.; Fumel, A.; Hebb, L.;
   Hellier, C.; Lanotte, A.; Maxted, P. F. L.; Mowlavi, N.; Smalley, B.
Bibcode: 2012A&A...542A...4G
Altcode: 2012arXiv1201.2789G
  We present twenty-three transit light curves and seven occultation
  light curves for the ultra-short period planet WASP-43 b, in addition
  to eight new measurements of the radial velocity of the star. Thanks to
  this extensive data set, we improve significantly the parameters of the
  system. Notably, the largely improved precision on the stellar density
  (2.41 ± 0.08 ρ<SUB>⊙</SUB>) combined with constraining the age
  to be younger than a Hubble time allows us to break the degeneracy
  of the stellar solution mentioned in the discovery paper. The
  resulting stellar mass and size are 0.717 ± 0.025 M<SUB>⊙</SUB>
  and 0.667 ± 0.011 R<SUB>⊙</SUB>. Our deduced physical parameters
  for the planet are 2.034 ± 0.052 M<SUB>Jup</SUB> and 1.036 ± 0.019
  R<SUB>Jup</SUB>. Taking into account its level of irradiation, the high
  density of the planet favors an old age and a massive core. Our deduced
  orbital eccentricity, 0.0035<SUB>-0.0025</SUB><SUP>+0.0060</SUP>, is
  consistent with a fully circularized orbit. We detect the emission of
  the planet at 2.09 μm at better than 11-σ, the deduced occultation
  depth being 1560 ± 140 ppm. Our detection of the occultation at 1.19
  μm is marginal (790 ± 320 ppm) and more observations are needed
  to confirm it. We place a 3-σ upper limit of 850 ppm on the depth
  of the occultation at ~0.9 μm. Together, these results strongly
  favor a poor redistribution of the heat to the night-side of the
  planet, and marginally favor a model with no day-side temperature
  inversion. <P />Based on data collected with the TRAPPIST and
  Euler telescopes at ESO La Silla Observatory, Chile, and with the
  VLT/HAWK-I instrument at ESO Paranal Observatory, Chile (program
  086.C-0222).Tables 1 and 4 are available in electronic form at <A
  href="http://www.aanda.org">http://www.aanda.org</A>Photometry
  is only available at the CDS via anonymous ftp
  to cdsarc.u-strasbg.fr (130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/542/A4">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/542/A4</A>

Title: VizieR Online Data Catalog: WASP-43b thirty eclipses (Gillon+,
    2012)
Authors: Gillon, M.; Triaud, A. H. M. J.; Fortney, J. J.; Demory,
   B. -O.; Jehin, E.; Lendl, M.; Magain, P.; Kabath, P.; Queloz, D.;
   Alonso, R.; Anderson, D. R.; Collier, Cameron A.; Fumel, A.; Hebb, L.;
   Hellier, C.; Lanotte, A.; Maxted, P. F. L.; Mowlavi, N.; Smalley, B.
Bibcode: 2012yCat..35420004G
Altcode: 2012yCat..35429004G
  We present photometric time-series obtained by the TRAPPIST, Euler
  and VLT telescopes. <P />(4 data files).

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2012MPC..79337...9J
Altcode:
  No abstract at ADS

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2012MPC..79015...3J
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2012MPC..78279..27J
Altcode:
  No abstract at ADS

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2012MPC..78580...7J
Altcode:
  No abstract at ADS

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses. X. Modeling based on high-precision astrometry of a sample
of 25 lensed quasars: consequences for ellipticity, shear, and
    astrometric anomalies
Authors: Sluse, D.; Chantry, V.; Magain, P.; Courbin, F.; Meylan, G.
Bibcode: 2012A&A...538A..99S
Altcode: 2011arXiv1112.0005S
  Gravitationally lensed quasars can be used as powerful cosmological and
  astrophysical probes. We can (i) infer the Hubble constant H<SUB>0</SUB>
  based on the so-called time-delay technique, (ii) unveil substructures
  along the line-of-sight toward distant galaxies, and (iii) compare the
  shape and the slope of baryons and dark matter distributions in the
  inner regions of galaxies. To reach these goals, we need high-accuracy
  astrometry of the quasar images relative to the lensing galaxy and
  morphology measurements of the lens. In this work, we first present
  new astrometry for 11 lenses with measured time delays, namely,
  JVAS B0218+357, SBS 0909+532, RX J0911.4+0551, FBQS J0951+2635, HE
  1104-1805, PG 1115+080, JVAS B1422+231, SBS 1520+530, CLASS B1600+434,
  CLASS B1608+656, and HE 2149-2745. These measurements proceed from
  the use of the Magain-Courbin-Sohy (MCS) deconvolution algorithm
  applied in an iterative way (ISMCS) to near-IR HST images. We obtain a
  typical astrometric accuracy of about 1-2.5 mas and an accurate shape
  measurement of the lens galaxy. Second, we combined these measurements
  with those of 14 other lensing systems, mostly from the COSMOGRAIL set
  of targets, to present new mass models of these lenses. The modeling
  of these 25 gravitational lenses led to the following results: 1)
  in four double-image quasars (HE0047-1746, J1226-006, SBS 1520+530,
  and HE 2149-2745), we show that the influence of the lens environment
  on the time delay can easily be quantified and modeled, hence putting
  these lenses with high priority for time-delay determination; 2)
  for quadruple-image quasars, the difficulty often encountered in
  reproducing the image positions to milli-arcsec accuracy (astrometric
  anomaly problem) is overcome by explicitly including the nearest visible
  galaxy/satellite in the lens model. However, one anomalous system
  (RXS J1131-1231) does not show any luminous perturber in its vicinity,
  and three others (WFI 2026-4536, WFI 2033-4723, and B2045+265) have
  problematic modeling. These four systems are the best candidates for
  a pertubation by a dark matter substructure along the line-of-sight;
  3) we revisit the correlation between the position angle (PA) and
  ellipticity of the light and of the mass distribution in lensing
  galaxies. As in previous studies, we find a significant correlation
  between the PA of the light and of the mass distributions. However, in
  contrast with these same studies, we find that the ellipticity of the
  light and of the mass also correlate well, suggesting that the overall
  spatial distribution of matter is not very different from the baryon
  distribution in the inner ~5 kpc of lensing galaxies. This offers a
  new test for high-resolution hydrodynamical simulations. <P />Based
  on observations made with the NASA/ESA HST Hubble Space Telescope by
  the CfA-Arizona Space Telescope Lens Survey (CASTLeS) collaboration,
  obtained from the data archive at the Space Science Institute, which
  is operated by AURA, the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS-5-26555.

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2012MPC..77877..22J
Altcode:
  No abstract at ADS

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2012MPC..78177...3J
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Kostov, A.; Vassileva, L.; Vales, J.; Gajdos, S.; Vilagi, J.;
   Foglia, S.; Galli, G.; Buzzi, L.; Naves, R.; Campas, M.; Ligustri,
   R.; Abe, H.; Seki, T.; Bill, H.; Arnold, L.; Kelemen, J.; Micheli,
   M.; Elliott, G. T.; Tholen, D. J.; Baransky, A.; Hergenrother, C. W.;
   Gibbs, A. R.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd,
   G. J.; Tricarico, P.; Grauer, A. D.; Hill, R. E.; Kowalski, R. A.;
   Larson, S. M.; McNaught, R. H.; Blythe, M.; Spitz, G.; Brungard,
   R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.; Gall, C.;
   Melita, M. D.; Durig, D. T.; Liu, H.; Ikari, Y.; Castellano, J.;
   Dupouy, P.; Jaeger, M.; Prosperi, E.; Vollmann, W.; Andreev, M.;
   Emelyanenko, V.; Sergeev, A.; Parakhin, N.; Kozlov, V.; Karpov, N.;
   Nevski, V.; Nicolas, J.; Lopesino, J.; Borghini, W.; Bosch, J. M.;
   Olivera, R. M.; Martignoni, M.; Bryssinck, E.; Diepvens, A.; Gerke,
   V.; Plaksa, S.; Novichonok, A.; Chestnov, D.; Xu, Z.; Gao, X.; Grau
   Horta, F.; Gaitan, J.; Brusa, M.; Sempio, L.; Ohshima, Y.; Sugiyama,
   Y.; Hills, K.; Yusa, T.; Koshikawa, M.; Takahashi, T.; Primak, N.;
   Schultz, A.; Watters, S.; Thiel, J.; Goggia, T.; Dymock, R.; Sato, H.;
   Guido, E.; Sostero, G.; Howes, N.; Kiyota, S.; Haugh, T.; Sherrod,
   P. C.; Bell, C.; Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers,
   D.; Magain, P.; Masek, M.; Cerny, J.; Ebr, J.; Prouza, M.; Kubanek,
   P.; Jelinek, M.; Martin, J. L.; Gonzalez, J.; Carreno, A.; Piqueras,
   J.; Pena Ciriza, F.; Garcia, F.; Henriquez, J. A.; Birtwhistle, P.;
   Climent, T.; Williams, G. V.
Bibcode: 2012MPEC....D...09K
Altcode:
  No abstract at ADS

Title: Modelling the huge, Herschel-resolved debris ring around
    HD 207129
Authors: Löhne, T.; Augereau, J. -C.; Ertel, S.; Marshall, J. P.;
   Eiroa, C.; Mora, A.; Absil, O.; Stapelfeldt, K.; Thébault, P.; Bayo,
   A.; Del Burgo, C.; Danchi, W.; Krivov, A. V.; Lebreton, J.; Letawe,
   G.; Magain, P.; Maldonado, J.; Montesinos, B.; Pilbratt, G. L.; White,
   G. J.; Wolf, S.
Bibcode: 2012A&A...537A.110L
Altcode:
  Debris disks, which are inferred from the observed infrared excess to
  be ensembles of dust, rocks, and probably planetesimals, are common
  features of stellar systems. As the mechanisms of their formation
  and evolution are linked to those of planetary bodies, they provide
  valuable information. The few well-resolved debris disks are even
  more valuable because they can serve as modelling benchmarks and
  help resolve degeneracies in modelling aspects such as typical grain
  sizes and distances. Here, we present an analysis of the HD 207129
  debris disk, based on its well-covered spectral energy distribution
  and Herschel/PACS images obtained in the framework of the DUNES
  (DUst around NEarby Stars) programme. We use an empirical power-law
  approach to the distribution of dust and we then model the production
  and removal of dust by means of collisions, direct radiation pressure,
  and drag forces. The resulting best-fit model contains a total of
  nearly 10<SUP>-2</SUP> Earth masses in dust, with typical grain sizes
  in the planetesimal belt ranging from 4 to 7 μm. We constrain the
  dynamical excitation to be low, which results in very long collisional
  lifetimes and a drag that notably fills the inner gap, especially at
  70 μm. The radial distribution stretches from well within 100 AU in
  an unusual, outward-rising slope towards a rather sharp outer edge
  at about 170-190 AU. The inner edge is therefore smoother than that
  reported for Fomalhaut, but the contribution from the extended halo
  of barely bound grains is similarly small. Both slowly self-stirring
  and planetary perturbations could potentially have formed and shaped
  this disk. <P />Herschel is an ESA space observatory with science
  instruments provided by European-led Principal Investigator consortia
  and with important participation from NASA.

Title: Observations and Orbits of Comets
Authors: Bacci, P.; Tesi, L.; Fagioli, G.; Jaeger, M.; Prosperi, E.;
   Vollmann, W.; Foglia, S.; Galli, G.; Naves, R.; Campas, M.; Ligustri,
   R.; Seki, T.; Shimomoto, S.; Sato, H.; Boattini, A.; Ahern, J. D.;
   Beshore, E. C.; Garradd, G. J.; Gibbs, A. R.; Tricarico, P.; Grauer,
   A. D.; Hill, R. E.; Kowalski, R. A.; Larson, S. M.; McNaught, R. H.;
   Bezpalko, M.; Torres, D.; Kracke, R.; Spitz, G.; Kistler, J.; Stuart,
   J.; Scruggs, S.; Ikari, Y.; Vidal, J. R.; Nicolas, J.; Lopesino, J.;
   Martignoni, M.; Bryssinck, E.; Soulier, J. F.; Diepvens, A.; Grau
   Horta, F.; Tremosa, L.; Brusa, M.; Sempio, L.; Ohshima, Y.; Hills,
   K.; Takahashi, T.; Camilleri, P.; Primak, N.; Schultz, A.; Watters,
   S.; Thiel, J.; Goggia, T.; Guido, E.; Howes, N.; Sostero, G.; Dymock,
   R.; Ryan, E. L.; Shappee, B.; Thompson, D.; Woodward, C. E.; Elenin,
   L.; Sherrod, P. C.; Ambrosioni Prosen, C.; Jehin, E.; Manfroid, J.;
   Gillon, M.; Hutsemekers, D.; Magain, P.; Buczynski, D.; Limon, F.;
   Gonzalez, J.; Garcia, F.; Henriquez, J. A.; Climent, T.; Williams,
   G. V.
Bibcode: 2012MPEC....A...52B
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Kostov, A.; Vassileva, L.; Bacci, P.; Vergari, S.; Tesi,
   L.; Fagioli, G.; Zakrajsek, J.; Casali, M.; Coffano, A.; Marinello,
   W.; Micheli, M.; Pizzetti, G.; Antonini, P.; Haver, R.; Gorelli, R.;
   Jaeger, M.; Prosperi, E.; Vollmann, W.; Buzzi, L.; Naves, R.; Campas,
   M.; Hasubick, W.; Ligustri, R.; Nishiyama, K.; Hashimoto, N.; Kadota,
   K.; Seki, T.; Shimomoto, S.; Sato, H.; Bill, H.; Arnold, L.; Baransky,
   A.; Barinova, K.; Vorontseva, A.; Pettarin, E.; Grauer, A. D.; Hill,
   R. E.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd, G. J.;
   Gibbs, A. R.; Tricarico, P.; Kowalski, R. A.; Larson, S. M.; McNaught,
   R. H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.;
   McVey, T.; Valdivia, A.; Gall, C.; Durig, D. T.; Ikari, Y.; Castellano,
   J.; Dymock, R.; Vidal, J. R.; Karami, M.; Fathivavsari, H.; Vaduvescu,
   O.; Bryssinck, E.; Linder, J.; Nicolas, J.; Martignoni, M.; Haeusler,
   B.; Noel, T.; Diepvens, A.; Zilch, T.; Gerke, V.; Novichonok, A.;
   Steffl, A.; Tremosa, L.; Caimmi, M.; Balanutsa, P.; Lipunov, V.;
   Zimnukhov, D.; Gorbovskoy, E.; Shurpakov, S.; Hills, K.; Koishikawa,
   M.; Takahashi, T.; Herald, D.; Camilleri, P.; Drummond, J.; Guido,
   E.; Sostero, G.; Howes, N.; Sherrod, P. C.; Bell, C.; Ortiz, J. L.;
   Morales, N.; de, I.; Ambrosioni Prosen, C.; Jehin, E.; Manfroid,
   J.; Gillon, M.; Hutsemekers, D.; Magain, P.; Buczynski, D.; Limon,
   F.; Gonzalez, J.; Rinner, C.; Kugel, F.; Benkhaldoun, Z.; Muler, G.;
   Ruiz, J. M.; Williams, G. V.
Bibcode: 2012MPEC....B...23K
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Vilagi, J.; Kornos, L.; Casali, M.; Coffano, A.; Marinello,
   W.; Micheli, M.; Pizzetti, G.; Jaeger, M.; Prosperi, E.; Vollmann, W.;
   Foglia, S.; Galli, G.; Buzzi, L.; Naves, R.; Campas, M.; Hasubick,
   W.; Ligustri, R.; Kadota, K.; Seki, T.; Shimomoto, S.; Sato, H.;
   Baransky, A.; Barinova, K.; Vorobjov, T.; Kowalski, R. A.; Gibbs,
   A. R.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd, G. J.;
   Tricarico, P.; Grauer, A. D.; Hill, R. E.; Larson, S. M.; McNaught,
   R. H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.;
   McVey, T.; Valdivia, A.; Gall, C.; Durig, D. T.; Duddlesten, A. J.;
   Cardamone, C. J.; Simpkins, H. R.; Lopez, J. O.; Clements, R. R.;
   Gardner, M. M.; Jenkins, R. E.; Bailey, E. T.; Miedaner, K. E.; Stitts,
   M. R.; Ikari, Y.; Castellano, J.; Vidal, J. R.; Dupouy, P.; James, N.;
   Cozzi, E.; Kugel, F.; Franco, L.; Bryssinck, E.; Garrigos Sanchez,
   A.; Nicolas, J.; Lopesino, J.; Borghini, W.; Bosch, J. M.; Olivera,
   R. M.; Martignoni, M.; Haeusler, B.; Diepvens, A.; Hui, M. -T.; Gao,
   X.; Tremosa, L.; Ohshima, Y.; Hills, K.; Koishikawa, M.; Takahashi,
   T.; Herald, D.; Primak, N.; Schultz, A.; Watters, S.; Thiel, J.;
   Goggia, T.; Guido, E.; Sostero, G.; Howes, N.; Elenin, L.; Sherrod,
   P. C.; Ambrosioni Prosen, C.; Jehin, E.; Manfroid, J.; Gillon, M.;
   Hutsemekers, D.; Magain, P.; Masek, M.; Cerny, J.; Ebr, J.; Prouza,
   M.; Kubanek, P.; Jelinek, M.; Buczynski, D.; Carrillo, J.; Limon,
   F.; Gonzalez, J.; Pena Ciriza, F.; Baez, J.; Garcia, F.; Muler, G.;
   Ruiz, J. M.; Williams, G. V.
Bibcode: 2012MPEC....B...78V
Altcode:
  No abstract at ADS

Title: Time delays for eleven gravitationally lensed quasars revisited
Authors: Eulaers, E.; Magain, P.
Bibcode: 2011A&A...536A..44E
Altcode: 2011arXiv1112.2609E
  <BR /> Aims: We test the robustness of published time delays for
  11 lensed quasars by using two techniques to measure time shifts in
  their light curves. <BR /> Methods: We chose to use two fundamentally
  different techniques to determine time delays in gravitationally lensed
  quasars: a method based on fitting a numerical model and another one
  derived from the minimum dispersion method introduced by Pelt and
  collaborators. To analyse our sample in a homogeneous way and avoid
  bias caused by the choice of the method used, we apply both methods to
  11 different lensed systems for which delays have been published: JVAS
  B0218+357, SBS 0909+523, RX J0911+0551, FBQS J0951+2635, HE 1104-1805,
  PG 1115+080, JVAS B1422+231, SBS 1520+530, CLASS B1600+434, CLASS
  B1608+656, and HE 2149-2745 <BR /> Results: Time delays for three
  double lenses, JVAS B0218+357, HE 1104-1805, and CLASS B1600+434,
  as well as the quadruply lensed quasar CLASS B1608+656 are confirmed
  within the error bars. We correct the delay for SBS 1520+530. For PG
  1115+080 and RX J0911+0551, the existence of a second solution on top
  of the published delay is revealed. The time delays in four systems,
  SBS 0909+523, FBQS J0951+2635, JVAS B1422+231, and HE 2149-2745 prove
  to be less reliable than previously claimed. <BR /> Conclusions: If
  we wish to derive an estimate of H<SUB>0</SUB> based on time delays
  in gravitationally lensed quasars, we need to obtain more robust light
  curves for most of these systems in order to achieve a higher accuracy
  and robustness on the time delays.

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses. IX. Time delays, lens dynamics and baryonic fraction in
    HE 0435-1223
Authors: Courbin, F.; Chantry, V.; Revaz, Y.; Sluse, D.; Faure, C.;
   Tewes, M.; Eulaers, E.; Koleva, M.; Asfandiyarov, I.; Dye, S.; Magain,
   P.; van Winckel, H.; Coles, J.; Saha, P.; Ibrahimov, M.; Meylan, G.
Bibcode: 2011A&A...536A..53C
Altcode: 2010arXiv1009.1473C
  We present accurate time delays for the quadruply imaged quasar HE
  0435-1223. The delays were measured from 575 independent photometric
  points obtained in the R-band between January 2004 and March 2010. With
  seven years of data, we clearly show that quasar image A is affected
  by strong microlensing variations and that the time delays are best
  expressed relative to quasar image B. We measured Δt<SUB>BC</SUB> = 7.8
  ± 0.8 days, Δt<SUB>BD</SUB> = -6.5 ± 0.7 days and Δt<SUB>CD</SUB>
  = -14.3 ± 0.8 days. We spacially deconvolved HST NICMOS2 F160W images
  to derive accurate astrometry of the quasar images and to infer the
  light profile of the lensing galaxy. We combined these images with
  a stellar population fitting of a deep VLT spectrum of the lensing
  galaxy to estimate the baryonic fraction, f<SUB>b</SUB>, in the Einstein
  radius. We measured f<SUB>b</SUB> = 0.65<SUB>-0.10</SUB><SUP>+0.13</SUP>
  if the lensing galaxy has a Salpeter IMF and f<SUB>b</SUB> =
  0.45<SUB>-0.07</SUB><SUP>+0.04</SUP> if it has a Kroupa IMF. The
  spectrum also allowed us to estimate the velocity dispersion of the
  lensing galaxy, σ<SUB>ap</SUB> = 222 ± 34 km s<SUP>-1</SUP>. We used
  f<SUB>b</SUB> and σ<SUB>ap</SUB> to constrain an analytical model
  of the lensing galaxy composed of an Hernquist plus generalized NFW
  profile. We solved the Jeans equations numerically for the model and
  explored the parameter space under the additional requirement that the
  model must predict the correct astrometry for the quasar images. Given
  the current error bars on f<SUB>b</SUB> and σ<SUB>ap</SUB>, we
  did not constrain H<SUB>0</SUB> yet with high accuracy, i.e., we
  found a broad range of models with χ<SUP>2</SUP> &lt; 1. However,
  narrowing this range is possible, provided a better velocity dispersion
  measurement becomes available. In addition, increasing the depth
  of the current HST imaging data of HE 0435-1223 will allow us to
  combine ourconstraints with lens reconstruction techniques that make
  use of the full Einstein ring that is visible in this object. <P
  />Based on observations made with the 1.2 m Euler Swiss Telescope,
  the 1.5 m telescope of Maidanak Observatory in Uzbekistan, and with
  the 1.2 m Mercator Telescope, operated on the island of La Palma by
  the Flemish Community, at the Spanish Observatorio del Roque de los
  Muchachos of the Instituto de Astrofísica de Canarias. The NASA/ESA
  Hubble Space Telescope data was obtained from the data archive at
  the Space Telescope Science Institute, which is operated by AURA,
  the Association of Universities for Research in Astronomy, Inc., under
  NASA contract NAS-5-26555.Light curves are only available at the CDS
  via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/536/A53">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/536/A53</A>

Title: New Insights into the Quasar Type 1/Type 2 Dichotomy from
    Correlations between Quasar Host Orientation and Polarization
Authors: Borguet, B.; Hutsemékers, D.; Letawe, G.; Letawe, Y.;
   Magain, P.
Bibcode: 2011ASPC..449..459B
Altcode: 2008arXiv0809.4539B
  We investigate correlations between the direction of the optical linear
  polarization and the orientation of the host galaxy/extended emission
  for type 1 and type 2 radio-loud and radio-quiet quasars. We have used
  high resolution Hubble Space Telescope data and a deconvolution process
  to obtain a good determination of the host galaxy/extended emission (EE)
  position angle. With these new measurements and a compilation of data
  from the literature, we find a significant correlation, different for
  type 1 and type 2 objects, between the linear polarization position
  angle and the orientation of the EE, suggesting scattering by an
  extended UV/blue region in both types of objects. Our observations
  support the extension of the Unification Model to the higher luminosity
  AGNs like the quasars, assuming a two component scattering model.

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..77008...8J
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..76684...9J
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Sybiryakova, Y.; Kozyryev, Y.; Kulichenko, N.; Vovk, V.;
   Shulga, O.; Cernis, K.; Zdanavicius, J.; Haver, R.; Buzzi, L.;
   Naves, R.; Campas, M.; Hasubick, W.; Donati, S.; Meyer, M.; Scotti,
   J. V.; Kadota, K.; Asami, A.; Abe, H.; Seki, T.; Shimomoto, S.; Sato,
   H.; Wakuda, S.; Bill, H.; Arnold, L.; Micheli, M.; Elliott, G. T.;
   Tholen, D. J.; Kashuba, S.; Kashuba, V.; Gorbanev, Y.; Podlesnyak,
   S.; Stogneeva, I.; Baransky, A.; Barinova, K.; Markov, Y.; Vorontseva,
   A.; Bressi, T. H.; Hergenrother, C. W.; Kowalski, R. A.; Hill, R. E.;
   Boattini, A.; Ahern, J. D.; Beshore, E. C.; Garradd, G. J.; Gibbs,
   A. R.; Tricarico, P.; Grauer, A. D.; Larson, S. M.; McNaught, R. H.;
   Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.; McVey,
   T.; Valdivia, A.; Gall, C.; Moritz, N.; Elliott, R.; Durig, D. T.;
   Roberts, C. A.; Smith, C. M.; Dziminski, H. T.; Ikari, Y.; Vidal,
   J. R.; Dupouy, P.; Jaeger, M.; Prosperi, E.; Prosperi, S.; Vollmann,
   W.; Shurpakov, S.; Bacci, P.; Antonacci, D.; Nevski, V.; Linder, J.;
   Nicolas, J.; Lopesino, J.; Overhaus, C.; Haeusler, B.; Novichonok, A.;
   Agletdinov, V.; Mezentsev, A.; Ignahin, V.; Bryssinck, E.; Veselkov,
   S.; Bros, X.; Soulier, J. F.; Diepvens, A.; Zilch, T.; Gerke, V.;
   Plaksa, S.; Chestnov, D.; Lindner, P.; Tudorica, A.; Badescu, T.;
   Rosicarelli, M.; Capella, E.; Gaitan, J.; Zhao, H. B.; Yao, J. S.;
   Zhaori, G. T.; Lu, H.; Wang, M.; Hong, R. Q.; Hu, L. F.; Xia, Y.;
   Ohshima, Y.; Hills, K.; Takahashi, T.; Camilleri, P.; Primak, N.;
   Schultz, A.; Watters, S.; Thiel, J.; Goggia, T.; Dymock, R.; Elenin,
   L.; Sherrod, P. C.; Bell, C.; Ortiz, J. L.; Morales, N.; de, I.;
   Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.; Magain, P.;
   Fraga, A.; Limon, F.; Gonzalez, J.; Baez, J.; Garcia, F.; Canales,
   O.; Fletcher, J.; Williams, G. V.
Bibcode: 2011MPEC....V...31S
Altcode:
  No abstract at ADS

Title: Long term photometric monitoring of comet 103P/Hartley2 with
    the new robotic TRAPPIST telescope
Authors: Jehin, E.; Manfroid, J.; Hutsemékers, D.; Gillon, M.;
   Magain, P.
Bibcode: 2011epsc.conf.1489J
Altcode: 2011DPS....43.1489J; 2011epsc.conf.1479J
  We report on a long term monitoring of comet 103P/Hartley2 with
  six cometary narrow band filters using the TRAPPIST 0.60m telescope
  installed recently at the ESO La Silla observatory in Chile. This
  new robotic telescope is dedicated to exoplanet and solar system
  research. The comet was observed with the cometary filters during 4
  months, from Oct. 29 to Feb. 22. Since then the monitoring continues
  but only through the BVRI filters and about two times per week. Those
  observations allowed us to make a detailed light curve of the comet
  after its perihelion passage and derive production rates of the 4
  main species (OH, CN, C2, C3) as well as the dust production rate
  (Afρ) over that period. The high sampling of our monitoring allowed
  us to find a periodicity in the gaseous light curves and to deduce a
  rotation period of 18.4h early November, slowing down to about 19h by
  the end of December.

Title: VizieR Online Data Catalog: R-band light curves of HE 0435-1223
    (Courbin+, 2011)
Authors: Courbin, F.; Chantry, V.; Revaz, Y.; Sluse, D.; Faure, C.;
   Tewes, M.; Eulaers, E.; Koleva, M.; Asfandiyarov, I.; Dye, S.; Magain,
   P.; van Winckel, H.; Coles, J.; Saha, P.; Ibrahimov, M.; Meylan, G.
Bibcode: 2011yCat..35360053C
Altcode: 2011yCat..35369053C
  Photometry of HE 0435-1223, as in Fig. 3 of the paper. The first column
  gives the Julian date and corresponds to HJD days. Columns 2-9 give
  the photometric measurements of the quasar components A, B, C and
  D respectively, with the corresponding error bars. The last column
  provides the name of the telescope used for each measurement. <P />(1
  data file).

Title: Observations and Orbits of Comets
Authors: Sanner, J.; Angelow, S.; Chaumont, F.; Heimann, L.; Lawida,
   M.; Pollitt, A.; Proels, J.; Ronken, K.; Saenger, S.; Honkova, M.;
   Tichy, M.; Ticha, J.; Kocer, M.; Bacci, P.; Tesi, L.; Fagioli, G.;
   Tombelli, M.; Foglia, S.; Interrante, G.; Bartolini, S.; Casali,
   M.; Coffano, A.; Marinello, W.; Micheli, M.; Pizzetti, G.; Jaeger,
   M.; Prosperi, E.; Vollmann, W.; Buzzi, L.; Naves, R.; Campas, M.;
   Donati, S.; Scotti, J. V.; Kadota, K.; Abe, H.; Seki, T.; Shimomoto,
   S.; Sato, H.; Wakuda, S.; Jung, M.; Bill, H.; Kashuba, S.; Kashuba,
   V.; Gorbanev, Y.; Podlesnyak, S.; Stogneeva, I.; Bressi, T. H.;
   Gibbs, A. R.; Kowalski, R. A.; Hill, R. E.; Ahern, J. D.; Beshore,
   E. C.; Boattini, A.; Garradd, G. J.; Tricarico, P.; Grauer, A. D.;
   Larson, S. M.; McNaught, R. H.; Blythe, M.; Spitz, G.; Brungard, R.;
   Paige, J.; Festler, P.; McVey, T.; Valdivia, A.; Gall, C.; Moritz,
   N.; Elliott, R.; Castellano, J.; Vidal, J. R.; Dupouy, P.; Manzini,
   F.; Behrend, R.; Bernasconi, L.; Shurpakov, S.; Thinius, B.; Nevski,
   V.; Linder, J.; Nicolas, J.; Pivato, D.; Lopesino, J.; Overhaus, C.;
   Bosch, J. M.; Olivera, R. M.; Martignoni, M.; Haeusler, B.; Noel,
   T.; Bryssinck, E.; Sachot, G.; Soulier, J. F.; Diepvens, A.; Gerke,
   V.; Novichonok, A.; Plyachshenko, Y.; Grau Horta, F.; Magrin, E.;
   Gonano, V.; Andrea, M.; Zhao, H. B.; Yao, J. S.; Zhaori, G. T.; Lu,
   H.; Wang, M.; Hong, R. Q.; Hu, L. F.; Xia, Y.; Sugiyama, Y.; Hills,
   K.; Takahashi, T.; Herald, D.; Guido, E.; Howes, N.; Sostero, G.;
   Lister, T.; Camilleri, P.; Drummond, J.; Primak, N.; Schultz, A.;
   Watters, S.; Thiel, J.; Goggia, T.; Elenin, L.; Molotov, I.; Haugh,
   T.; Bell, C.; Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.; Losse, F.; Limon, F.; Gonzalez, J.; Garcia, F.; Canales,
   O.; Fletcher, J.; Ruiz, J.; Curto Amigo, J.; Williams, G. V.
Bibcode: 2011MPEC....U...42S
Altcode:
  No abstract at ADS

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..76020...7J
Altcode:
  No abstract at ADS

Title: WASP-50 b: a hot Jupiter transiting a moderately active
    solar-type star
Authors: Gillon, M.; Doyle, A. P.; Lendl, M.; Maxted, P. F. L.;
   Triaud, A. H. M. J.; Anderson, D. R.; Barros, S. C. C.; Bento, J.;
   Collier-Cameron, A.; Enoch, B.; Faedi, F.; Hellier, C.; Jehin, E.;
   Magain, P.; Montalbán, J.; Pepe, F.; Pollacco, D.; Queloz, D.;
   Smalley, B.; Segransan, D.; Smith, A. M. S.; Southworth, J.; Udry,
   S.; West, R. G.; Wheatley, P. J.
Bibcode: 2011A&A...533A..88G
Altcode: 2011arXiv1108.2641G
  We report the discovery by the WASP transit survey of a giant planet
  in a close orbit (0.0295 ± 0.0009 AU) around a moderately bright
  (V = 11.6, K = 10) G9 dwarf (0.89 ± 0.08 M<SUB>⊙</SUB>, 0.84 ±
  0.03 R<SUB>⊙</SUB>) in the Southern constellation Eridanus. Thanks
  to high-precision follow-up photometry and spectroscopy obtained by
  the telescopes TRAPPIST and Euler, the mass and size of this planet,
  WASP-50 b, are well constrained to 1.47 ± 0.09 M<SUB>Jup</SUB>
  and 1.15 ± 0.05 R<SUB>Jup</SUB>, respectively. The transit
  ephemeris is 2 455 558.6120 (±0.0002) + N × 1.955096 (±0.000005)
  HJD<SUB>UTC</SUB>. The size of the planet is consistent with basic
  models of irradiated giant planets. The chromospheric activity (log
  R'<SUB>HK = -4.67</SUB>) and rotational period (P<SUB>rot</SUB>
  = 16.3 ± 0.5 days) of the host star suggest an age of 0.8 ± 0.4
  Gy that is discrepant with a stellar-evolution estimate based on
  the measured stellar parameters (ρ<SUB>∗</SUB> = 1.48 ± 0.10
  ρ<SUB>⊙</SUB>, T<SUB>eff</SUB> = 5400 ± 100 K, [Fe/H] = -0.12
  ± 0.08) which favors an age of 7 ± 3.5 Gy. This discrepancy could
  be explained by the tidal and magnetic influence of the planet on
  the star, in good agreement with the observations that stars hosting
  hot Jupiters tend to show faster rotation and magnetic activity. We
  measure a stellar inclination of 84<SUB>-31<SUP>+6</SUP></SUB> deg,
  disfavoring a high stellar obliquity. Thanks to its large irradiation
  and the relatively small size of its host star, WASP-50 b is a
  good target for occultation spectrophotometry, making it able to
  constrain the relationship between hot Jupiters' atmospheric thermal
  profiles and the chromospheric activity of their host stars. <P />The
  photometric time-series used in this work are only available at the
  CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/533/A88">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/533/A88</A>

Title: TRAPPIST: TRAnsiting Planets and PlanetesImals Small Telescope
Authors: Jehin, E.; Gillon, M.; Queloz, D.; Magain, P.; Manfroid,
   J.; Chantry, V.; Lendl, M.; Hutsemékers, D.; Udry, S.
Bibcode: 2011Msngr.145....2J
Altcode:
  TRAPPIST is a 60-cm robotic telescope that was installed in April 2010
  at the ESO La Silla Observatory. The project is led by the Astrophysics
  and Image Processing group (AIP) at the Department of Astrophysics,
  Geophysics and Oceanography (AGO) of the University of Liège, in
  close collaboration with the Geneva Observatory, and has been funded by
  the Belgian Fund for Scientific Research (F.R.S.-FNRS) and the Swiss
  National Science Foundation (SNF). It is devoted to the detection and
  characterisation of exoplanets and to the study of comets and other
  small bodies in the Solar System. We describe here the goals of the
  project and the hardware and present some results obtained during the
  first six months of operation.

Title: Observations and Orbits of Comets
Authors: Tesi, L.; Bacci, P.; Fagioli, G.; Tombelli, M.; Foglia, S.;
   Galli, F.; Bartolini, S.; Cernis, K.; Zdanavicius, J.; Jaeger, M.;
   Prosperi, E.; Vollmann, W.; Galli, G.; Buzzi, L.; Naves, R.; Campas,
   M.; Kadota, K.; Abe, H.; Baransky, A.; Aleksakhina, E.; Ikari, Y.;
   Vidal, J. R.; Kocher, P.; Rinner, C.; Kugel, F.; Reszelski, M.; Nevski,
   V.; Linder, J.; Nicolas, J.; Pivato, D.; Haeusler, B.; Bryssinck,
   E.; Plaksa, S.; Sachot, G.; Soulier, J. F.; Diepvens, A.; Lindner,
   P.; Dangl, G.; Hills, K.; Herald, D.; McNaught, R. H.; Ahern, J. D.;
   Beshore, E. C.; Boattini, A.; Garradd, G. J.; Gibbs, A. R.; Grauer,
   A. D.; Hill, R. E.; Kowalski, R. A.; Larson, S. M.; Camilleri, P.;
   McCormick, J.; Drummond, J.; Primak, N.; Schultz, A.; Watters, S.;
   Thiel, J.; Goggia, T.; Boaz, R. Z.; Howes, N.; Blyth, H.; Sostero,
   G.; Guido, E.; Sato, H.; Elenin, L.; Holmes, R.; Vorobjov, T.; Haugh,
   T.; Bell, C.; Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.; Sparrenberger, M.; Ruiz, J. M.; Baez, J.; Lozano, I.;
   Cardenete, S.; Chinchilla, J.; Garri, M.; Limon, F.; Gonzalez, J.;
   Garcia, F.; Muler, G.; Vazquez Lopez, G.; Henriquez, J. A.; Canales,
   O.; Benavides, R.; Temprano, J.; Fletcher, J.; Williams, G. V.
Bibcode: 2011MPEC....P...23T
Altcode:
  No abstract at ADS

Title: VizieR Online Data Catalog: WASP-50b photometry and radial
    velocities (Gillon+, 2011)
Authors: Gillon, M.; Doyle, A. P.; Lendl, M.; Maxted, P. F. L.;
   Triaud, A. H. M. J.; Anderson, D. R.; Barros, S. C. C.; Bento,
   J.; Collier-Cameron, A.; Enoch, B.; Faedi, F.; Hellier, C.; Jehin,
   E.; Magain, P.; Montalban, J.; Pepe, F.; Pollacco, D.; Queloz, D.;
   Smalley, B.; Segransan, D.; Smith, A. M. S.; Southworth, J.; Udry,
   S.; West, R. G.; Wheatley, P. J.
Bibcode: 2011yCat..35330088G
Altcode: 2011yCat..35339088G
  Files wasp.dat, trappist.dat and euler.dat contain the photometric
  time-series presented in the paper and obtained by the WASP transit
  survey, and by the TRAPPIST and Euler telescopes. <P />(4 data files).

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..75700...7J
Altcode:
  No abstract at ADS

Title: Comet 45P/HONDA-MRKOS-PAJDUSAKOVA
Authors: McNaught, R. H.; Jehin, E.; Manfroid, J.; Gillon, M.;
   Hutsemekers, D.; Magain, P.; Williams, G. V.
Bibcode: 2011MPEC....P...11M
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..75563...4J
Altcode:
  No abstract at ADS

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..75510..12J
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Tesi, L.; Bacci, P.; Fagioli, G.; Bacci, R.; Casali, M.;
   Coffano, A.; Marinello, W.; Micheli, M.; Pizzetti, G.; Cernis, K.;
   Zdanavicius, J.; Maskoliunas, M.; Haver, R.; Foglia, S.; Galli, G.;
   Buzzi, L.; Naves, R.; Campas, M.; Hasubick, W.; Donati, S.; McAndrew,
   S. G.; Sanchez C., A.; Donato, L.; Gonano, V.; Travagini, M.; Bill, H.;
   Baransky, A.; Buriev, A.; Ponomarenko, V.; Scotti, J. V.; Kowalski,
   R. A.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd, G. J.;
   Gibbs, A. R.; Tricarico, P.; Grauer, A. D.; Hill, R. E.; Larson,
   S. M.; McNaught, R. H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige,
   J.; Festler, P.; McVey, T.; Valdivia, A.; Brewington, H.; Dembicky,
   J.; Harvanek, M.; Ketzeback, B.; Long, D.; Pan, K.; Malanushenko, O.;
   McMillan, R.; Snedden, S.; Watters, S.; Sarneczky, K.; Durig, D. T.;
   Uriostegui, J. R.; Danusantoso, J. F.; Kharel, S.; Duenas, D. E.;
   Rice, A. C.; Vasquez, J. A.; Murphree, C. L.; Koury, E. S.; Castellano,
   J.; Ferrando, R.; Vidal, J. R.; Baldris, F.; Kocher, P.; Jaeger, M.;
   Prosperi, E.; Vollmann, W.; Rinner, C.; Kugel, F.; Nicolas, J.; Bel,
   J.; Borghini, W.; Bryssinck, E.; Sachot, G.; Soulier, J. F.; Diepvens,
   A.; Dangl, G.; Hills, K.; Takahashi, T.; Novichonok, A.; Baroni, S.;
   Concari, P.; Tombelli, M.; Chestnov, D.; Sato, H.; Herald, D.; Lister,
   T.; Guido, E.; Howes, N.; Sostero, G.; McCormick, J.; Primak, N.;
   Schultz, A.; Thiel, J.; Goggia, T.; Glinos, T.; Plaksa, S.; Elenin,
   L.; Hall-Angel Peaks Observatory, J.; Hall, J.; Holmes, R.; Vorobjov,
   T.; Linder, T.; Mills, M.; Hug, G.; Sherrod, P. C.; Bell, C.; Jehin,
   E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.; Magain, P.; Limon,
   F.; Gonzalez, J.; Pena Ciriza, F.; Del Maes, A.; Hernandez, J. F.;
   Garcia, F.; Fletcher, J.; Climent, T.; Williams, G. V.
Bibcode: 2011MPEC....N...13T
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..75359..19J
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Naves, R.; Campas, M.; Seki, T.; Shimomoto, S.; Sato, H.;
   Donato, L.; Gonano, V.; Travagini, M.; Baransky, A.; Buriev, A.;
   Ponomarenko, V.; Beshore, E.; Ahern, J. D.; Boattini, A.; Garradd,
   G. J.; Gibbs, A. R.; Tricarico, P.; Grauer, A. D.; Hill, R. E.;
   Kowalski, R. A.; Larson, S. M.; McNaught, R. H.; Blythe, M.; Spitz,
   G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.;
   Schwartz, M.; Holvorcem, P. R.; Jaeger, M.; Prosperi, E.; Vollmann,
   W.; Rinner, C.; Kugel, F.; Camarasa, J.; Bryssinck, E.; Sachot,
   G.; Diepvens, A.; Hills, K.; Takahashi, T.; Baroni, S.; Buzzi, L.;
   Concari, P.; Foglia, S.; Galli, G.; Tombelli, M.; Camilleri, P.;
   Primak, N.; Schultz, A.; Watters, S.; Thiel, J.; Goggia, T.; Glinos,
   T.; Guido, E.; Sostero, G.; Bell, C.; Jehin, E.; Manfroid, J.; Gillon,
   M.; Hutsemekers, D.; Magain, P.; Williams, G. V.
Bibcode: 2011MPEC....M...11N
Altcode:
  No abstract at ADS

Title: EPOXI: Comet 103P/Hartley 2 Observations from a Worldwide
    Campaign
Authors: Meech, K. J.; A'Hearn, M. F.; Adams, J. A.; Bacci, P.; Bai,
   J.; Barrera, L.; Battelino, M.; Bauer, J. M.; Becklin, E.; Bhatt,
   B.; Biver, N.; Bockelée-Morvan, D.; Bodewits, D.; Böhnhardt, H.;
   Boissier, J.; Bonev, B. P.; Borghini, W.; Brucato, J. R.; Bryssinck,
   E.; Buie, M. W.; Canovas, H.; Castellano, D.; Charnley, S. B.;
   Chen, W. P.; Chiang, P.; Choi, Y. -J.; Christian, D. J.; Chuang,
   Y. -L.; Cochran, A. L.; Colom, P.; Combi, M. R.; Coulson, I. M.;
   Crovisier, J.; Dello Russo, N.; Dennerl, K.; DeWahl, K.; DiSanti,
   M. A.; Facchini, M.; Farnham, T. L.; Fernández, Y.; Florén,
   H. G.; Frisk, U.; Fujiyoshi, T.; Furusho, R.; Fuse, T.; Galli, G.;
   García-Hernández, D. A.; Gersch, A.; Getu, Z.; Gibb, E. L.; Gillon,
   M.; Guido, E.; Guillermo, R. A.; Hadamcik, E.; Hainaut, O.; Hammel,
   H. B.; Harker, D. E.; Harmon, J. K.; Harris, W. M.; Hartogh, P.;
   Hashimoto, M.; Häusler, B.; Herter, T.; Hjalmarson, A.; Holland,
   S. T.; Honda, M.; Hosseini, S.; Howell, E. S.; Howes, N.; Hsieh,
   H. H.; Hsiao, H. -Y.; Hutsemékers, D.; Immler, S. M.; Jackson, W. M.;
   Jeffers, S. V.; Jehin, E.; Jones, T. J.; de Juan Ovelar, M.; Kaluna,
   H. M.; Karlsson, T.; Kawakita, H.; Keane, J. V.; Keller, L. D.;
   Kelley, M. S.; Kinoshita, D.; Kiselev, N. N.; Kleyna, J.; Knight,
   M. M.; Kobayashi, H.; Kobulnicky, H. A.; Kolokolova, L.; Kreiny, M.;
   Kuan, Y. -J.; Küppers, M.; Lacruz, J. M.; Landsman, W. B.; Lara,
   L. M.; Lecacheux, A.; Levasseur-Regourd, A. C.; Li, B.; Licandro,
   J.; Ligustri, R.; Lin, Z. -Y.; Lippi, M.; Lis, D. C.; Lisse, C. M.;
   Lovell, A. J.; Lowry, S. C.; Lu, H.; Lundin, S.; Magee-Sauer, K.;
   Magain, P.; Manfroid, J.; Mazzotta Epifani, E.; McKay, A.; Melita,
   M. D.; Mikuz, H.; Milam, S. N.; Milani, G.; Min, M.; Moreno, R.;
   Mueller, B. E. A.; Mumma, M. J.; Nicolini, M.; Nolan, M. C.; Nordh,
   H. L.; Nowajewski, P. B.; Odin Team; Ootsubo, T.; Paganini, L.;
   Perrella, C.; Pittichová, J.; Prosperi, E.; Radeva, Y. L.; Reach,
   W. T.; Remijan, A. J.; Rengel, M.; Riesen, T. E.; Rodenhuis, M.;
   Rodríguez, D. P.; Russell, R. W.; Sahu, D. K.; Samarasinha, N. H.;
   Sánchez Caso, A.; Sandqvist, A.; Sarid, G.; Sato, M.; Schleicher,
   D. G.; Schwieterman, E. W.; Sen, A. K.; Shenoy, D.; Shi, J. -C.;
   Shinnaka, Y.; Skvarc, J.; Snodgrass, C.; Sitko, M. L.; Sonnett, S.;
   Sosseini, S.; Sostero, G.; Sugita, S.; Swinyard, B. M.; Szutowicz,
   S.; Takato, N.; Tanga, P.; Taylor, P. A.; Tozzi, G. -P.; Trabatti,
   R.; Trigo-Rodríguez, J. M.; Tubiana, C.; de Val-Borro, M.; Vacca,
   W.; Vandenbussche, B.; Vaubaillion, J.; Velichko, F. P.; Velichko,
   S. F.; Vervack, R. J., Jr.; Vidal-Nunez, M. J.; Villanueva, G. L.;
   Vinante, C.; Vincent, J. -B.; Wang, M.; Wasserman, L. H.; Watanabe,
   J.; Weaver, H. A.; Weissman, P. R.; Wolk, S.; Wooden, D. H.; Woodward,
   C. E.; Yamaguchi, M.; Yamashita, T.; Yanamandra-Fischer, P. A.; Yang,
   B.; Yao, J. -S.; Yeomans, D. K.; Zenn, T.; Zhao, H.; Ziffer, J. E.
Bibcode: 2011ApJ...734L...1M
Altcode: 2011arXiv1106.0367K
  Earth- and space-based observations provide synergistic information
  for space mission encounters by providing data over longer timescales,
  at different wavelengths and using techniques that are impossible with
  an in situ flyby. We report here such observations in support of the
  EPOXI spacecraft flyby of comet 103P/Hartley 2. The nucleus is small and
  dark, and exhibited a very rapidly changing rotation period. Prior to
  the onset of activity, the period was ~16.4 hr. Starting in 2010 August
  the period changed from 16.6 hr to near 19 hr in December. With respect
  to dust composition, most volatiles and carbon and nitrogen isotope
  ratios, the comet is similar to other Jupiter-family comets. What
  is unusual is the dominance of CO<SUB>2</SUB>-driven activity near
  perihelion, which likely persists out to aphelion. Near perihelion the
  comet nucleus was surrounded by a large halo of water-ice grains that
  contributed significantly to the total water production.

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..75288...5J
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Eglitis, I.; Cernis, K.; Tesi, L.; Bacci, P.; Fagioli,
   G.; Caronia, A.; Buzzi, L.; Urakawa, S.; Hashimoto, N.; Asami, A.;
   Nishiyama, K.; Okumura, S.; Sakamoto, T.; Kadota, K.; Abe, H.; Seki,
   T.; Shimomoto, S.; Sato, H.; Endate, K.; Sarneczky, K.; Donato,
   L.; Gonano, V.; Travagini, M.; Bill, H.; Kashuba, S.; Kashuba, V.;
   Gorbanev, Y.; Podlesnyak, S.; Stogneeva, I.; Baransky, A.; Buriev,
   A.; Ponomarenko, V.; Zhdanov, A.; Butygina, O.; Weissman, P. R.;
   Brozovic, M.; Owen, W. M., Jr.; Bressi, T. H.; Hergenrother, C. W.;
   Grauer, A. D.; Gibbs, A. R.; Kowalski, R. A.; Beshore, E.; Ahern,
   J. D.; Boattini, A.; Garradd, G. J.; Tricarico, P.; Hill, R. E.;
   Larson, S. M.; McNaught, R. H.; Blythe, M.; Spitz, G.; Brungard,
   R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.; Mackintosh,
   R.; Konishi, M.; Salvo, R.; Bruzzone, S.; Roland, S.; Tancredi,
   G.; Martinez, M.; Abe, S.; Guo, J. K.; Chen, W. P.; Schwartz, M.;
   Holvorcem, P. R.; Castellano, J.; Vidal, J. R.; Dupouy, P.; Baldris,
   F.; Jaeger, M.; Prosperi, E.; Prosperi, S.; Vollmann, W.; Rinner, C.;
   Kugel, F.; Bryssinck, E.; Soulier, J. F.; Diepvens, A.; Zilch, T.;
   Hills, K.; Takahashi, T.; Baroni, S.; Concari, P.; Foglia, S.; Galli,
   G.; Tombelli, M.; Camilleri, P.; Linder, J.; Herald, D.; Miles, R.;
   Primak, N.; Schultz, A.; Watters, S.; Thiel, J.; Goggia, T.; Micheli,
   M.; Dymock, R.; Masek, M.; Chestnov, D.; Novichonok, A.; Plaksa, S.;
   Elenin, L.; Holmes, R.; Vorobjov, T.; Sherrod, P. C.; Bell, C.; Colazo,
   C.; Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.; Magain, P.;
   Gonzalez, J.; Hernandez, J. F.; Garcia, F.; Lacruz, J.; Williams, G. V.
Bibcode: 2011MPEC....L...51E
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..75109..50J
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..74775..38J
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Tesi, L.; Bacci, P.; Fagioli, G.; Vivarelli, M.; Greco, L.;
   Casali, M.; Coffano, A.; Marinello, W.; Micheli, M.; Pizzetti, G.;
   Apitzsch, R.; Naves, R.; Campas, M.; Hasubick, W.; Seki, T.; Shimomoto,
   S.; Sato, H.; Christie, G. W.; Natusch, T.; Donato, L.; Gonano, V.;
   Travagini, M.; Bill, H.; Baransky, A.; Bambery, R.; Helin, E.; Pravdo,
   S.; Hicks, M.; Lawrence, K.; Kervin, P.; Matson, R.; Grauer, A. D.;
   Gibbs, A. R.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd,
   G. J.; Tricarico, P.; Hill, R. E.; Kowalski, R. A.; Larson, S. M.;
   McNaught, R. H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.;
   Festler, P.; McVey, T.; Valdivia, A.; Castellano, J.; Ferrando,
   R.; Vidal, J. R.; Dupouy, P.; Baldris, F.; Muller, J. J.; Cozzi,
   E.; Jaeger, M.; Prosperi, E.; Vollmann, W.; Rinner, C.; Kugel, F.;
   Franco, L.; Camarasa, J.; Nicolas, J.; Bosch, J. M.; Soulier, J. F.;
   Diepvens, A.; Ohshima, Y.; Takahashi, T.; Camilleri, P.; Sostero,
   G.; Guido, E.; Bryssinck, E.; Chestnov, D.; Novichonok, A.; Plaksa,
   S.; Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.; Magain,
   P.; Buczynski, D.; Fraga, A.; Losse, F.; Pena Ciriza, F.; Del Maes,
   A.; Muler, G.; Ruiz, J. M.; Williams, G. V.
Bibcode: 2011MPEC....J...52T
Altcode:
  No abstract at ADS

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.; Magain,
   P.; Levesque, M.; Christiaens, V.
Bibcode: 2011MPC..75004..11J
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Tesi, L.; Bacci, P.; Garozzo, M.; Mikuz, B.; Mikuz, H.;
   Knoefel, A.; Lehmann, G.; Vilagi, J.; Kornos, L.; Haver, R.; Jaeger,
   M.; Prosperi, E.; Vollmann, W.; Buzzi, L.; Naves, R.; Campas, M.;
   Hasubick, W.; Donati, S.; Ligustri, R.; Brunato, P.; Kadota, K.; Abe,
   H.; Seki, T.; Shimomoto, S.; Sato, H.; Endate, K.; Sanchez, A.; Kuli,
   Z.; Sarneczky, K.; Christie, G. W.; Natusch, T.; Bill, H.; Quadri, U.;
   Strabla, L.; Girelli, R.; Kashuba, S.; Gorbanev, Y.; Podlesnyak, S.;
   Stogneeva, I.; Baransky, A.; Zhdanov, A.; Vorontseva, A.; Markov, Y.;
   Bressi, T. H.; Scotti, J. V.; Grauer, A. D.; Boattini, A.; Tricarico,
   P.; Kowalski, R. A.; Hill, R. E.; Ahern, J. D.; Beshore, E. C.;
   Garradd, G. J.; Gibbs, A. R.; Tric, P.; Larson, S. M.; McNaught,
   R. H.; Tricario, P.; Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.;
   Festler, P.; McVey, T.; Valdivia, A.; Durig, D. T.; Caine, C. S.;
   Green, J. P.; Best, H. L.; Hamilton, I. G.; Liu, H.; Skidmore, L. M.;
   Stinson, J. W.; Cowan, W. M.; Ikari, Y.; Castellano, J.; Dymock, R.;
   Vidal, J. R.; Dupouy, P.; Storey, D.; Mueller, J. J.; Cozzi, E.;
   Rinner, C.; Kugel, F.; Franco, L.; Shurpakov, S.; Pietschnig, M.;
   Aymami, J. M.; Nevski, V.; Linder, J.; Bel, J.; Overhaus, C.; Bosch,
   J. M.; Haeusler, B.; Noel, T.; Bryssinck, E.; Sachot, G.; Soulier,
   J. F.; Diepvens, A.; Zilch, T.; Gao, X.; Hui, M. -T.; Plyachshenko,
   Y.; Curtis, I.; Hills, K.; Takahashi, T.; Camilleri, P.; Chestnov,
   D.; Novichonok, A.; Plaksa, S.; Baroni, S.; Concari, P.; Foglia, S.;
   Galli, G.; Tombelli, M.; Sostero, G.; Guido, E.; Kiely, W.; Herald,
   D.; McCormick, J.; Primak, N.; Schultz, A.; Watters, S.; Thiel, J.;
   Goggia, T.; Hergenrother, C. W.; Elenin, L.; Holmes, R.; Vorobjov, T.;
   Haugh, T.; Sherrod, P. C.; Bell, C.; Tifner, F.; Jehin, E.; Manfroid,
   J.; Gillon, M.; Hutsemekers, D.; Magain, P.; Eugenio Tapia Ayuga, C.;
   Losse, F.; Limon, F.; Gonzalez, J.; Martin, J. J.; Garcia, F.; Muler,
   G.; Ruiz, J. M.; Canales, O.; Temprano, J.; Lacruz, J.; Fletcher,
   J.; Williams, G. V.
Bibcode: 2011MPEC....G...58T
Altcode:
  No abstract at ADS

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.; Magain,
   P.; Christiaens, V.
Bibcode: 2011MPC..74632...9J
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..74333..40J
Altcode:
  No abstract at ADS

Title: Observations and Orbits of Comets
Authors: Tombelli, M.; Foglia, S.; Interrante, G.; Masotti, E.;
   Castro, L.; Casali, M.; Marinello, W.; Micheli, M.; Pizzetti, G.;
   Soffiantini, A.; Buzzi, L.; Almendros, I.; Naves, R.; Campas, M.;
   Reina, E.; Ligustri, R.; Brunato, P.; Turchetti, R.; Benvenuti, M.;
   Scotti, J. V.; Asami, A.; Hashimoto, N.; Nishiyama, K.; Okumura, S.;
   Sakamoto, T.; Urakawa, S.; Abe, H.; Seki, T.; Shimomoto, S.; Sato, H.;
   Endate, K.; McAndrew, S. G.; Donato, L.; Gonano, V.; Travagini, M.;
   Kelemen, J.; Baransky, A.; Zhdanov, A.; Pasichnyk, P.; Ponomarenko,
   V.; Vorontseva, A.; Markov, Y.; Barinova, K.; Tarasenko, Y.; Hill,
   R. E.; Ahern, J. D.; Beshore, E. C.; Boattini, A.; Garradd, G. J.;
   Gibbs, A. R.; Tricarico, P.; Grauer, A. D.; Kowalski, R. A.; Larson,
   S. M.; McNaught, R. H.; Blythe, M.; Spitz, G.; Brungard, R.; Paige,
   J.; Festler, P.; McVey, T.; Valdivia, A.; Mackintosh, R.; Konishi,
   M.; Durig, D. T.; Green, J. P.; Maxey, S. H.; Patton, J. E.; Stevens,
   D. S.; Singer, J. T.; Skidmore, L. M.; Morgan, W. R.; Vines, L. F.;
   Castellano, J.; Ferrando, R.; Ferrando, M.; Vidal, J. R.; Dupouy,
   P.; Mueller, J. J.; Jaeger, M.; Prosperi, E.; Prosperi, S.; Vollmann,
   W.; Rinner, C.; Kugel, F.; Nevski, V.; Haeusler, B.; Bryssinck, E.;
   Soulier, J. F.; Diepvens, A.; Shurpakov, S.; Hui, M. -T.; Sugiyama,
   Y.; Camilleri, P.; Plaksa, S.; Primak, N.; Schultz, A.; Watters,
   S.; Thiel, J.; Goggia, T.; Chestnov, D.; Novichonok, A.; Elenin,
   L.; Molotov, I.; Sherrod, P. C.; Bell, C.; Jehin, E.; Manfroid,
   J.; Gillon, M.; Hutsemekers, D.; Magain, P.; Gonzalez, J.; Garcia,
   R.; Pena Ciriza, F.; Del Maes, A.; Baez, J.; Garcia, F.; Muler, G.;
   Ruiz, J. M.; Henriquez, J. A.; Canales, O.; Curto, J.; Temprano, J.;
   Pascual, J. I.; Williams, G. V.
Bibcode: 2011MPEC....G...90T
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..73990..25J
Altcode:
  No abstract at ADS

Title: Minor Planet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..74232...7J
Altcode:
  No abstract at ADS

Title: TRAPPIST: a robotic telescope dedicated to the study of
    planetary systems
Authors: Gillon, M.; Jehin, E.; Magain, P.; Chantry, V.; Hutsemékers,
   D.; Manfroid, J.; Queloz, D.; Udry, S.
Bibcode: 2011EPJWC..1106002G
Altcode: 2011arXiv1101.5807G
  We present here a new robotic telescope called TRAPPIST (TRAnsiting
  Planets and PlanetesImals Small Telescope). Equipped with a high-quality
  CCD camera mounted on a 0.6 meter light weight optical tube, TRAPPIST
  has been installed in April 2010 at the ESO La Silla Observatory
  (Chile), and is now beginning its scientific program. The science goal
  of TRAPPIST is the study of planetary systems through two approaches:
  the detection and study of exoplanets, and the study of comets. We
  describe here the objectives of the project, the hardware, and we
  present some of the first results obtained during the commissioning
  phase.

Title: Observations and Orbits of Comets
Authors: Gajdos, S.; Vilagi, J.; Apitzsch, R.; Buzzi, L.; Ligustri,
   R.; Kadota, K.; Asami, A.; Seki, T.; Muraoka, K.; Shimomoto, S.;
   Donato, L.; Gonano, V.; Jung, M.; Bill, H.; Kelemen, J.; Kashuba, S.;
   Kashuba, V.; Gorbanev, Y.; Podlesnyak, S.; Stogneeva, I.; Baransky,
   A.; Ponomarenko, V.; Simon, A.; Boattini, A.; Ahern, J. D.; Beshore,
   E. C.; Garradd, G. J.; Gibbs, A. R.; Grauer, A. D.; Hill, R. E.;
   Kowalski, R. A.; Larson, S. M.; McNaught, R. H.; Blythe, M.; Spitz,
   G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.; Valdivia, A.;
   Ikari, Y.; Castellano, J.; Kocher, P.; Rinner, C.; Kugel, F.; Bacci,
   P.; Enzo, R.; Emilio, R.; Martignoni, M.; Bryssinck, E.; Soulier, J.;
   Curtis, I.; Hills, K.; Takahashi, T.; Camilleri, P.; Sato, H.; Herald,
   D.; Drummond, J.; Dymock, R.; Chestnov, D.; Novichonok, A.; Linder,
   J.; Baroni, S.; Concari, P.; Foglia, S.; Galli, G.; Tombelli, M.;
   Elenin, L.; Molotov, I.; Bell, C.; Jehin, E.; Manfroid, J.; Gillon,
   M.; Hutsemekers, D.; Magain, P.; Carreno, A.; Piqueras, J.; Hernandez,
   J. F.; Garcia, F.; Muler, G.; Ruiz, J. M.; Williams, G. V.
Bibcode: 2011MPEC....D...36G
Altcode:
  No abstract at ADS

Title: Comet Observations [I40 La Silla--TRAPPIST]
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2011MPC..73618..49J
Altcode:
  No abstract at ADS

Title: Comet P/2005 l1 (mcnaught)
Authors: Honkova, M.; Tichy, M.; Ticha, J.; Kocer, M.; Bilkina, B.;
   Tesi, L.; Fagioli, G.; Bacci, P.; Mikuz, H.; Gajdos, S.; Vilagi, J.;
   Casali, M.; Marinello, W.; Micheli, M.; Pizzetti, G.; Soffiantini, A.;
   Galli, G.; Buzzi, L.; Almendros, I.; Naves, R.; Campas, M.; Hasubick,
   W.; Scotti, J. V.; Asami, A.; Nishiyama, K.; Kadota, K.; Abe, H.;
   Seki, T.; Shimomoto, S.; Sato, H.; Muraoka, K.; Wakuda, S.; Kuli, Z.;
   Sarneczky, K.; Donato, L.; Gonano, V.; Muschallik, I.; Peters, J. P.;
   Bill, H.; Elliott, G. T.; Tholen, D. J.; Pittichova, J.; Kleyna, J.;
   Ishiguro, M.; Baransky, A.; Baransky, B.; Baranska, O.; Grauer, A. D.;
   Kowalski, R. A.; Boattini, A.; Hill, R. E.; Ahern, J. D.; Beshore,
   E. C.; Garradd, G. J.; Gibbs, A. R.; Larson, S. M.; McNaught, R. H.;
   Blythe, M.; Spitz, G.; Brungard, R.; Paige, J.; Festler, P.; McVey, T.;
   Valdivia, A.; Durig, D. T.; Murphree, V. J.; Wetherbee, R. M.; Liu,
   H.; Caine, C. S.; Hamilton, I. G.; Ikari, Y.; Le Corre, L.; Reddy,
   V.; Dyvig, R.; Castellano, J.; Vidal, J. R.; Dupouy, P.; Baldris,
   F.; Cortes, E.; Jaeger, M.; Prosperi, E.; Prosperi, S.; Vollmann,
   W.; Rinner, C.; Kugel, F.; Trigo-Rodriguez, J. M.; Camarasa, J.;
   Bel, J.; Lopesino, J.; Borghini, W.; Bosch, J. M.; Martignoni, M.;
   Haeusler, B.; Noel, T.; Bryssinck, E.; Bros, X.; Sachot, G.; Soulier,
   J.; Rhemann, G.; Chestnov, D.; Matkin, A.; de Groote, B.; Diepvens,
   A.; Xu, Z.; Gao, X.; Ohshima, Y.; Sugiyama, Y.; Hills, K.; Takahashi,
   T.; Shurpakov, S.; Linder, J.; Sostero, G.; Guido, E.; Novichonok,
   A.; McCusker, C.; McInteggart, H.; Adams, J.; Camilleri, P.; Dymock,
   R.; Glinos, T.; Ryan, W. H.; Ryan, E. V.; Ligustri, R.; Plaksa, S.;
   Baroni, S.; Concari, P.; Foglia, S.; Tombelli, M.; Karge, S.; Elenin,
   L.; Molotov, I.; Sherrod, P. C.; Bell, C.; Renzi, M.; Jehin, E.;
   Manfroid, J.; Gillon, M.; Hutsemekers, D.; Magain, P.; Limon, F.;
   Gonzalez, J.; Carreno, A.; Piqueras, J.; Hernandez, J. F.; Martin,
   J. J.; Baez, J.; Garcia, F.; Ruiz, J. M.; Muler, G.; Benavides, R.;
   Curto, J.; Temprano, J.; Pascual, J. I.; Climent, T.; Williams, G. V.
Bibcode: 2011MPEC....D...06H
Altcode:
  No abstract at ADS

Title: (596) Scheila
Authors: Jehin, E.; Manfroid, J.; Hutsemekers, D.; Gillon, M.;
   Magain, P.
Bibcode: 2011CBET.2632....2J
Altcode:
  E. Jehin, J. Manfroid, D. Hutsemekers, M. Gillon, and P. Magain,
  Fonds National de la Recherche Scientifique, Liege University, report
  on broad- and narrow-band imaging of the (596) Scheila outburst
  (CBET 2583) with the TRAPPIST 0.60-m telescope at La Silla, and
  on optical spectroscopy with the European Southern Observatory's
  Very Large Telescope (VLT) at Paranal. R-band imaging from 2010
  Dec. 12.3 to 21.3 UT revealed two arc-like coma features expanding
  at a regular pace. The first such feature was 1' long on 2010
  Dec. 12, oriented to the northeast and bending to p.a. 280 deg
  (the anti-solar direction). The second feature was shorter, 30"
  on Dec. 12, oriented to the south and bending to p.a. 230 deg. Both
  features were getting larger and fainter with time (4' and 2' long,
  respectively, on Dec. 21.3). A narrow 45"-long tail, opposite the sun
  (p.a. 280 deg), was also observed in good seeing. R-band images taken
  on 2011 Jan. 4.3 and 5.3 after the full moon allowed Jehin et al. to
  again observe these features, seen as 7' and 4' long, respectively --
  and much fainter. This discards any sustained activity of the minor
  planet. Narrow-band images obtained on 2010 Dec. 12.3 with cometary
  filters do not show any contribution from gases. A 20-min optical
  spectrum was obtained with FORS2 at the VLT on Dec. 13.3; it does not
  show any extended cometary gaseous emissions, but only a spatially
  extended continuum due to dust-scattered sunlight. Short B, V, R,
  and I exposures performed nearly every two nights from 2010 Dec. 12.3
  to 2011 Jan. 5.3 give a magnitude for the nuclear condensation of V =
  14.2 +/- 0.1 over the whole period, in agreement with the "APmag" value
  reported in the Jet Propulsion Laboratory ephemeris. No flux variation
  of the nuclear condensation was observed. Those preliminary results are
  in favor of a collisional scenario to explain the outburst of (596)
  Scheila, rather than a cometary driven activity. This case might be
  similar to the outburst of comet P/2010 A2, which may have resulted
  from an impact of a minor planet (Snodgrass 2010, Nature 467, 814).

Title: Comet 103P/Hartley
Authors: Jehin, E.; Manfroid, J.; Hutsemekers, D.; Gillon, M.;
   Magain, P.
Bibcode: 2010CBET.2589....1J
Altcode:
  E. Jehin, J. Manfroid, D. Hutsemekers, M. Gillon, and P. Magain, Liege
  University, report narrowband imaging of comet 103P using the TRAPPIST
  0.60m telescope at the European Southern Observatory, La Silla. Three to
  four hours of observation were secured on 26 clear nights from Oct. 29
  to Dec. 7, using six different cometary filters (Farnham et al. 2000,
  Icarus 147, 180). The flux of five gaseous species (CN, OH, H_2O+,
  C_2, C_3) and the dust continuum (via the C/1995 O1 green continuum
  filter, GC) was measured in a 26" aperture. Periodic variations of
  the gas species are observed, superimposed on the long-term trend,
  with CN showing the strongest variations (0.4-mag amplitude). The dust
  light curve is nearly flat. No gas or dust outburst has been detected
  during the above period of observation, although CN and OH show a
  slow flux increase with respect to other species during several days
  in early November. A period search with the first two weeks of data
  gave a smooth phase diagram for a period of 18.4 +/- 0.3 hours. These
  observations are in good agreement with the period reported from Arecibo
  radar observations of the nucleus (18.1 +/- 0.3 hours on Oct. 24-27;
  IAUC 9179). Including two more weeks of data, it became clear that
  the period was increasing. A change from about 18.2 to 19 hours was
  derived during the above observing window that might be related to a
  change of the rotation period of comet 103P of about 2 hours in 100
  days. Such a rapid slowing down is in agreement with rotation values
  reported before perihelion (16.6 +/- 0.5 hr on Aug. 13-17; IAUC 9163).

Title: Occultation by (136199) Eris
Authors: Jehin, E.; Manfroid, J.; Gillon, M.; Hutsemekers, D.;
   Magain, P.
Bibcode: 2010IAUC.9184....2J
Altcode: 2010IAUC.9184B...2J
  E. Jehin, J. Manfroid, M. Gillon, D. Hutsemekers, and P. Magain report
  that they observed an occultation of a star of magnitude I about 15.2
  by the dwarf planet Eris (then at V about 18.7) on Nov. 6 using the new
  telescope TRAPPIST at the European Southern Observatory (La Silla). A
  series of 3-s exposures of a field of size 3' x 3' (1".3/pixel) were
  secured in fast-readout mode (with a deadtime of 1.5 s), starting at
  01h50m UT for one hour. Seven frames centered at 02h19m34s UT allowed
  them to derive the start of the occultation as 02h19m16s.75 +/- 0s.75
  and the end as 02h19m47s.6 +/- 0s.2, for a total occultation time of
  30.4 +/- 1.0 seconds. The predictions (see above) made by the Rio de
  Janeiro group (Assafin et al., Nov. 5) and by J. L. Ortiz estimated the
  time of the occultation around 02h18m UT for Chile, in good agreement
  with the observations. During the occultation, a point source is
  detected with a magnitude corresponding to that of Eris. A small flux
  increase was also seen at the middle of the occultation, which might
  result from refraction in Eris' atmosphere (Elliot and Olkin 1996,
  Ann. Rev. Earth Planet. Sci. 24, 89). Eris is by far the most-remote
  solar-system object observed to date via stellar occultation, with a
  geocentric distance of about 96 AU. TRAPPIST is a project driven by
  the University of Liege, in close collaboration with the Observatory
  of Geneva, supported by the Belgian Fund for Scientific Research and
  the Swiss National Science Foundation.

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses. VIII. Deconvolution of high resolution near-IR images and
    simple mass models for 7 gravitationally lensed quasars
Authors: Chantry, V.; Sluse, D.; Magain, P.
Bibcode: 2010A&A...522A..95C
Altcode: 2010arXiv1007.3142C
  <BR /> Aims: We attempt to place very accurate positional constraints
  on seven gravitationally lensed quasars currently being monitored
  by the COSMOGRAIL collaboration, and shape parameters for the light
  distribution of the lensing galaxy. We attempt to determine simple
  mass models that reproduce the observed configuration and predict time
  delays. We finally test, for the quads, whether there is evidence of
  astrometric perturbations produced by substructures in the lensing
  galaxy, which may preclude a good fit with the simple models. <BR />
  Methods: We apply the iterative MCS deconvolution method to near-IR
  HST archival data of seven gravitationally lensed quasars. This
  deconvolution method allows us to differentiate the contributions of
  the point sources from those of extended structures such as Einstein
  rings. This method leads to an accuracy of 1-2 mas in the relative
  positions of the sources and lens. The limiting factor of the method
  is the uncertainty in the instrumental geometric distortions. We then
  compute mass models of the lensing galaxy using state-of-the-art
  modeling techniques. <BR /> Results: We determine the relative
  positions of the lensed images and lens shape parameters of seven
  lensed quasars: HE 0047-1756, RX J1131-1231, SDSS J1138+0314, SDSS
  J1155+6346, SDSS J1226-0006, WFI J2026-4536, and HS 2209+1914. The
  lensed image positions are derived with 1-2 mas accuracy. Isothermal
  and de Vaucouleurs mass models are calculated for the whole sample. The
  effect of the lens environment on the lens mass models is taken into
  account with a shear term. Doubly imaged quasars are equally well
  fitted by each of these models. A large amount of shear is necessary
  to reproduce SDSS J1155+6346 and SDSS J1226-006. In the latter case, we
  identify a nearby galaxy as the dominant source of shear. The quadruply
  imaged quasar SDSS J1138+0314 is reproduced well by simple lens models,
  which is not the case for the two other quads, RX J1131-1231 and WFI
  J2026-4536. This might be the signature of astrometric perturbations
  caused by massive substructures in the galaxy, which are unaccounted
  for by the models. Other possible explanations are also presented. <P
  />Based on observations made with the NASA/ESA HST Hubble Space
  Telescope, obtained from the data archive at the Space Science
  Institute, which is operated by AURA, the Association of Universities
  for Research in Astronomy, Inc., under NASA contract NAS-5-26555.

Title: The 3/4 July 2010 Pluto Stellar-Occultation Observations
Authors: Pasachoff, Jay M.; Elliot, J. L.; Souza, S. P.; Person, M. J.;
   Zuluaga, C.; Bosh, A. S.; Zangari, A. M.; Jensen-Clem, R.; Lockhart,
   M.; Gulbis, A. A. S.; Rojo, P.; Lu, M.; Malamut, C.; Levine, S. E.;
   Ivarsen, K. M.; Reichart, D. E.; LaCluyze, A. P.; Nysewander, M. C.;
   Haislip, J. B.; MacDonald, R. K. D.; Bailyn, C. D.; Emilio, M.; Jehin,
   E.; Gillon, M.; Manfroid, J.; Chantry, V.; Magain, P.; Hutsemekers,
   D.; Queloz, D.
Bibcode: 2010DPS....42.2002P
Altcode: 2010BAAS...42Q.983P
  Continuing our monitoring of Pluto's atmospheric temperature and
  pressure, previously shown by us to be increasing (Elliot et al.,
  Nature 424, 165, 2003; Pasachoff et al., AJ 129, 1718, 2005)
  and subsequently found by us to be leveling off (Elliot et al.,
  AJ 134, 1, 2007), we report on a stellar occultation by Pluto of
  UCAC2 mag=15.3, observed from South America and Africa on 4 July
  2010 UT. Success was achieved with a 0.45 m at Cerro Calan using
  one of our POETS (Portable Occultation, Eclipse, and Transit System;
  Souza et al. PASP 118, 1550, 2006), a 1.0 SMARTS (Small and Medium
  Aperture Research Telescope System) at Cerro Tololo, four 0.6 m
  telescopes of PROMPT (Panchromatic Robotic Optical Monitoring and
  Polarimetry Telescopes) on Cerro Tololo, and TRAPPIST's (TRansiting
  Planets and Planetesimals Small Telescope) 0.6-m telescope on La
  Silla in Chile; the 0.35 m telescope of U. Ponta Grossa, Brazil;
  and the 0.75-m ATOM (Automatic Telescope for Optical Monitoring),
  Namibia, using POETS. Winds prevented opening the 6.5 m Magellan/Clay
  telescope on Las Campanas, Chile, with its own frame-transfer camera,
  and clouds obscured the 1.9 m telescope at Sutherland, South Africa,
  which had POETS. With shadow velocity 23.6 km/s, it was a rapid event:
  maximum occultation &lt;2 minutes. <P />The observations were supported
  in part by grants NNX08AO50G to Williams College and NNX10AB27G to
  MIT from NASA's Planetary Astronomy Division, and NNH08AI17I to USNO
  for astrometry. Student participation was supported in part by NASA's
  Massachusetts Space Grant and NSF's REU. Japan's government donated
  U. Chile's Cerro Calan Goto telescope. PROMPT observations were made
  possible by the Robert Martin Ayers Science Fund. TRAPPIST is a project
  driven by the University of Liège, in close collaboration with the
  Observatory of Geneva, supported by the Belgian Fund for Scientific
  Research and the Swiss National Science Foundation.

Title: TRAPPIST : un télescope liégeois à la découverte des
    systèmes planétaires
Authors: Jehin, E.; Gillon, M.; Chantry, V.; Magain, P.
Bibcode: 2010Ciel...72..326J
Altcode:
  No abstract at ADS

Title: The Spitzer search for the transits of HARPS low-mass
    planets. I. No transit for the super-Earth HD 40307b
Authors: Gillon, M.; Deming, D.; Demory, B. -O.; Lovis, C.; Seager,
   S.; Mayor, M.; Pepe, F.; Queloz, D.; Segransan, D.; Udry, S.; Delmelle,
   S.; Magain, P.
Bibcode: 2010A&A...518A..25G
Altcode: 2010arXiv1002.4707G
  We used Spitzer and its IRAC camera to search for the transit of the
  super-Earth HD 40307b. The hypothesis that the planet transits could not
  be firmly discarded from our first photometric monitoring of a transit
  window because of the uncertainty coming from the modeling of the
  photometric baseline. To obtain a firm result, two more transit windows
  were observed and a global Bayesian analysis of the three IRAC time
  series and the HARPS radial velocities was performed. Unfortunately,
  the hypothesis that the planet transited during the observed phase
  window is firmly rejected, while the probability that the planet
  does transit but that the eclipse was missed by our observations
  is nearly negligible (0.26%). <P />The photometric time series
  used in this work are only available in electronic form at the CDS
  via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via <A
  href="http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/518/A25">http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/518/A25</A>

Title: VizieR Online Data Catalog: Transits of HD40307b by Spitzer
    (Gillon+, 2010)
Authors: Gillon, M.; Deming, D.; Demory, B. -O.; Lovis, C.; Seager,
   S.; Mayor, M.; Pepe, F.; Queloz, D.; Segransan, D.; Udry, S.; Delmelle,
   S.; Magain, P.
Bibcode: 2010yCat..35180025G
Altcode: 2010yCat..35189025G
  We used Spitzer and its IRAC camera to search for the transit of the
  super-Earth HD 40307b. The hypothesis that the planet transits could not
  be firmly discarded from our first photometric monitoring of a transit
  window because of the uncertainty coming from the modeling of the
  photometric baseline. To obtain a firm result, two more transit windows
  were observed and a global Bayesian analysis of the three IRAC time
  series and the HARPS radial velocities was performed. Unfortunately,
  the hypothesis that the planet transited during the observed phase
  window is firmly rejected, while the probability that the planet does
  transit but that the eclipse was missed by our observations is nearly
  negligible (0.26%) <P />(3 data files).

Title: Deep near-infrared imaging of the HE0450-2958 system
Authors: Letawe, G.; Magain, P.
Bibcode: 2010A&A...515A..84L
Altcode: 2010arXiv1003.3746L
  Context. The QSO HE0450-2958 and the companion galaxy with which it
  is interacting, both ultra luminous in the infrared, have been the
  subject of much attention in recent years, as the quasar host galaxy
  remained undetected. This led to various interpretations on QSO and
  galaxy formation and co-evolution, such as black hole ejection, jet
  induced star formation, dust obscured galaxy, or normal host below the
  detection limit. <BR /> Aims: We carried out deep observations in the
  near-IR in order to solve the puzzle concerning the existence of any
  host. <BR /> Methods: The object was observed with the ESO VLT and
  HAWK-I in the near-IR J-band for 8 h. The images have been processed
  with the MCS deconvolution method, permitting accurate subtraction
  of the QSO light from the observations. <BR /> Results: The compact
  emission region situated close to the QSO, called the blob, which
  previously showed only gas emission lines in the optical spectra, is
  now detected in our near-IR images. Its high brightness implies that
  stars likely contribute to the near-IR emission. The blob might thus
  be interpreted as an off-centre, bright and very compact host galaxy,
  involved in a violent collision with its companion.

Title: Eclipsing binary candidates in Corot-IRa01 field (Carpano+,
    2009)
Authors: Carpano, S.; Cabrera, J.; Alonso, R.; Barge, P.; Aigrain, S.;
   Almenara, J. -M.; Borde, P.; Bouchy, F.; Carone, L.; Deeg, H. J.;
   de La, Reza R.; Deleuil, M.; Dvorak, R.; Erikson, A.; Fressin,
   F.; Fridlund, M.; Gondoin, P.; Guillot, T.; Hatzes, A.; Jorda, L.;
   Lammer, H.; Leger, A.; Llebaria, A.; Magain, P.; Moutou, C.; Ofir, A.;
   Ollivier, M.; Janot-Pacheco, E.; Paetzold, M.; Pont, F.; Queloz, D.;
   Rauer, H.; Regulo, C.; Renner, S.; Rouan, D.; Samuel, B.; Schneider,
   J.; Wuchterl, G.
Bibcode: 2010yCat..35060491C
Altcode:
  CoRoT observed its first field from early February 2008 until early
  April, for approximatively 60 days. The run code "IRa01" is explained as
  following. The "IR" means "initial run" in contrast to the subsequent
  "long runs" (LR) and "short runs" (SR). The third letter refers to
  the direction with respect to the Galactic center ("a", as in this
  case, anticenter or "c" Galactic center). The last two digits are the
  sequence for this type of observation (01 being the first one). <P
  />(1 data file).

Title: The Power of Deconvolution for Study of QSO Host Galaxies
Authors: Letawe, Géraldine; Letawe, Yannick; Magain, Pierre
Bibcode: 2010IAUS..267..117L
Altcode:
  The major challenge in studying QSO host galaxies is to remove the
  QSO contribution, which often outshines the whole system. Our group
  has acquired the technical ability to handle such data, for images
  and slit spectroscopy, as well as integral field spectroscopy. We
  review here the major techniques developed by our team, and their
  latest applications. We are open for collaboration with other teams
  to spread the use of these powerful techniques.

Title: Study of a homogeneous QSO sample: relations between the QSO
    and its host galaxy
Authors: Letawe, Y.; Letawe, G.; Magain, P.
Bibcode: 2010MNRAS.403.2088L
Altcode: 2010arXiv1001.0463L; 2010MNRAS.tmp..217L
  We analyse a sample of 69 quasi-stellar objects (QSOs) which have
  been randomly selected in a complete sample of 104 QSOs (R &lt;=
  18,0.142 &lt; z &lt; 0.198,δ &lt; 10°). 60 have been observed with
  the NTT/SUSI2 at La Silla, through two filters in the optical band
  (WB 655 and V 812), and the remaining nine are taken from archive data
  bases. The filter V 812 contains the redshifted Hβ and forbidden
  [OIII] emission lines, while WB 655 covers a spectral region devoid
  of emission lines, thus measuring the QSO and stellar continua. The
  contributions of the QSO and the host are separated thanks to the MCS
  deconvolution algorithm, allowing a morphological classification of the
  host, and the computation of several parameters such as the host and
  nucleus absolute V magnitude, distance between the luminosity centre of
  the host and the QSO and colour of the host and nucleus. We define a
  new asymmetry coefficient, independent of any galaxy models and well
  suited for QSO host studies. The main results from this study are
  (i) 25 per cent of the total number of QSO hosts are spirals, 51 per
  cent are ellipticals and 60 per cent show signs of interaction, (ii)
  highly asymmetric systems tend to have a higher gas ionization level and
  (iii) elliptical hosts contain a substantial amount of ionized gas and
  some show off-nuclear activity. These results agree with hierarchical
  models merger driven evolution. <P />Based on observations collected
  at the European Organisation for Astronomical Research in the Southern
  Hemisphere, Chile, under programme IDs 77.B-0229 and 78.B-0081. <P
  />E-mail: gletawe@ulg.ac.be

Title: Transiting exoplanets from the CoRoT space
mission. IX. CoRoT-6b: a transiting ``hot Jupiter'' planet in an
    8.9d orbit around a low-metallicity star
Authors: Fridlund, M.; Hébrard, G.; Alonso, R.; Deleuil, M.;
   Gandolfi, D.; Gillon, M.; Bruntt, H.; Alapini, A.; Csizmadia, Sz.;
   Guillot, T.; Lammer, H.; Aigrain, S.; Almenara, J. M.; Auvergne, M.;
   Baglin, A.; Barge, P.; Bordé, P.; Bouchy, F.; Cabrera, J.; Carone,
   L.; Carpano, S.; Deeg, H. J.; de La Reza, R.; Dvorak, R.; Erikson,
   A.; Ferraz-Mello, S.; Guenther, E.; Gondoin, P.; den Hartog, R.;
   Hatzes, A.; Jorda, L.; Léger, A.; Llebaria, A.; Magain, P.; Mazeh,
   T.; Moutou, C.; Ollivier, M.; Pätzold, M.; Queloz, D.; Rauer, H.;
   Rouan, D.; Samuel, B.; Schneider, J.; Shporer, A.; Stecklum, B.;
   Tingley, B.; Weingrill, J.; Wuchterl, G.
Bibcode: 2010A&A...512A..14F
Altcode: 2010arXiv1001.1426F
  The CoRoT satellite exoplanetary team announces its sixth transiting
  planet in this paper. We describe and discuss the satellite observations
  as well as the complementary ground-based observations - photometric and
  spectroscopic - carried out to assess the planetary nature of the object
  and determine its specific physical parameters. The discovery reported
  here is a “hot Jupiter” planet in an 8.9d orbit, 18 stellar radii,
  or 0.08 AU, away from its primary star, which is a solar-type star
  (F9V) with an estimated age of 3.0 Gyr. The planet mass is close to
  3 times that of Jupiter. The star has a metallicity of 0.2 dex lower
  than the Sun, and a relatively high <SUP>7</SUP>Li abundance. While
  the light curve indicates a much higher level of activity than, e.g.,
  the Sun, there is no sign of activity spectroscopically in e.g.,
  the [Ca ii] H&amp;K lines. <P />The CoRoT space mission, launched on
  December 27, 2006, has been developed and is being operated by CNES,
  with the contribution of Austria, Belgium, Brazil, ESA, The Research
  and Scientific Support Department of ESA, Germany and Spain.

Title: The thermal emission of the young and massive planet CoRoT-2b
    at 4.5 and 8 μm
Authors: Gillon, M.; Lanotte, A. A.; Barman, T.; Miller, N.; Demory,
   B. -O.; Deleuil, M.; Montalbán, J.; Bouchy, F.; Collier Cameron, A.;
   Deeg, H. J.; Fortney, J. J.; Fridlund, M.; Harrington, J.; Magain,
   P.; Moutou, C.; Queloz, D.; Rauer, H.; Rouan, D.; Schneider, J.
Bibcode: 2010A&A...511A...3G
Altcode: 2009arXiv0911.5087G
  We report measurements of the thermal emission of the young and massive
  planet CoRoT-2b at 4.5 and 8 μm with the Spitzer Infrared Array Camera
  (IRAC). Our measured occultation depths are 0.510±0.042% at 4.5 and
  0.41±0.11% at 8 μm. In addition to the CoRoT optical measurements,
  these planet/star flux ratios indicate a poor heat distribution on the
  night side of the planet and agree better with an atmosphere free of
  temperature inversion layer. Still, such an inversion is not definitely
  ruled out by the observations and a larger wavelength coverage is
  required to remove the current ambiguity. Our global analysis of CoRoT,
  Spitzer, and ground-based data confirms the high mass and large size of
  the planet with slightly revised values (M_p = 3.47±0.22 M<SUB>J</SUB>,
  R_p = 1.466±0.044 R<SUB>J</SUB>). We find a small but significant
  offset in the timing of the occultation when compared to a purely
  circular orbital solution, leading to e \cosω = -0.00291±0.00063
  where e is the orbital eccentricity and ω is the argument of
  periastron. Constraining the age of the system to at most a few hundred
  Myr and assuming that the non-zero orbital eccentricity does not come
  from a third undetected body, we modeled the coupled orbital-tidal
  evolution of the system with various tidal Q values, core sizes, and
  initial orbital parameters. For Q_s' = 10<SUP>5</SUP>-10<SUP>6</SUP>,
  our modeling is able to explain the large radius of CoRoT-2b if
  Q_p'≤ 10<SUP>5.5</SUP> through a transient tidal circularization and
  corresponding planet tidal heating event. Under this model, the planet
  will reach its Roche limit within 20 Myr at most. <P />Based on data
  collected with the VLT/FORS2 instrument at ESO Paranal Observatory,
  Chile (programs 081.C-0413(B)). <P />The photometric timeseries
  used in this work are only available in electronic form at the CDS
  via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via <A
  href="http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/511/A3">http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/511/A3</A>

Title: Transit timing analysis of CoRoT-1b
Authors: Csizmadia, Sz.; Renner, S.; Barge, P.; Agol, E.; Aigrain,
   S.; Alonso, R.; Almenara, J. -M.; Bonomo, A. S.; Bordé, P.; Bouchy,
   F.; Cabrera, J.; Deeg, H. J.; de La Reza, R.; Deleuil, M.; Dvorak, R.;
   Erikson, A.; Guenther, E. W.; Fridlund, M.; Gondoin, P.; Guillot, T.;
   Hatzes, A.; Jorda, L.; Lammer, H.; Lázaro, C.; Léger, A.; Llebaria,
   A.; Magain, P.; Moutou, C.; Ollivier, M.; Pätzold, M.; Queloz, D.;
   Rauer, H.; Rouan, D.; Schneider, J.; Wuchterl, G.; Gandolfi, D.
Bibcode: 2010A&A...510A..94C
Altcode: 2009arXiv0911.3585C
  Context. CoRoT, the pioneer space-based transit search, steadily
  provides thousands of high-precision light curves with continuous
  time sampling over periods of up to 5 months. The transits of a planet
  perturbed by an additional object are not strictly periodic. By studying
  the transit timing variations (TTVs), additional objects can be detected
  in the system. <BR /> Aims: A transit timing analysis of CoRoT-1b is
  carried out to constrain the existence of additional planets in the
  system. <BR /> Methods: We used data obtained by an improved version of
  the CoRoT data pipeline (version 2.0). Individual transits were fitted
  to determine the mid-transit times, and we analyzed the derived O-C
  diagram. N-body integrations were used to place limits on secondary
  planets. <BR /> Results: No periodic timing variations with a period
  shorter than the observational window (55 days) are found. The presence
  of an Earth-mass Trojan is not likely. A planet of mass greater than
  ~1 Earth mass can be ruled out by the present data if the object is
  in a 2:1 (exterior) mean motion resonance with CoRoT-1b. Considering
  initially circular orbits: (i) super-Earths (less than 10 Earth-masses)
  are excluded for periods less than about 3.5 days; (ii) Saturn-like
  planets can be ruled out for periods less than about 5 days; (iii)
  Jupiter-like planets should have a minimum orbital period of about 6.5
  days. <P />Based on observations obtained with CoRoT, a space project
  operated by the French Space Agency, CNES, with participation of the
  Science Programs of ESA, ESTEC/RSSD, Austria, Belgium, Brazil, Germany,
  and Spain.

Title: High-dispersion infrared spectroscopic observations of comet
    8P/Tuttle with VLT/CRIRES
Authors: Kobayashi, H.; Bockelée-Morvan, D.; Kawakita, H.; Dello
   Russo, N.; Jehin, E.; Manfroid, J.; Smette, A.; Hutsemékers,
   D.; Stüwe, J.; Weiler, M.; Arpigny, C.; Biver, N.; Cochran, A.;
   Crovisier, J.; Magain, P.; Sana, H.; Schulz, R.; Vervack, R. J.;
   Weaver, H.; Zucconi, J. -M.
Bibcode: 2010A&A...509A..80K
Altcode:
  We report on the composition of the Halley-family comet (HFC) 8P/Tuttle
  investigated with high-dispersion near-infrared spectroscopic
  observations. The observations were carried out at the ESO VLT
  (Very Large Telescope) with the CRIRES instrument as part of a
  multi-wavelength observation campaign of 8P/Tuttle performed in late
  January and early February 2008. Radar observations suggested that
  8P/Tuttle is a contact binary, and it was proposed that these components
  might be heterogeneous in chemistry. We determined mixing ratios of
  organic volatiles with respect to H<SUB>2</SUB>O and found that mixing
  ratios were consistent with previous near infrared spectroscopic
  observations obtained in late December 2007 and in late January
  2008. It has been suggested that because 8P/Tuttle is a contact binary,
  it might be chemically heterogeneous. However, we find no evidence
  for chemical heterogeneity within the nucleus of 8P/Tuttle. We also
  compared the mixing ratios of organic molecules in 8P/Tuttle with those
  of both other HFCs and long period comets (LPCs) and found that HCN,
  C<SUB>2</SUB>H<SUB>2</SUB>, and C<SUB>2</SUB>H<SUB>6</SUB> are depleted
  whereas CH<SUB>4</SUB> and CH<SUB>3</SUB>OH have normal abundances. This
  may indicate that 8P/Tuttle was formed in a different region of the
  early solar nebula than other HFCs and LPCs. We estimated the conversion
  efficiency from C<SUB>2</SUB>H<SUB>2</SUB> to C<SUB>2</SUB>H<SUB>6</SUB>
  by hydrogen addition reactions on cold grains by employing the
  C<SUB>2</SUB>H<SUB>6</SUB>/(C<SUB>2</SUB>H<SUB>6</SUB>+C<SUB>2</SUB>H<SUB>2</SUB>)
  ratio. The
  C<SUB>2</SUB>H<SUB>6</SUB>/(C<SUB>2</SUB>H<SUB>6</SUB>+C<SUB>2</SUB>H<SUB>2</SUB>)
  ratio in 8P/Tuttle is consistent with the ratios found in other
  HFCs and LPCs within the error bars. We also discuss the source of
  C<SUB>2</SUB> and CN based on our observations and conclude that the
  abundances of C<SUB>2</SUB>H<SUB>2</SUB> and C<SUB>2</SUB>H<SUB>6</SUB>
  are insufficient to explain the C<SUB>2</SUB> abundances in comet
  8P/Tuttle and that the abundance of HCN is insufficient to explain
  the CN abundances in the comet, so at least one additional parent is
  needed for each species, as pointed out in previous study. <P />Based on
  observations collected at the European Southern Observatory, Paranal,
  Chile (ESO Prog. 080.C-0615 and 280.C-5053).We regret to note the
  death of Dr. J. -M. Zucconi in 2009 May.

Title: Eclipsing binaries in CoRoT-LRc01 field (Cabrera+, 2009)
Authors: Cabrera, J.; Fridlund, M.; Ollivier, M.; Gandolfi, D.;
   Csizmadia, Sz.; Alonso, R.; Aigrain, S.; Alapini, A.; Almenara, J. -M.;
   Barge, P.; Bonomo, A. S.; Borde, P.; Bouchy, F.; Bruntt, H.; Carone,
   L.; Carpano, S.; Deeg, H. J.; de La, Reza R.; Deleuil, M.; Dvorak,
   R.; Erikson, A.; Gillon, M.; Gondoin, P.; Guenther, E. W.; Guillot,
   T.; Hartmann, M.; Hatzes, A.; Hebrard, G.; Jorda, L.; Lammer, H.;
   Leger, A.; Llebaria, A.; Lovis, C.; Magain, P.; Mayor, M.; Mazeh,
   T.; Moutou, C.; Ofir, A.; Paetzold, M.; Pepe, F.; Pont, F.; Queloz,
   D.; Rabus, M.; Rauer, H.; Regulo, C.; Renner, S.; Rouan, D.; Samuel,
   B.; Santerne, A.; Schneider, J.; Shporer, A.; Stecklum, B.; Tingley,
   B.; Udry, S.; Wuchterl, G.
Bibcode: 2010yCat..35060501C
Altcode:
  The 11408 targets observed by CoRoT were selected using the information
  gathered in the database Exo-Dat (Deleuil et al. 2009AJ....138..649D;
  Meunier et al. 2007, ASP Conf., 376, 339), built with dedicated ground
  based photometric observations in the visible and near IR bands from
  2MASS catalog. <P />(3 data files).

Title: Study of Quasar Host Galaxies Combining HST/ACS Images and
    VLT Spectra
Authors: Letawe, Yannick; Letawe, Géraldine; Magain, Pierre
Bibcode: 2010ASSP...15..197L
Altcode: 2010ihea.book..197L
  We present the results of a study of the host galaxies of a few bright
  low redshift quasars, based on a combination of high resolution HST/ACS
  images with deep VLT spectra. Using a version of the MCS deconvolution
  algorithm specially adapted to HST images, the light from the central
  point source can be efficiently removed, which allows to study the
  environment of the quasar down to a few hundreds of parsecs from
  the center. In a similar way, the spectra can be separated into a
  quasar contribution and a spatially resolved slit spectrum of the
  host galaxy. Combining the images and spectra allows to carry out
  a detailed analysis of the immediate environment of the quasar:
  excitation and ionization state of the gas, dynamics… Up to now,
  this method has been applied to six quasars, including the peculiar
  HE0450-2958 (Magain et al. in Nature 437:381, 2005), for which no host
  galaxy could be detected.

Title: VizieR Online Data Catalog: Light curves of CoRoT-2 in z-band,
    4.5um and 8um (Gillon+, 2010)
Authors: Gillon, M.; Lanotte, A. A.; Barman, T.; Miller, N.; Demory,
   B. -O.; Deleuil, M.; Montalban, J.; Bouchy, F.; Collier, Cameron A.;
   Deeg, H. J.; Fortney, J. J.; Fridlund, M.; Harrington, J.; Magain,
   P.; Moutou, C.; Queloz, D.; Rauer, H.; Rouan, D.; Schneider, J.
Bibcode: 2009yCat..35110003G
Altcode: 2009yCat..35119003G
  Photometric time series obtained for CoRoT-2 with the VLT/FORS2 camera
  in z band during a transit of the planet CoRoT-2b and with the SST/IRAC
  camera at 4.5 and 8um during an occultation of the same planet. <P
  />(3 data files).

Title: Transiting exoplanets from the CoRoT space mission. VII. The
    ``hot-Jupiter''-type planet CoRoT-5b
Authors: Rauer, H.; Queloz, D.; Csizmadia, Sz.; Deleuil, M.; Alonso,
   R.; Aigrain, S.; Almenara, J. M.; Auvergne, M.; Baglin, A.; Barge,
   P.; Bordé, P.; Bouchy, F.; Bruntt, H.; Cabrera, J.; Carone, L.;
   Carpano, S.; de La Reza, R.; Deeg, H. J.; Dvorak, R.; Erikson, A.;
   Fridlund, M.; Gandolfi, D.; Gillon, M.; Guillot, T.; Guenther, E.;
   Hatzes, A.; Hébrard, G.; Kabath, P.; Jorda, L.; Lammer, H.; Léger,
   A.; Llebaria, A.; Magain, P.; Mazeh, T.; Moutou, C.; Ollivier, M.;
   Pätzold, M.; Pont, F.; Rabus, M.; Renner, S.; Rouan, D.; Shporer,
   A.; Samuel, B.; Schneider, J.; Triaud, A. H. M. J.; Wuchterl, G.
Bibcode: 2009A&A...506..281R
Altcode: 2009arXiv0909.3397R
  Aims: The CoRoT space mission continues to photometrically monitor
  about 12 000 stars in its field-of-view for a series of target fields
  to search for transiting extrasolar planets ever since 2007. Deep
  transit signals can be detected quickly in the “alarm-mode”
  in parallel to the ongoing target field monitoring. CoRoT's first
  planets have been detected in this mode. <BR />Methods: The CoRoT
  raw lightcurves are filtered for orbital residuals, outliers,
  and low-frequency stellar signals. The phase folded lightcurve
  is used to fit the transit signal and derive the main planetary
  parameters. Radial velocity follow-up observations were initiated to
  secure the detection and to derive the planet mass. <BR />Results:
  We report the detection of CoRoT-5b, detected during observations
  of the LRa01 field, the first long-duration field in the galactic
  anti-center direction. CoRoT-5b is a “hot Jupiter-type”
  planet with a radius of 1.388<SUP>+0.046</SUP><SUB>-0.047</SUB>
  R_Jup, a mass of 0.467<SUP>+0.047</SUP><SUB>-0.024</SUB> M_Jup, and
  therefore, a mean density of 0.217<SUP>+0.031</SUP><SUB>-0.025</SUB>
  g cm<SUP>-3</SUP>. The planet orbits an F9V star of 14.0
  mag in 4.0378962 ± 0.0000019 days at an orbital distance of
  0.04947<SUP>+0.00026</SUP><SUB>-0.00029</SUB> AU. <P />Observations
  made with SOPHIE spectrograph at the Observatoire de Haute Provence
  (07B.PNP.MOUT), France, and HARPS spectrograph at ESO La Silla
  Observatory (072.C-0488(E), 082.C-0312(A)), and partly based on
  observations made at the Anglo-Australian Telescope. The CoRoT space
  mission, launched on December 27, 2006, was developed and is operated by
  CNES, with the contribution of Austria, Belgium, Brasil, ESA, Germany,
  and Spain.

Title: VLT transit and occultation photometry for the bloated
    planet CoRoT-1b
Authors: Gillon, M.; Demory, B. -O.; Triaud, A. H. M. J.; Barman, T.;
   Hebb, L.; Montalbán, J.; Maxted, P. F. L.; Queloz, D.; Deleuil, M.;
   Magain, P.
Bibcode: 2009A&A...506..359G
Altcode: 2009arXiv0905.4571G
  We present VLT eclipse photometry for the giant planet CoRoT-1b. We
  observed a transit in the R-band filter and an occultation in
  a narrow filter centered on 2.09 μm. Our analysis of this new
  photometry and published radial velocities, in combination
  with stellar-evolutionary modeling, leads to a planetary
  mass and radius of 1.07<SUP>+0.13</SUP><SUB>-0.18</SUB>
  M_Jup and 1.45<SUP>+0.07</SUP><SUB>-0.13</SUB> R_Jup,
  confirming the very low density previously deduced from CoRoT
  photometry. The large occultation depth that we measure at 2.09
  μm (0.278<SUP>+0.043</SUP><SUB>-0.066</SUB>%) is consistent
  with thermal emission and is better reproduced by an atmospheric
  model with no redistribution of the absorbed stellar flux to the
  night side of the planet. <P />Based on data collected with the
  VLT/FORS2 and VLT/HAWK-I instruments at ESO Paranal Observatory,
  Chile (programs 080.C-0661(B) and 382.C-0642(A)). The photometric
  time-series used in this work are only available in electronic form
  at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
  or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/359

Title: Planetary transit candidates in CoRoT-LRc01 field
Authors: Cabrera, J.; Fridlund, M.; Ollivier, M.; Gandolfi, D.;
   Csizmadia, Sz.; Alonso, R.; Aigrain, S.; Alapini, A.; Almenara, J. -M.;
   Barge, P.; Bonomo, A. S.; Bordé, P.; Bouchy, F.; Bruntt, H.; Carone,
   L.; Carpano, S.; Deeg, H. J.; de La Reza, R.; Deleuil, M.; Dvorak,
   R.; Erikson, A.; Gillon, M.; Gondoin, P.; Guenther, E. W.; Guillot,
   T.; Hartmann, M.; Hatzes, A.; Hebrard, G.; Jorda, L.; Lammer, H.;
   Léger, A.; Llebaria, A.; Lovis, C.; Magain, P.; Mayor, M.; Mazeh,
   T.; Moutou, C.; Ofir, A.; Pätzold, M.; Pepe, F.; Pont, F.; Queloz,
   D.; Rabus, M.; Rauer, H.; Régulo, C.; Renner, S.; Rouan, D.; Samuel,
   B.; Santerne, A.; Schneider, J.; Shporer, A.; Stecklum, B.; Tingley,
   B.; Udry, S.; Wuchterl, G.
Bibcode: 2009A&A...506..501C
Altcode:
  Aims: We present here the list of planetary transit candidates detected
  in the first long run observed by CoRoT: LRc01, towards the galactic
  center in the direction of Aquila, which lasted from May to October
  2007. <BR />Methods: we analyzed 3719 (33%) sources in the chromatic
  bands and 7689 in the monochromatic band. Instrumental noise and the
  stellar variability were treated with several detrending tools, on
  which subsequently several transit search algorithms were applied. <BR
  />Results: Forty two sources were classified as planetary transit
  candidates and up to now 26 cases have been solved. One planet
  (CoRoT-2b) and one brown-dwarf (CoRoT-3b) have been the subjects
  of detailed publications. <P />The CoRoT space mission, launched
  on December 27 2006, was developed and is operated by CNES, with
  contributions from Austria, Belgium, Brazil, ESA, Germany and Spain. The
  first CoRoT data are available to the community from the CoRoT archive:
  http://idoc-corot.ias.u-psud.fr.

Title: Planetary transit candidates in the CoRoT initial run:
    resolving their nature
Authors: Moutou, C.; Pont, F.; Bouchy, F.; Deleuil, M.; Almenara,
   J. M.; Alonso, R.; Barbieri, M.; Bruntt, H.; Deeg, H. J.; Fridlund,
   M.; Gandolfi, D.; Gillon, M.; Guenther, E.; Hatzes, A.; Hébrard, G.;
   Loeillet, B.; Mayor, M.; Mazeh, T.; Queloz, D.; Rabus, M.; Rouan, D.;
   Shporer, A.; Udry, S.; Aigrain, S.; Auvergne, M.; Baglin, A.; Barge,
   P.; Benz, W.; Bordé, P.; Carpano, S.; de La Reza, R.; Dvorak, R.;
   Erikson, A.; Gondoin, P.; Guillot, T.; Jorda, L.; Kabath, P.; Lammer,
   H.; Léger, A.; Llebaria, A.; Lovis, C.; Magain, P.; Ollivier, M.;
   Pätzold, M.; Pepe, F.; Rauer, H.; Schneider, J.; Wuchterl, G.
Bibcode: 2009A&A...506..321M
Altcode:
  With the release of CoRoT lightcurves of the Initial Run IRa01, 50
  transiting planetary candidates have been published in a companion
  paper. About twenty of them were identified as binary stars from
  the CoRoT lightcurve itself. Complementary observations were
  conducted for 29 candidates, including ground-based photometry and
  radial-velocity measurements. Two giant planets were identified and
  fully characterized. Nineteen binaries are recognized, from which 10
  are background eclipsing binaries in the CoRoT mask or triple systems,
  diluted by the main CoRoT target. Eight cases remain of unclear
  origin, one of them still being a planetary candidate. Comparison
  with simulations shows that the actual threshold of confirmed planet
  detection in this field does not yet fulfill the expectations, and
  a number of reasons are invoked, like the ranking process based
  on lightcurve analyses, and the strategy and limits of follow-up
  observations for targets fainter than magnitude 15. <P />Based on data
  obtained at Observatoire de Haute Provence with SOPHIE and with HARPS
  on the ESO 3.6 m telescope at La Silla Observatory. The CoRoT space
  mission, launched on December 27th 2006, has been developed and is
  operated by CNES, with the contribution of Austria, Belgium, Brazil ,
  ESA (RSSD and Science Programme), Germany and Spain. <P />Tables 2 to
  13, 15 to 17 and Figs. 4 to 7 are only available in electronic form
  at http://www.aanda.org

Title: Planetary transit candidates in Corot-IRa01 field
Authors: Carpano, S.; Cabrera, J.; Alonso, R.; Barge, P.; Aigrain, S.;
   Almenara, J. -M.; Bordé, P.; Bouchy, F.; Carone, L.; Deeg, H. J.;
   de La Reza, R.; Deleuil, M.; Dvorak, R.; Erikson, A.; Fressin,
   F.; Fridlund, M.; Gondoin, P.; Guillot, T.; Hatzes, A.; Jorda,
   L.; Lammer, H.; Léger, A.; Llebaria, A.; Magain, P.; Moutou, C.;
   Ofir, A.; Ollivier, M.; Janot-Pacheco, E.; Pätzold, M.; Pont, F.;
   Queloz, D.; Rauer, H.; Régulo, C.; Renner, S.; Rouan, D.; Samuel,
   B.; Schneider, J.; Wuchterl, G.
Bibcode: 2009A&A...506..491C
Altcode: 2009arXiv0907.5150C
  Context: CoRoT is a pioneering space mission devoted to the analysis
  of stellar variability and the photometric detection of extrasolar
  planets. <BR />Aims: We present the list of planetary transit candidates
  detected in the first field observed by CoRoT, IRa01, the initial
  run toward the Galactic anticenter, which lasted for 60 days. <BR
  />Methods: We analysed 3898 sources in the coloured bands and 5974
  in the monochromatic band. Instrumental noise and stellar variability
  were taken into account using detrending tools before applying various
  transit search algorithms. <BR />Results: Fifty sources were classified
  as planetary transit candidates and the most reliable 40 detections
  were declared targets for follow-up ground-based observations. Two
  of these targets have so far been confirmed as planets, CoRoT-1b and
  CoRoT-4b, for which a complete characterization and specific studies
  were performed. <P />The CoRoT space mission, launched on December
  27th 2006, <P />has been developed and is operated by CNES, with
  contributions from Austria, Belgium, Brazil, ESA, <P />Germany, and
  Spain. Four <P />French laboratories associated with the CNRS (LESIA,
  LAM, IAS ,OMP) collaborate with CNES on the satellite development. <P
  />First CoRoT data are available to the public from the CoRoT archive:
  http://idoc-corot.ias.u-psud.fr.

Title: Removing systematics from the CoRoT light
    curves. I. Magnitude-dependent zero point
Authors: Mazeh, T.; Guterman, P.; Aigrain, S.; Zucker, S.; Grinberg,
   N.; Alapini, A.; Alonso, R.; Auvergne, M.; Barbieri, M.; Barge,
   P.; Bordé, P.; Bouchy, F.; Deeg, H.; de La Reza, R.; Deleuil, M.;
   Dvorak, R.; Erikson, A.; Fridlund, M.; Gondoin, P.; Jorda, L.; Lammer,
   H.; Léger, A.; Llebaria, A.; Magain, P.; Moutou, C.; Ollivier, M.;
   Pätzold, M.; Pont, F.; Queloz, D.; Rauer, H.; Rouan, D.; Sabo, R.;
   Schneider, J.; Wuchterl, G.
Bibcode: 2009A&A...506..431M
Altcode: 2009arXiv0907.2237M
  This paper presents an analysis that searched for systematic effects
  within the CoRoT exoplanet field light curves. The analysis identified
  a systematic effect that modified the zero point of most CoRoT exposures
  as a function of stellar magnitude. We could find this effect only after
  preparing a set of learning light curves that were relatively free of
  stellar and instrumental noise. Correcting for this effect, rejecting
  outliers that appear in almost every exposure, and applying SysRem,
  reduced the stellar RMS by about 20%, without attenuating transit
  signals. <P />The CoRoT space mission, launched on December 27th 2006,
  has been developed and is operated by CNES, with the contribution of
  Austria, Belgium, Brazil, ESA, Germany, and Spain. CoRoT data become
  publicly available one year after release to the Co-Is of the mission
  from the CoRoT archive: http://idoc-corot.ias.u-psud.fr/.

Title: Rate and nature of false positives in the CoRoT exoplanet
    search
Authors: Almenara, J. M.; Deeg, H. J.; Aigrain, S.; Alonso, R.;
   Auvergne, M.; Baglin, A.; Barbieri, M.; Barge, P.; Bordé, P.; Bouchy,
   F.; Bruntt, H.; Cabrera, J.; Carone, L.; Carpano, S.; Catala, C.;
   Csizmadia, Sz.; de La Reza, R.; Deleuil, M.; Dvorak, R.; Erikson, A.;
   Fridlund, M.; Gandolfi, D.; Gillon, M.; Gondoin, P.; Guenther, E.;
   Guillot, T.; Hatzes, A.; Hébrard, G.; Jorda, L.; Lammer, H.; Léger,
   A.; Llebaria, A.; Loeillet, B.; Magain, P.; Mayor, M.; Mazeh, T.;
   Moutou, C.; Ollivier, M.; Pätzold, M.; Pont, F.; Queloz, D.; Rauer,
   H.; Régulo, C.; Renner, S.; Rouan, D.; Samuel, B.; Schneider, J.;
   Shporer, A.; Wuchterl, G.; Zucker, S.
Bibcode: 2009A&A...506..337A
Altcode: 2009arXiv0908.1172A
  Context: The CoRoT satellite searches for planets by applying the
  transit method, monitoring up to 12 000 stars in the galactic plane
  for 150 days in each observing run. This search is contaminated by
  a large fraction of false positives, caused by different eclipsing
  binary configurations that might be confused with a transiting
  planet. <BR />Aims: We evaluate the rates and nature of false
  positives in the CoRoT exoplanets search and compare our results with
  semiempirical predictions. <BR />Methods: We consider the detected
  binary and planet candidates in the first three extended CoRoT runs,
  and classify the results of the follow-up observations completed to
  verify their planetary nature. We group the follow-up results into
  undiluted binaries, diluted binaries, and planets and compare their
  abundances with predictions from the literature. <BR />Results: 83%
  of the initial detections are classified as false positives using
  only the CoRoT light-curves, the remaining 17% require follow-up
  observations. Finally, 12% of the candidates in the follow-up program
  are planets. The shape of the overall distribution of the false positive
  rate follows previous predictions, except for candidates with transit
  depths below about 0.4%. For candidates with transit depths in the
  range from 0.1-0.4%, CoRoT detections are nearly complete, and this
  difference from predictions is probably real and dominated by a lower
  than expected abundance of diluted eclipsing binaries. <P />The CoRoT
  space mission, launched on December 27th 2006, has been developed
  and is operated by CNES, with the contribution of Austria, Belgium,
  Brazil , ESA (RSSD and Science Programme), Germany and Spain.

Title: Noise properties of the CoRoT data. A planet-finding
    perspective
Authors: Aigrain, S.; Pont, F.; Fressin, F.; Alapini, A.; Alonso,
   R.; Auvergne, M.; Barbieri, M.; Barge, P.; Bordé, P.; Bouchy,
   F.; Deeg, H.; de La Reza, R.; Deleuil, M.; Dvorak, R.; Erikson,
   A.; Fridlund, M.; Gondoin, P.; Guterman, P.; Jorda, L.; Lammer, H.;
   Léger, A.; Llebaria, A.; Magain, P.; Mazeh, T.; Moutou, C.; Ollivier,
   M.; Pätzold, M.; Queloz, D.; Rauer, H.; Rouan, D.; Schneider, J.;
   Wuchter, G.; Zucker, S.
Bibcode: 2009A&A...506..425A
Altcode: 2009arXiv0903.1829A
  In this short paper, we study the photometric precision of stellar
  light curves obtained by the CoRoT satellite in its planet-finding
  channel, with a particular emphasis on the time scales characteristic
  of planetary transits. Together with other articles in the same issue
  of this journal, it forms an attempt to provide the building blocks
  for a statistical interpretation of the CoRoT planet and eclipsing
  binary catch to date. After pre-processing the light curves so as to
  minimise long-term variations and outliers, we measure the scatter
  of the light curves in the first three CoRoT runs lasting more than
  1 month, using an iterative non-linear filter to isolate signal on
  the time scales of interest. The behaviour of the noise on 2 h time
  scales is described well by a power-law with index 0.25 in R-magnitude,
  ranging from 0.1 mmag at R=11.5 to 1 mmag at R=16, which is close
  to the pre-launch specification, though still a factor 2-3 above the
  photon noise due to residual jitter noise and hot pixel events. There
  is evidence of slight degradation in the performance over time. We
  find clear evidence of enhanced variability on hour time scales (at
  the level of 0.5 mmag) in stars identified as likely giants from their
  R magnitude and B-V colour, which represent approximately 60 and 20%
  of the observed population in the directions of Aquila and Monoceros,
  respectively. On the other hand, median correlated noise levels over 2
  h for dwarf stars are extremely low, reaching 0.05 mmag at the bright
  end. <P />The CoRoT space mission, launched on December 27, 2006, has
  been developed and is operated by the CNES, with the contribution of
  Austria, Belgium, Brazil, ESA, Germany, and Spain. CoRoT data become
  publicly available one year after release to the Co-Is of the mission
  from the CoRoT archive: http://idoc-corot.ias.u-psud.fr/.

Title: The secondary eclipse of CoRoT-1b
Authors: Alonso, R.; Alapini, A.; Aigrain, S.; Auvergne, M.; Baglin,
   A.; Barbieri, M.; Barge, P.; Bonomo, A. S.; Bordé, P.; Bouchy, F.;
   Chaintreuil, S.; de La Reza, R.; Deeg, H. J.; Deleuil, M.; Dvorak,
   R.; Erikson, A.; Fridlund, M.; de Oliveira Fialho, F.; Gondoin, P.;
   Guillot, T.; Hatzes, A.; Jorda, L.; Lammer, H.; Léger, A.; Llebaria,
   A.; Magain, P.; Mazeh, T.; Moutou, C.; Ollivier, M.; Pätzold, M.;
   Pont, F.; Queloz, D.; Rauer, H.; Rouan, D.; Schneider, J.; Wuchterl, G.
Bibcode: 2009A&A...506..353A
Altcode: 2009arXiv0907.1653A
  The transiting planet CoRoT-1b is thought to belong to the pM-class
  of planets, in which the thermal emission dominates in the optical
  wavelengths. We present a detection of its secondary eclipse in
  the CoRoT white channel data, whose response function goes from
  ~400 to ~1000 nm. We used two different filtering approaches, and
  several methods to evaluate the significance of a detection of the
  secondary eclipse. We detect a secondary eclipse centered within 20
  min at the expected times for a circular orbit, with a depth of 0.016
  ± 0.006%. The center of the eclipse is translated in a 1-σ upper
  limit to the planet's eccentricity of e cosω&lt; 0.014. Under the
  assumption of a zero Bond Albedo and blackbody emission from the planet,
  it corresponds to a T_CoRoT = 2330<SUP>+120</SUP><SUB>-140</SUB> K. We
  provide the equilibrium temperatures of the planet as a function of
  the amount of reflected light. If the planet is in thermal equilibrium
  with the incident flux from the star, our results imply an inefficient
  transport mechanism of the flux from the day to the night sides. <P
  />Based on observations obtained with CoRoT, a space project operated
  by the French Space Agency, CNES, with participation of the Science
  Programme of ESA, ESTEC/RSSD, Austria, Belgium, Brazil, Germany
  and Spain.

Title: VizieR Online Data Catalog: CoRoT-7 radial velocities
    (Queloz+, 2009)
Authors: Queloz, D.; Bouchy, F.; Moutou, C.; Hatzes, A.; Hebrard, G.;
   Alonso, R.; Auvergne, M.; Baglin, A.; Barbieri, M.; Barge, P.; Benz,
   W.; Borde, P.; Deeg, H. J.; Deleuil, M.; Dvorak, R.; Erikson, A.;
   Ferraz Mello, S.; Fridlund, M.; Gandolfi, D.; Gillon, M.; Guenther,
   E.; Guillot, T.; Jorda, L.; Hartmann, M.; Lammer, H.; Leger, A.;
   Llebaria, A.; Lovis, C.; Magain, P.; Mayor, M.; Mazeh, T.; Ollivier,
   M.; Patzold, M.; Pepe, F.; Rauer, H.; Rouan, D.; Schneider, J.;
   Segransan, D.; Udry, S.; Wuchterl, G.
Bibcode: 2009yCat..35060303Q
Altcode:
  First, a simple pre-whitening procedure was employed to find and
  subsequently remove periodic signals from the complex frequency
  structure of the radial velocity data. The dominant frequency in the
  power spectrum was found at 23 days, which corresponds to the rotation
  period of CoRoT-7. The 0.8535 day period of CoRoT-7b planetary candidate
  was detected with an amplitude of 3.3m/s. <P />(1 data file).

Title: The CoRoT-7 planetary system: two orbiting super-Earths
Authors: Queloz, D.; Bouchy, F.; Moutou, C.; Hatzes, A.; Hébrard, G.;
   Alonso, R.; Auvergne, M.; Baglin, A.; Barbieri, M.; Barge, P.; Benz,
   W.; Bordé, P.; Deeg, H. J.; Deleuil, M.; Dvorak, R.; Erikson, A.;
   Ferraz Mello, S.; Fridlund, M.; Gandolfi, D.; Gillon, M.; Guenther,
   E.; Guillot, T.; Jorda, L.; Hartmann, M.; Lammer, H.; Léger, A.;
   Llebaria, A.; Lovis, C.; Magain, P.; Mayor, M.; Mazeh, T.; Ollivier,
   M.; Pätzold, M.; Pepe, F.; Rauer, H.; Rouan, D.; Schneider, J.;
   Segransan, D.; Udry, S.; Wuchterl, G.
Bibcode: 2009A&A...506..303Q
Altcode:
  We report on an intensive observational campaign carried out with HARPS
  at the 3.6 m telescope at La Silla on the star CoRoT-7. Additional
  simultaneous photometric measurements carried out with the Euler
  Swiss telescope have demonstrated that the observed radial velocity
  variations are dominated by rotational modulation from cool spots
  on the stellar surface. Several approaches were used to extract the
  radial velocity signal of the planet(s) from the stellar activity
  signal. First, a simple pre-whitening procedure was employed to find
  and subsequently remove periodic signals from the complex frequency
  structure of the radial velocity data. The dominant frequency in the
  power spectrum was found at 23 days, which corresponds to the rotation
  period of CoRoT-7. The 0.8535 day period of CoRoT-7b planetary candidate
  was detected with an amplitude of 3.3 m s<SUP>-1</SUP>. Most other
  frequencies, some with amplitudes larger than the CoRoT-7b signal,
  are most likely associated with activity. A second approach used
  harmonic decomposition of the rotational period and up to the first
  three harmonics to filter out the activity signal from radial velocity
  variations caused by orbiting planets. After correcting the radial
  velocity data for activity, two periodic signals are detected: the
  CoRoT-7b transit period and a second one with a period of 3.69 days
  and an amplitude of 4 m s<SUP>-1</SUP>. This second signal was also
  found in the pre-whitening analysis. We attribute the second signal
  to a second, more remote planet CoRoT-7c . The orbital solution of
  both planets is compatible with circular orbits. The mass of CoRoT-7b
  is 4.8±0.8 (M<SUB>⊕</SUB>) and that of CoRoT-7c is 8.4± 0.9
  (M<SUB>⊕</SUB>), assuming both planets are on coplanar orbits. We
  also investigated the false positive scenario of a blend by a faint
  stellar binary, and this may be rejected by the stability of the
  bisector on a nightly scale. According to their masses both planets
  belong to the super-Earth planet category. The average density of
  CoRoT-7b is ρ=5.6± 1.3 g cm<SUP>-3</SUP>, similar to the Earth. The
  CoRoT-7 planetary system provides us with the first insight into
  the physical nature of short period super-Earth planets recently
  detected by radial velocity surveys. These planets may be denser than
  Neptune and therefore likely made of rocks like the Earth, or a mix
  of water ice and rocks. <P />Based on observations made with HARPS
  spectrograph on the 3.6-m ESO telescope and the EULER Swiss telescope at
  La Silla Observatory, Chile. The HARPS results presented in this paper
  (Appendix A) are available in electronic form at http://www.aanda.org
  and at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
  or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/506/303

Title: A Multi-Wavelength Simultaneous Study of the Composition of
    the Halley Family Comet 8P/Tuttle
Authors: Jehin, E.; Bockelée-Morvan, D.; Dello Russo, N.; Manfroid,
   J.; Hutsemékers, D.; Kawakita, H.; Kobayashi, H.; Schulz, R.;
   Smette, A.; Stüwe, J.; Weiler, M.; Arpigny, C.; Biver, N.; Cochran,
   A.; Crovisier, J.; Magain, P.; Rauer, H.; Sana, H.; Vervack, R. J.;
   Weaver, H.; Zucconi, J. -M.
Bibcode: 2009EM&P..105..343J
Altcode: 2009EM&P..tmp...38J
  We report on simultaneous optical and infrared observations
  of the Halley Family comet 8P/Tuttle performed with the ESO
  Very Large Telescope. Such multi-wavelength and coordinated
  observations are a good example of what can be done to support
  space missions. From high resolution optical spectroscopy of the CN
  (0,0) 388 nm and NH<SUB>2</SUB> (0,9,0) 610 nm bands using UVES
  at UT2 we determined <SUP>12</SUP>C/<SUP>13</SUP>C = 90 ± 10 and
  <SUP>14</SUP>N/<SUP>15</SUP>N = 150 ± 20 in CN and we derived
  a nuclear spin temperature of NH<SUB>3</SUB> of 29 ± 1 K. These
  values are similar to those found in Oort-Cloud and Jupiter Family
  comets. From low resolution long slit spectroscopy with FORS1 at UT2
  we determined the CN, C<SUB>3</SUB> and C<SUB>2</SUB> production rates
  and the parent and daughter scale lengths up to 5.2 10<SUP>5</SUP>
  km tailward. From high resolution IR spectroscopy with CRIRES at UT1
  we measured simultaneously the production rates and mixing ratios
  of H<SUB>2</SUB>O, HCN, C<SUB>2</SUB>H<SUB>2</SUB>, CH<SUB>4</SUB>,
  C<SUB>2</SUB>H<SUB>6</SUB>, and CH<SUB>3</SUB>OH.

Title: Near-infrared observations of the HE0450-2958 system: discovery
    of a second active galactic nucleus?
Authors: Letawe, G.; Magain, P.; Chantry, V.; Letawe, Y.
Bibcode: 2009MNRAS.396...78L
Altcode: 2009arXiv0903.1718L
  The quasi-stellar object (QSO) HE0450-2958 was brought to the front
  scene by the non-detection of its host galaxy and strong upper limits on
  the latter's luminosity. The QSO is also a powerful infrared emitter,
  in gravitational interaction with a strongly distorted ultraluminous
  infrared companion galaxy. We investigate the properties of the
  companion galaxy, through new near- and mid-infrared observations of the
  system obtained with Near Infrared Camera and Multi-Object Spectrometer
  (NICMOS) onboard Hubble Space Telescope, Infrared Spectrometer and
  Array Camera (ISAAC) and Very Large Telescope Imager and Spectrometer
  in the Infrared (VISIR) on the European Southern Observatory Very Large
  Telescope. The companion galaxy is found to harbour a point source
  revealed only in the infrared, in what appears as a hole or dark patch
  in the optical images. Various hypotheses on the nature of this point
  source are analysed and it is found that the only plausible one is
  that it is a strongly reddened active galactic nucleus hidden behind
  a thick dust cloud. The hypothesis that the QSO supermassive black
  hole might have been ejected from the companion galaxy in the course
  of a galactic collision involving three-body black holes interaction
  is also reviewed, on the basis of this new insight on a definitely
  complex system. <P />Based on observations made with the ESO Very
  Large Telescope at ESO Paranal Observatory, Chile, under program IDs
  076.B-0693(C), 276.B-5011 and NASA/ESA HST program 10797 during cycle
  15. <P />E-mail: gletawe@ulg.ac.be

Title: VizieR Online Data Catalog: FORS2 and HAWKI photometry of
    CoRoT-1 (Gillon+, 2009)
Authors: Gillon, M.; Demory, B. -O.; Triaud, A. H. M. J.; Barman,
   T.; Hebb, L.; Montalban, J.; Maxted, P. F. L.; Queloz, D.; Deleuil,
   M.; Magain, P.
Bibcode: 2009yCat..35060359G
Altcode:
  We present VLT eclipse photometry for the giant planet CoRoT-1b. We
  observed a transit in the R-band filter and an occultation in
  a narrow filter centered on 2.09{mu}m. Our analysis of this new
  photometry and published radial velocities, in combination with
  stellar-evolutionary modeling, leads to a planetary mass and
  radius of 1.07<SUP>+0.13</SUP><SUB>-0.18</SUB>M<SUB>{Jup}</SUB>
  and 1.45<SUP>+0.07</SUP><SUB>-0.13</SUB>R_{Jup}, confirming the
  very low density previously deduced from CoRoT photometry. The
  large occultation depth that we measure at 2.09{mu}m
  (0.278<SUP>0.043</SUP><SUB>-0.066</SUB>% ) is consistent with thermal
  emission and is better reproduced by an atmospheric model with no
  redistribution of the absorbed stellar flux to the night side of the
  planet. <P />(2 data files).

Title: Transiting exoplanets from the CoRoT space
mission. IV. CoRoT-Exo-4b: a transiting planet in a 9.2 day
    synchronous orbit
Authors: Aigrain, S.; Collier Cameron, A.; Ollivier, M.; Pont, F.;
   Jorda, L.; Almenara, J. M.; Alonso, R.; Barge, P.; Bordé, P.; Bouchy,
   F.; Deeg, H.; de La Reza, R.; Deleuil, M.; Dvorak, R.; Erikson, A.;
   Fridlund, M.; Gondoin, P.; Gillon, M.; Guillot, T.; Hatzes, A.; Lammer,
   H.; Lanza, A. F.; Léger, A.; Llebaria, A.; Magain, P.; Mazeh, T.;
   Moutou, C.; Paetzold, M.; Pinte, C.; Queloz, D.; Rauer, H.; Rouan,
   D.; Schneider, J.; Wuchter, G.; Zucker, S.
Bibcode: 2008A&A...488L..43A
Altcode: 2008arXiv0807.3767A
  CoRoT, the first space-based transit search, provides
  ultra-high-precision light curves with continuous time-sampling over
  periods of up to 5 months. This allows the detection of transiting
  planets with relatively long periods, and the simultaneous study of
  the host star's photometric variability. In this Letter, we report the
  discovery of the transiting giant planet CoRoT-Exo-4b and use the CoRoT
  light curve to perform a detailed analysis of the transit and determine
  the stellar rotation period. The CoRoT light curve was pre-processed
  to remove outliers and correct for orbital residuals and artefacts
  due to hot pixels on the detector. After removing stellar variability
  about each transit, the transit light curve was analysed to determine
  the transit parameters. A discrete autocorrelation function method was
  used to derive the rotation period of the star from the out-of-transit
  light curve. We determine the periods of the planetary orbit and star's
  rotation of 9.20205 ± 0.00037 and 8.87 ± 1.12 days respectively,
  which is consistent with this being a synchronised system. We also
  derive the inclination, i = 90.00_-0.085<SUP>+0.000</SUP> in degrees,
  the ratio of the orbital distance to the stellar radius, a/R<SUB>s</SUB>
  = 17.36<SUB>-0.25</SUB><SUP>+0.05</SUP>, and the planet-to-star radius
  ratio R_p/R_s=0.1047<SUB>-0.0022</SUB><SUP>+0.0041</SUP>. We discuss
  briefly the coincidence between the orbital period of the planet and the
  stellar rotation period and its possible implications for the system's
  migration and star-planet interaction history. <P />The CoRoT space
  mission, launched on <P />December 27th 2006, has been developed and
  is operated by <P />CNES, with the contribution of Austria, Belgium,
  Brazil, ESA, <P />Germany, and Spain. The first CoRoT data will be
  available to the <P />public in February 2009 from the CoRoT archive:
  http://idoc-corot.ias.u-psud.fr/ <P />Figures 1, 4 and 5 are only
  available in electronic form at http://www.aanda.org

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses. VII. Time delays and the Hubble constant from WFI J2033-4723
Authors: Vuissoz, C.; Courbin, F.; Sluse, D.; Meylan, G.; Chantry,
   V.; Eulaers, E.; Morgan, C.; Eyler, M. E.; Kochanek, C. S.; Coles,
   J.; Saha, P.; Magain, P.; Falco, E. E.
Bibcode: 2008A&A...488..481V
Altcode: 2008arXiv0803.4015V
  Gravitationally lensed quasars can be used to map the mass distribution
  in lensing galaxies and to estimate the Hubble constant H<SUB>0</SUB>
  by measuring the time delays between the quasar images. Here we report
  the measurement of two independent time delays in the quadruply imaged
  quasar WFI J2033-4723 (z = 1.66). Our data consist of R-band images
  obtained with the Swiss 1.2 m EULER telescope located at La Silla and
  with the 1.3 m SMARTS telescope located at Cerro Tololo. The light
  curves have 218 independent epochs spanning 3 full years of monitoring
  between March 2004 and May 2007, with a mean temporal sampling of one
  observation every 4th day. We measure the time delays using three
  different techniques, and we obtain Δ t<SUB>B-A</SUB> = 35.5 ±
  1.4 days (3.8%) and Δ t<SUB>B-C</SUB> = 62.6<SUP>+ 4.1</SUP><SUB>-
  2.3</SUB>~days ~ (<SUP>+ 6.5%</SUP><SUB>- 3.7%</SUB>), where A is a
  composite of the close, merging image pair. After correcting for the
  time delays, we find R-band flux ratios of F<SUB>A</SUB>/F<SUB>B</SUB>
  = 2.88 ± 0.04, F<SUB>A</SUB>/F<SUB>C</SUB> = 3.38 ± 0.06, and
  F<SUB>A1</SUB>/F<SUB>A2</SUB> = 1.37 ± 0.05 with no evidence for
  microlensing variability over a time scale of three years. However,
  these flux ratios do not agree with those measured in the quasar
  emission lines, suggesting that longer term microlensing is present. Our
  estimate of H<SUB>0</SUB> agrees with the concordance value:
  non-parametric modeling of the lensing galaxy predicts H<SUB>0</SUB>
  = 67<SUP>+13</SUP><SUB>-10</SUB> km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>,
  while the Single Isothermal Sphere model yields H<SUB>0</SUB> =
  63<SUP>+7</SUP><SUB>-3</SUB> km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>
  (68% confidence level). More complex lens models using a composite
  de Vaucouleurs plus NFW galaxy mass profile show twisting of the mass
  isocontours in the lensing galaxy, as do the non-parametric models. As
  all models also require a significant external shear, this suggests that
  the lens is a member of the group of galaxies seen in field of view
  of WFI J2033-4723. <P />Based on observations obtained with the 1.2 m
  EULER Swiss Telescope, the 1.3 m Small and Moderate Aperture Research
  Telescope System (SMARTS) which is operated by the SMARTS Consortium,
  and the NASA/ESA Hubble Space Telescope as part of program HST-GO-9744
  of the Space Telescope Science Institute, which is operated by the
  Association of Universities for Research in Astronomy, Inc., under
  NASA contract NAS 5-26555. Table 4 is only available in electronic
  form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
  or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/488/481

Title: Transiting exoplanets from the CoRoT space
mission. V. CoRoT-Exo-4b: stellar and planetary parameters
Authors: Moutou, C.; Bruntt, H.; Guillot, T.; Shporer, A.; Guenther,
   E.; Aigrain, S.; Almenara, J. M.; Alonso, R.; Auvergne, M.; Baglin, A.;
   Barbieri, M.; Barge, P.; Benz, W.; Bordé, P.; Bouchy, F.; Deeg, H. J.;
   de La Reza, R.; Deleuil, M.; Dvorak, R.; Erikson, A.; Fridlund, M.;
   Gillon, M.; Gondoin, P.; Hatzes, A.; Hébrard, G.; Jorda, L.; Kabath,
   P.; Lammer, H.; Léger, A.; Llebaria, A.; Loeillet, B.; Magain, P.;
   Mayor, M.; Mazeh, T.; Ollivier, M.; Pätzold, M.; Pepe, F.; Pont,
   F.; Queloz, D.; Rabus, M.; Rauer, H.; Rouan, D.; Schneider, J.; Udry,
   S.; Wuchterl, G.
Bibcode: 2008A&A...488L..47M
Altcode: 2008arXiv0807.3739M
  Aims: The CoRoT satellite has announced its fourth transiting planet
  (Aigrain et al. 2008, A&amp;A, 488, L43) with space photometry. We
  describe and analyse complementary observations of this system
  performed to establish the planetary nature of the transiting
  body and to estimate the fundamental parameters of the planet and
  its parent star. <BR />Methods: We have analysed high precision
  radial-velocity data, ground-based photometry, and high signal-to-noise
  ratio spectroscopy. <BR />Results: The parent star CoRoT-Exo-4 (2MASS
  06484671-0040219) is a late F-type star of mass of 1.16 M<SUB>⊙</SUB>
  and radius of 1.17 R<SUB>⊙</SUB>. The planet has a circular orbit with
  a period of 9.20205 d. The planet radius is 1.19 R_Jup and the mass
  is 0.72 M_Jup. It is a gas-giant planet with a “normal” internal
  structure of mainly H and He. CoRoT-Exo-4b has the second longest period
  of the known transiting planets. It is an important discovery since
  it occupies an empty area in the mass-period diagram of transiting
  exoplanets. <P />Based on observations obtained with CoRoT, a space
  project operated by the French Space Agency, CNES, with participation
  of the Science Programme of ESA, ESTEC/RSSD, Austria, Belgium, Brazil,
  Germany and Spain; and on observations made with the SOPHIE spectrograph
  at Observatoire de Haute Provence, France (PNP.07B.MOUT), and the HARPS
  spectrograph at ESO La Silla Observatory (079.C-0127/F). <P />Table 2
  and Fig. 5 are only available in electronic form at http://www.aanda.org

Title: High-dispersion Spectroscopic Observations Of 8P/Tuttle
    With VLT/CRIRES
Authors: Kobayashi, Hitomi; Bockelee-Morvan, D.; Dello Russo, N.;
   Kawakita, H.; Verback, R. J.; Weaver, H.; Jehin, E.; Manfroid, J.;
   Smette, A.; Cochran, A.; Hutsemekers, D.; Schulz, R.; Stuwe, J.;
   Weiler, M.; Zucconi, J.; Arpigny, C.; Biver, N.; Crovisier, J.;
   Magain, P.; Rauer, H.; Sana, H.
Bibcode: 2008DPS....40.0504K
Altcode: 2008BAAS...40..394K
  We present near-infrared observations of organic molecules in comet
  8P/Tuttle. <P />Comet 8P/Tuttle is a Halley-type comet and its last
  perihelion was in early January 2008. Our observations were carried out
  on January 28 and February 4 using CRIRES (CRyogenic high-resolution
  InfraRed Echelle Spectrograph) at the Very Large Telescope (VLT). We
  used a 0.2" slit which provided a spectral resolving power of 80,000. We
  detected H<SUB>2</SUB>O, OH, HCN, C<SUB>2</SUB>H<SUB>2</SUB> on Jan 28,
  and H<SUB>2</SUB>O, OH, CH<SUB>4</SUB>, C<SUB>2</SUB>H<SUB>6</SUB>, and
  CH<SUB>3</SUB>OH on Feb 4. <P />We find that 8P/Tuttle is depleted in
  HCN, C<SUB>2</SUB>H<SUB>2</SUB> and C<SUB>2</SUB>H<SUB>6</SUB> relative
  to H<SUB>2</SUB>O compared with most other Oort cloud comets studied
  to date. Perhaps these depletions suggest that 8P/Tuttle formed in a
  different region from most Oort cloud comets, but it is also possible
  that the depletions are caused by repeated passages through the inner
  solar system.

Title: VizieR Online Data Catalog: Time delays and H0 from WFI
    J2033-4723 (Vuissoz+, 2008)
Authors: Vuissoz, C.; Courbin, F.; Sluse, D.; Meylan, G.; Chantry,
   V.; Eulaers, E.; Morgan, C.; Eyler, M. E.; Kochanek, C. S.; Coles,
   J.; Saha, P.; Magain, P.; Falco, E. E.
Bibcode: 2008yCat..34880481V
Altcode:
  Photometry of WFI J2033-4723, as in Fig. 3 of the paper. The first
  column gives the Julian date and corresponds to HJD days. The second
  column is the seeing, in arcsec. Column 3-8 display the photometric
  measurements of the quasar components A, B and C respectively, with
  the corresponding error bars. The last column finally provides the
  name of the telescope used for each measurement. <P />(1 data file).

Title: Understanding the Relations between QSOs and Their Host
    Galaxies from Combined HST Imaging and VLT Spectroscopy
Authors: Letawe, Y.; Magain, P.; Letawe, G.; Courbin, F.; Hutsemékers,
   D.
Bibcode: 2008ApJ...679..967L
Altcode: 2008arXiv0802.1386L
  The host galaxies of six nearby QSOs are studied on the basis of
  high-resolution HST optical images and spatially resolved VLT slit
  spectra. The gas ionization and velocity are mapped as a function
  of the distance to the central QSO. In the majority of the cases,
  the QSO significantly contributes to the gas ionization in its whole
  host galaxy, and sometimes even outside. Reflection or scattering
  of the QSO Hα line from remote regions of the galaxy is detected
  in several instances. The line shifts show that, in all cases,
  the matter responsible for the light reflection moves away from the
  QSO, likely accelerated by its radiation pressure. The two faintest
  QSOs reside in spirals, with some signs of a past gravitational
  perturbation. One of the intermediate-luminosity QSOs resides in
  a massive elliptical containing gas ionized (and probably pushed
  away) by the QSO radiation. The other medium-power object is found
  in a spiral galaxy displaying complex velocity structure, with the
  central QSO moving with respect to the bulge, probably as a result of
  a galactic collision. The two most powerful objects are involved in
  violent gravitational interactions, and one of them has no detected
  host. These results suggest that (1) large-scale phenomena, such as
  galactic collisions, are closely related to the triggering and the
  feeding of the QSO and (2) once ignited, the QSO has significant
  influence on its large-scale neighborhood (often the whole host and
  sometimes further away). <P />Based on observations made with the
  Nasa/ESA Hubble Space Telescope (Cycle 13 proposal 10238), and with
  ANTU/UT1 at ESO-Paranal observatory in Chile [programs 65.P-0361(A)
  and 66.B-0139(A)].

Title: Transiting exoplanets from the CoRoT space
mission. II. CoRoT-Exo-2b: a transiting planet around an active G star
Authors: Alonso, R.; Auvergne, M.; Baglin, A.; Ollivier, M.; Moutou,
   C.; Rouan, D.; Deeg, H. J.; Aigrain, S.; Almenara, J. M.; Barbieri, M.;
   Barge, P.; Benz, W.; Bordé, P.; Bouchy, F.; de La Reza, R.; Deleuil,
   M.; Dvorak, R.; Erikson, A.; Fridlund, M.; Gillon, M.; Gondoin, P.;
   Guillot, T.; Hatzes, A.; Hébrard, G.; Kabath, P.; Jorda, L.; Lammer,
   H.; Léger, A.; Llebaria, A.; Loeillet, B.; Magain, P.; Mayor, M.;
   Mazeh, T.; Pätzold, M.; Pepe, F.; Pont, F.; Queloz, D.; Rauer, H.;
   Shporer, A.; Schneider, J.; Stecklum, B.; Udry, S.; Wuchterl, G.
Bibcode: 2008A&A...482L..21A
Altcode: 2008arXiv0803.3207A
  Context: The CoRoT mission, a pioneer in exoplanet searches from
  space, has completed its first 150 days of continuous observations
  of ~12 000 stars in the galactic plane. An analysis of the raw data
  identifies the most promising candidates and triggers the ground-based
  follow-up. <BR />Aims: We report on the discovery of the transiting
  planet CoRoT-Exo-2b, with a period of 1.743 days, and characterize its
  main parameters. <BR />Methods: We filter the CoRoT raw light curve
  of cosmic impacts, orbital residuals, and low frequency signals from
  the star. The folded light curve of 78 transits is fitted to a model
  to obtain the main parameters. Radial velocity data obtained with the
  SOPHIE, CORALIE and HARPS spectrographs are combined to characterize
  the system. The 2.5 min binned phase-folded light curve is affected by
  the effect of sucessive occultations of stellar active regions by the
  planet, and the dispersion in the out of transit part reaches a level
  of 1.09×10<SUP>-4</SUP> in flux units. <BR />Results: We derive a
  radius for the planet of 1.465 ± 0.029 R_Jup and a mass of 3.31 ±
  0.16 M_Jup, corresponding to a density of 1.31 ± 0.04 g/cm^3. The
  large radius of CoRoT-Exo-2b cannot be explained by current models of
  evolution of irradiated planets. <P />Based on observations obtained
  with CoRoT, a space project operated by the French Space Agency, CNES,
  with participation of the Science Programme of ESA, ESTEC/RSSD, Austria,
  Belgium, Brazil, Germany and Spain; and on observations made with
  SOPHIE spectrograph at Observatoire de Haute Provence, France (PNP.07
  A.MOUT), CORALIE, and HARPS spectrograph at ESO La Silla Observatroy
  (079.C-0127/F)). <P />Table 2 is only available in electronic form
  at http://www.aanda.org

Title: Transiting exoplanets from the CoRoT space
mission. I. CoRoT-Exo-1b: a low-density short-period planet around
    a G0V star
Authors: Barge, P.; Baglin, A.; Auvergne, M.; Rauer, H.; Léger,
   A.; Schneider, J.; Pont, F.; Aigrain, S.; Almenara, J. -M.; Alonso,
   R.; Barbieri, M.; Bordé, P.; Bouchy, F.; Deeg, H. J.; La Reza,
   De; Deleuil, M.; Dvorak, R.; Erikson, A.; Fridlund, M.; Gillon, M.;
   Gondoin, P.; Guillot, T.; Hatzes, A.; Hebrard, G.; Jorda, L.; Kabath,
   P.; Lammer, H.; Llebaria, A.; Loeillet, B.; Magain, P.; Mazeh, T.;
   Moutou, C.; Ollivier, M.; Pätzold, M.; Queloz, D.; Rouan, D.; Shporer,
   A.; Wuchterl, G.
Bibcode: 2008A&A...482L..17B
Altcode: 2008arXiv0803.3202B
  Context: The pioneer space mission for photometric planet searches,
  CoRoT, steadily monitors about 12 000 stars in each of its fields of
  view. Transit candidates can be detected early in the processing of the
  data and before the end of a run of observation. <BR />Aims: We report
  the detection of the first planet discovered by CoRoT and characterizing
  it with the help of follow-up observations. <BR />Methods: Raw data
  were filtered from outliers and residuals at the orbital period of
  the satellite. The orbital parameters and the radius of the planet
  were estimated by best fitting the phase folded light curve with 34
  successive transits. Doppler measurements with the SOPHIE spectrograph
  permitted us to secure the detection against binaries and to estimate
  the mass of the planet. <BR />Results: The accuracy of the data is
  very high with a dispersion in the 2.17 min binned phase-folded light
  curve that does not exceed ~3.×10<SUP>-4</SUP> in flux unit. The
  planet orbits a mildly metal-poor G0V star of magnitude V=13.6 in
  1.5 days. The estimated mass and radius of the star are 0.95±0.15
  M<SUB>⊙</SUB> and 1.11±0.05 R<SUB>⊙</SUB>. We find the planet
  has a radius of 1.49±0.08 R_Jup, a mass of 1.03±0.12 M_Jup, and
  a particularly low mean density of 0.38±0.05 g cm<SUP>-3</SUP>. <P
  />The CoRoT space mission, launched on Dec. 27th, 2006, was developed
  and is operated by the CNES, with participation of the Science
  Program of ESA, ESTEC/RSSD, Austria, Belgium, Brazil, Germany and
  Spain. Based in part on observations with the SOPHIE spectrograph
  at Obs. de Haute Provence, France. Table [see full text] is only
  available in electronic form at http://www.aanda.org Individual
  photometric measurements are only available in electronic form at
  the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or
  via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/482/L17

Title: Transiting exoplanets from the CoRoT space mission. III. The
    spectroscopic transit of CoRoT-Exo-2b with SOPHIE and HARPS
Authors: Bouchy, F.; Queloz, D.; Deleuil, M.; Loeillet, B.; Hatzes,
   A. P.; Aigrain, S.; Alonso, R.; Auvergne, M.; Baglin, A.; Barge, P.;
   Benz, W.; Bordé, P.; Deeg, H. J.; de La Reza, R.; Dvorak, R.; Erikson,
   A.; Fridlund, M.; Gondoin, P.; Guillot, T.; Hébrard, G.; Jorda, L.;
   Lammer, H.; Léger, A.; Llebaria, A.; Magain, P.; Mayor, M.; Moutou,
   C.; Ollivier, M.; Pätzold, M.; Pepe, F.; Pont, F.; Rauer, H.; Rouan,
   D.; Schneider, J.; Triaud, A. H. M. J.; Udry, S.; Wuchterl, G.
Bibcode: 2008A&A...482L..25B
Altcode: 2008arXiv0803.3209B
  We report on the spectroscopic transit of the massive hot-Jupiter
  CoRoT-Exo-2b observed with the high-precision spectrographs SOPHIE
  and HARPS. By modeling the radial velocity anomaly occurring during
  the transit due to the Rossiter-McLaughlin (RM) effect, we determine
  the sky-projected angle between the stellar spin and the planetary
  orbital axis to be close to zero λ = 7.2 ± 4.5 deg, and we secure
  the planetary nature of CoRoT-Exo-2b. We discuss the influence of
  the stellar activity on the RM modeling. Spectral analysis of the
  parent star from HARPS spectra are presented. <P />Observations made
  with SOPHIE spectrograph at Observatoire de Haute Provence, France
  (PNP.07A.MOUT) and HARPS spectrograph at ESO La Silla Observatory
  (079.C-0127(F)). The CoRoT space mission, launched on December 27th
  2006, has been developed and is operated by CNES, with the contribution
  of Austria, Belgium, Brasil, ESA, Germany, and Spain.

Title: Quasar Host Orientation and Polarization: Insights into the
    Type 1/Type 2 Dichotomy
Authors: Borguet, B.; Hutsemékers, D.; Letawe, G.; Letawe, Y.;
   Magain, P.
Bibcode: 2008RMxAC..32..167B
Altcode: 2007arXiv0710.4072B
  We investigate correlations between the optical linear polarization
  position angle and the orientation of the host galaxy/extended
  emission of Type 1 and Type 2 Radio-Loud (RL) and Radio-Quiet (RQ)
  quasars. We have used high resolution Hubble Space Telescope (HST)
  data and deconvolution process to obtain a good determination of the
  host galaxy orientation. With these new measurements and a compilation
  of data from the literature, we find a significant correlation between
  the polarization position angle and the position angle of the major
  axis of the host galaxy/extended emission. The correlation appears
  different for Type 1 and Type 2 objects and depends on the redshift
  of the source. Interpretations in the framework of the unification
  model are discussed.

Title: VizieR Online Data Catalog: CoRoT space mission. I. (Barge+,
    2008)
Authors: Barge, P.; Baglin, A.; Auvergne, M.; Rauer, H.; Leger, A.;
   Schneider, J.; Pont, F.; Aigrain, S.; Almenara, J. -M.; Alonso, R.;
   Barbieri, M.; Borde, P.; Bouchy, F.; Deeg, H. J.; de La, R. Reza;
   Deleuil, M.; Dvorak, R.; Erikson, A.; Fridlund, M.; Gillon, M.;
   Gondoin, P.; Guillot, T.; Hatzes, A.; Hebrard, G.; Jorda, L.; Kabath,
   P.; Lammer, H.; Llebaria, A.; Loeillet, B.; Magain, P.; Mazeh,
   T.; Moutou, C.; Ollivier, M.; Patzold, M.; Queloz, D.; Rouan, D.;
   Shporer, A.
Bibcode: 2008yCat..34829017B
Altcode:
  Raw data were filtered from outliers and residuals at the orbital period
  of the satellite. The orbital parameters and the radius of the planet
  were estimated by best fitting the phase folded light curve with 34
  successive transits. Doppler measurements with the SOPHIE spectrograph
  permitted us to secure the detection against binaries and to estimate
  the mass of the planet. <P />The individual photometric measurements
  will be available after the proprietary period of the CoRoT project. See
  http://smsc.cnes.fr/COROT for more information

Title: Slit and integral-field optical spectroscopy of the enigmatic
    quasar HE 0450-2958
Authors: Letawe, G.; Magain, P.; Courbin, F.
Bibcode: 2008A&A...480...69L
Altcode: 2007arXiv0709.3743L
  Context: Interest in the quasar HE 0450-2958 arose following the
  publication of the non-detection of its expected massive host, leading
  to various interpretations. <BR />Aims: This article investigates the
  gaseous and stellar contents of the system through additional VLT/FORS
  slit spectra and integral field spectroscopy from VLT/VIMOS. <BR
  />Methods: We apply our MCS deconvolution algorithm on slit spectra
  for the separation of the QSO and diffuse components, and develop a new
  method to remove the point sources in Integral Field Spectra, allowing
  extraction of velocity maps, narrow-line images, spatially resolved
  spectra or ionization diagrams of the surroundings of HE 0450-2958. <BR
  />Results: The whole system is embedded in gas, mostly ionized by
  the QSO radiation field and shocks associated with radio jets. The
  observed gas and star dynamics are unrelated, revealing a strongly
  perturbed system. Despite longer spectroscopic observations, the host
  galaxy remains undetected. <P />Based on observations made with VLT/UT1
  (program 76.B-0693(B)), and with the VLT/UT3 (program 72.B-0268(B))
  at ESO-Paranal observatory in Chile, in addition with NASA/ESA Hubble
  Space Telescope observations from Cycle 13, proposal #10238.

Title: Evidence of a type 1/type 2 dichotomy in the correlation
    between quasar optical polarization and host-galaxy/extended emission
    position angles
Authors: Borguet, B.; Hutsemékers, D.; Letawe, G.; Letawe, Y.;
   Magain, P.
Bibcode: 2008A&A...478..321B
Altcode: 2007arXiv0710.4048B
  Aims:For Seyfert galaxies, the AGN unification model provides a simple
  and well-established explanation of the type 1/type 2 dichotomy through
  orientation-based effects. The generalization of this unification
  model to the higher luminosity AGNs that quasars are remains a key
  question. The recent detection of type 2 radio-quiet quasars seems
  to support such an extension. We propose a further test of this
  scenario. <BR />Methods: On the basis of a compilation of quasar
  host-galaxy position angles consisting of previously published data and
  of new measurements performed using HST Archive images, we investigate
  the possible existence of a correlation between the linear polarization
  position angle and the host-galaxy/extended emission position angle of
  quasars. <BR />Results: We find that the orientation of the rest-frame
  UV/blue extended emission is correlated to the direction of the
  quasar polarization. For type 1 quasars, the polarization is aligned
  with the extended UV/blue emission, while these two quantities are
  perpendicular in type 2 objects. This result is independent of the
  quasar radio loudness. We interpret this (anti-)alignment effect in
  terms of scattering in a two-component polar+equatorial model that
  applies to both type 1 and type 2 objects. Moreover, the orientation
  of the polarization -and then of the UV/blue scattered light- does
  not appear correlated to the major axis of the stellar component of
  the host-galaxy measured from near-IR images.

Title: Study of the QSO HE0354-5500 with combined HST imaging and
    VLT spectroscopy . An example of a deconvolution-based method for
    probing the QSOs host galaxies characteristics
Authors: Letawe, Y.; Magain, P.; Letawe, G.; Courbin, F.; Hutsemékers,
   D.
Bibcode: 2008MmSAI..79.1251L
Altcode:
  The host galaxy of the QSO HE0354-5500 (M_B=-24.7, z=0.2674)
  is studied on the basis of high resolution HST optical images and
  spatially resolved VLT slit spectra. The morphology and dynamics of
  the host are described. The gas ionization and velocity are mapped
  as a function of the distance to the central QSO. Reflection or
  scattering of the QSO Halpha line from remote regions of the galaxy
  is detected. The line shifts show that the matter responsible for the
  light reflection moves away from the QSO, likely accelerated by its
  radiation pressure. Moreover, different resolved emission regions are
  found in the central kpc, both in the images and the spectra.

Title: A Multi-Wavelength Simultaneous Study of the Composition of
    the Halley-Family Comet 8P/Tuttle at the VLT
Authors: Bockelée-Morvan, D.; Dello Russo, N.; Jehin, E.; Manfroid,
   J.; Smette, A.; Cochran, A.; Hutsemékers, D.; Kawakita, H.; Kobayashi,
   H.; Schulz, R.; Weiler, M.; Zucconi, J. M.; Arpigny, C.; Biver,
   N.; Crovisier, J.; Magain, P.; Rauer, H.; Sana, H.; Vervack, R. J.;
   Weaver, H.
Bibcode: 2008LPICo1405.8190B
Altcode:
  No abstract at ADS

Title: VizieR Online Data Catalog: QSO Type1/Type2 dichotomy
    (Borguet+, 2008)
Authors: Borguet, B.; Hutsemekers, D.; Letawe, G.; Letawe, Y.;
   Magain, P.
Bibcode: 2007yCat..34780321B
Altcode:
  This table contains the measurements/compilation of host galaxy/
  extended emission position angle in the visible and near-IR domain,
  polarimetric data, and radio axis orientation for the 135 quasars of
  our sample. The angles are given in degrees east of north. The table
  gives the spectral and the radio-loud/radio-quiet classification of
  each object according to the references. <P />(2 data files).

Title: Deconvolution of HST images of the Cloverleaf gravitational
    lens. Detection of the lensing galaxy and a partial Einstein ring
Authors: Chantry, V.; Magain, P.
Bibcode: 2007A&A...470..467C
Altcode: 2006astro.ph.12094C
  Archival HST/NICMOS-2 images of the Cloverleaf gravitational lens
  (H1413+117), a quadruply-imaged quasar, were analysed with a new method
  derived from the MCS deconvolution algorithm (Magain et al. 1998). This
  method is based on an iterative process which simultaneously allows
  us to determine the Point Spread Function (PSF) and to perform
  a deconvolution of images containing several point sources plus
  extended structures. As such, it is well-adapted to the processing of
  gravitational lens images, especially in the case of multiply-imaged
  quasars. Two sets of data were analysed: the first one, which was
  obtained through the F160W filter in 1997, basically corresponds to a
  continuum image, while the second one, obtained through the narrower
  F180M filter in 2003, is centered around the forbidden [Oiii] emission
  lines at the source redshift, thus probing the narrow-line region of the
  quasar. The deconvolution gives astrometric and photometric measurements
  in both filters and reveals the primary lensing galaxy as well as a
  partial Einstein ring. The high accuracy of the results is particularly
  important in order to model the lensing system and to reconstruct the
  source undergoing the strong lensing. The reliability of the method
  is checked on a synthetic image similar to H1413+117. <P />Based
  on observations made with the NASA/ESA HST Hubble Space Telescope,
  obtained from the data archive at the Space Science Institute. STScI
  is operated by AURA, the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS-5-26555.

Title: DECPHOT: An Optimal Deconvolution-based Photometric Reduction
    Method
Authors: Gillon, M.; Magain, P.; Chantry, V.; Letawe, G.; Sohy, S.;
   Courbin, F.; Pont, F.; Moutou, C.
Bibcode: 2007ASPC..366..113G
Altcode: 2007astro.ph..1607G
  A high accuracy photometric reduction method is needed to take full
  advantage of the potential of the transit method for the detection and
  characterization of exoplanets, especially in deep crowded fields. In
  this context, we present DECPHOT, a new deconvolution-based photometry
  algorithm able to deal with a very high level of crowding and large
  variations of seeing. It also increases the resolution of astronomical
  images, an important advantage for the discrimination of false positives
  in transit photometry.

Title: On the Influence of Blends on the Potential of Ground-based
    Transit Surveys
Authors: Gillon, M.; Magain, P.
Bibcode: 2007ASPC..366..283G
Altcode: 2007astro.ph..1609G
  Transit surveys have to observe many stars all at once in order
  to compensate for the rarity of the searched events. Such surveys,
  especially the ones observing a deep field of view and/or broadening
  their stellar images, have to deal with a relatively high level of
  crowding. This crowding could lead to a reduction of the number of
  detectable transits, and the estimation of the potential of such
  surveys without taking into account the influence of blends could
  give overoptimistic results. We have developed a code which allows to
  estimate the extent by which such a survey is affected by the crowding
  of the field of view. Our results show that the influence of blends
  is important only for severe levels of crowding and is in general much
  less crucial than the influence of red noise.

Title: On-axis spectroscopy of the host galaxies of 20 optically
    luminous quasars at z ~ 0.3
Authors: Letawe, G.; Magain, P.; Courbin, F.; Jablonka, P.; Jahnke,
   K.; Meylan, G.; Wisotzki, L.
Bibcode: 2007MNRAS.378...83L
Altcode: 2007MNRAS.tmp..450L; 2006astro.ph..5288L
  We present the analysis of a sample of 20 bright low-redshift quasars
  (M<SUB>B</SUB> &lt; -23 and z &lt; 0.35) observed spectroscopically
  with the Very Large Telescope (VLT). The Focal Reducer/low dispersion
  Spectrograph (FORS1) spectra, obtained in Multi-Object Spectroscopy
  (MOS) mode, allow to observe simultaneously the quasars and several
  reference stars used to spatially deconvolve the data. Applying the
  Magain, Courbin &amp; Sohy (MCS) deconvolution method, we are able to
  separate the individual spectra of the quasar and of the underlying
  host galaxy. Contrary to some previous claims, we find that luminous
  quasars are not exclusively hosted by massive ellipticals. Most quasar
  host galaxies harbour large amounts of gas, irrespective of their
  morphological type. Moreover, the stellar content of half of the hosts
  is a young Sc-like population, associated with a rather low-metallicity
  interstellar medium. A significant fraction of the galaxies contain
  gas ionized at large distances by the quasar radiation. This large
  distance ionization is always associated with signs of gravitational
  interactions (as detected from images or disturbed rotation curves). The
  spectra of the quasars themselves provide evidence that gravitational
  interactions bring dust and gas in the immediate surrounding of the
  super massive black hole, allowing to feed it. The quasar activity
  might thus be triggered (1) in young gas-rich spiral galaxies by local
  events and (2) in more evolved galaxies by gravitational interactions
  or collisions. The latter mechanism gives rises to the most powerful
  quasars. Finally, we derive mass models for the isolated spiral
  host galaxies and we show that the most reliable estimators of the
  systemic redshift in the quasar spectrum are the tips of the Hα
  and Hβ lines. <P />Based on observations made with the European
  Southern Observatory (ESO) Very Large Telescope Unit 1 (ANTU/UT1)
  at ESO Paranal Observatory, Chile, under program IDs 65.P-0361 and
  66.B-0139. <P />E-mail: gletawe@ulg.ac.be

Title: The transiting planet OGLE-TR-132b revisited with new
    spectroscopy and deconvolution photometry<SUP>, </SUP>
Authors: Gillon, M.; Pont, F.; Moutou, C.; Santos, N. C.; Bouchy, F.;
   Hartman, J. D.; Mayor, M.; Melo, C.; Queloz, D.; Udry, S.; Magain, P.
Bibcode: 2007A&A...466..743G
Altcode: 2007astro.ph..2192G
  OGLE-TR-132b transits a very metal-rich F dwarf about 2000 pc from
  the Sun, in the Galactic disc towards Carina. It orbits very close
  to its host star (a = 0.03 AU) and has an equilibrium temperature
  of nearly 2000 K. Using rapid-cadence transit photometry from the
  FORS2 camera on the VLT and SUSI2 on the NTT, and high-resolution
  spectroscopy with UVES on the VLT, we refine the shape of the transit
  light curve and the parameters of the system. In particular, we
  improve the planetary radius estimate, R = 1.18 ± 0.07 R<SUB>J</SUB>
  and provide very precise ephemeris, T_tr = 2 453 142.59123 ± 0.0003
  BJD and P = 1.689868 ± 0.000003 days. The obtained planetary mass is
  1.14 ± 0.12 M_J. Our results give a slightly smaller and lighter star,
  and bigger planet, than previous values. As the VLT/FORS2 light curve
  obtained in this analysis with the deconvolution photometry algorithm
  DECPHOT shows a transit depth in disagreement with the one obtained
  by a previous study using the same data, we analyze them with two
  other reduction methods (aperture and image subtraction). The light
  curves obtained with the three methods are in good agreement, though
  deconvolution-based photometry is significantly more precise. It
  appears from these results that the smaller transit depth obtained in
  the previous study was due to a normalisation problem inherent to the
  reduction procedure used. <P />Based on data collected with the FORS2
  imager at the VLT-UT4 telescope (Paranal Observatory, ESO, Chile) in
  the programme 273.C-5017A, with the SUSI2 imager at the NTT telescope
  (La Silla Observatory, ESO, Chile) in the programme 075.C-0462A,
  and with the UVES spectrograph at the VLT-UT2 telescope (Paranal
  Observatory, ESO, Chile) in the programme 076.C-0131. The reduced
  photometric data used in this work are available only in electronic
  form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
  or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/466/743

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses. V. The time delay in SDSS J1650+4251
Authors: Vuissoz, C.; Courbin, F.; Sluse, D.; Meylan, G.; Ibrahimov,
   M.; Asfandiyarov, I.; Stoops, E.; Eigenbrod, A.; Le Guillou, L.;
   van Winckel, H.; Magain, P.
Bibcode: 2007A&A...464..845V
Altcode: 2006astro.ph..6317V
  Aims:Our aim is to measure the time delay between the two
  gravitationally lensed images of the z_qso = 1.547 quasar SDSS
  J1650+4251, in order to estimate the Hubble constant H_0. <BR
  />Methods: Our measurement is based on R-band light curves with 57
  epochs obtained at Maidanak Observatory, in Uzbekistan, from May 2004
  to September 2005. The photometry is performed using simultaneous
  deconvolution of the data, which provides the individual light curves
  of the otherwise blended quasar images. The time delay is determined
  from the light curves using two very different numerical techniques,
  i.e., polynomial fitting and direct cross-correlation. The time delay
  is converted into H<SUB>0</SUB> following analytical modeling of the
  potential well. <BR />Results: Our best estimate of the time delay is
  Δ t = 49.5 ± 1.9 days, i.e., we reach a 3.8% accuracy. The R-band
  flux ratio between the quasar images, corrected for the time delay
  and for slow microlensing, is F_A/F<SUB>B</SUB> = 6.2 ± 5%. <BR
  />Conclusions: .The accuracy reached on the time delay allows us
  to discriminate well between families of lens models. As for most
  other multiply imaged quasars, only models of the lensing galaxy
  that have a de Vaucouleurs mass profile plus external shear give
  a Hubble constant compatible with the current most popular value
  (H<SUB>0</SUB> = 72 ± 8 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>). A more
  realistic singular isothermal sphere model plus external shear gives
  H<SUB>0</SUB> = 51.7<SUP>+4.0</SUP><SUB>-3.0</SUB> km s<SUP>-1</SUP>
  Mpc<SUP>-1</SUP>. <P />Table [see full text] is only available in
  electronic form at http://www.aanda.org

Title: VizieR Online Data Catalog: Transiting planet OGLE-TR-132b
    (Gillon+, 2007)
Authors: Gillon, M.; Pont, F.; Moutou, C.; Santos, C. N.; Bouchy, F.;
   Hartman, D. J.; Mayor, M.; Melo, C.; Queloz, D.; Udry, S.; Magain, P.
Bibcode: 2007yCat..34660743G
Altcode:
  We present high-precision photometric coverage of two transits of the
  planet OGLE-TR-132b. These data have been obtained with the FORS2 camera
  on the VLT and the SUSI2 on the NTT. Both transits have been observed
  in the R filter. The deconvolution-based method DECPHOT (Gillon et
  al., 2006A&amp;A...459..249G, Magain et al., 2007A&amp;A...461..373M,
  Gillon et al., 2007, in prep.) was used to reduce the data. <P />(2
  data files).

Title: A deconvolution-based algorithm for crowded field photometry
    with unknown point spread function
Authors: Magain, P.; Courbin, F.; Gillon, M.; Sohy, S.; Letawe, G.;
   Chantry, V.; Letawe, Y.
Bibcode: 2007A&A...461..373M
Altcode: 2006astro.ph..9600M
  A new method is presented for determining the point <P />spread function
  (PSF) of images that lack bright and isolated <P />stars. It is based on
  the same principles as the MCS image <P />deconvolution algorithm. It
  uses the <P />information contained in all stellar images to achieve
  <P />the double task of reconstructing the PSFs for single or multiple
  <P />exposures of the same field and to extract the photometry of
  <P />all point sources in the field of view. The use of the full <P
  />information available allows us to construct an accurate PSF. The <P
  />possibility to simultaneously consider several exposures makes it <P
  />well suited to the measurement of the <P />light curves of blended
  point sources from data that would be <P />very difficult or even
  impossible to analyse with traditional PSF <P />fitting techniques. <P
  />The potential of the method for the <P />analysis of ground-based and
  space-based data is tested on <P />artificial images and illustrated by
  several examples, including <P />HST/NICMOS images of a lensed quasar
  and VLT/ISAAC images of <P />a faint blended Mira star in the halo of
  the giant elliptical <P />galaxy NGC 5128 (Cen A).

Title: High accuracy transit photometry of the planet OGLE-TR-113b
    with a new deconvolution-based method
Authors: Gillon, M.; Pont, F.; Moutou, C.; Bouchy, F.; Courbin, F.;
   Sohy, S.; Magain, P.
Bibcode: 2006A&A...459..249G
Altcode: 2006astro.ph..6395G
  A high accuracy photometry algorithm is needed to take full advantage
  of the potential of the transit method for the characterization of
  exoplanets, especially in deep crowded fields. It has to reduce to the
  lowest possible level the negative influence of systematic effects
  on the photometric accuracy. It should also be able to cope with a
  high level of crowding and with large-scale variations of the spatial
  resolution from one image to another. A recent deconvolution-based
  photometry algorithm fulfills all these requirements, and it also
  increases the resolution of astronomical images, which is an important
  advantage for the detection of blends and the discrimination of
  false positives in transit photometry. We made some changes to this
  algorithm <P />to optimize it for transit photometry and used it to
  reduce NTT/SUSI2 observations of two transits of OGLE-TR-113b. This
  reduction has led to two very high precision transit light curves
  with a low level of systematic residuals, used together with former
  photometric and spectroscopic measurements to derive new stellar and
  planetary parameters in excellent agreement with previous ones, but
  significantly more precise.

Title: VLT on-axis spectroscopy of quasar host galaxies
Authors: Letawe, G.; Magain, P.; Courbin, F.; Jablonka, P.; Meylan,
   G.; Jahnke, K.; Wisotzki, L.
Bibcode: 2006NewAR..50..779L
Altcode:
  We present the full analysis of our sample of 20 bright low
  redshift quasars (M<SUB>B</SUB> &lt; -23 and z &lt; 0.35),
  observed spectroscopically with the VLT FORS1, with objectives of
  characterizing the hosts and trying to understand how quasars are
  fueled or triggered. Applying the MCS deconvolution method, we are
  able to separate the galactic light from the quasar light, enabling
  i.e. global analysis of the gaseous and stellar content and gaseous
  dynamics. We find that 45% of the sample show signs of interaction,
  while half of the quasars are hosted in spiral galaxies, even when
  brighter than M<SUB>V</SUB> = -23.5. We also find many galaxies
  containing gas ionized by the quasar radiation far from the nucleus,
  all of these showing interaction or merger signs. We find spectroscopic
  evidences that such interactions bring gas in the broad and narrow
  line regions and power the nucleus.

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
Lenses.  II. SDSS J0924+0219: the redshift of the lensing galaxy,
    the quasar spectral variability and the Einstein rings
Authors: Eigenbrod, A.; Courbin, F.; Dye, S.; Meylan, G.; Sluse, D.;
   Vuissoz, C.; Magain, P.
Bibcode: 2006A&A...451..747E
Altcode: 2005astro.ph.10641E
  Aims.To provide the observational constraints required to use the
  gravitationally lensed quasar SDSS J0924+0219 for the determination
  of H<SUB>0</SUB> from the time delay method. We measure here the
  redshift of the lensing galaxy, we show the spectral variability of
  the source, and we resolve the lensed host galaxy of the source. <BR
  />Methods.We present our VLT/FORS1 deep spectroscopic observations
  of the lensed quasar SDSS J0924+0219, as well as archival HST/NICMOS
  and ACS images of the same object. The two-epoch spectra, obtained in
  the Multi Object Spectroscopy (MOS) mode, allow for very accurate flux
  calibration and spatial deconvolution. This strategy provides spectra
  for the lensing galaxy and for the quasar images A and B, free of any
  mutual light contamination. We deconvolve the HST images as well,
  which reveal a double Einstein ring. The mass distributions in the
  lens, reconstructed in several ways, are compared. <BR />Results.We
  determine the redshift of the lensing galaxy in SDSS J0924+0219:
  z_lens = 0.394±0.001. Only slight spectral variability is seen in
  the continuum of quasar images A and B, while the C III] , Mg II and
  Fe II emission lines display obvious changes. The flux ratio between
  the quasar images A and B is the same in the emission lines and in
  the continuum. One of the Einstein rings found using deconvolution
  corresponds to the lensed quasar host galaxy at z=1.524 and a second
  bluer one, is the image either of a star-forming region in the
  host galaxy, or of another unrelated lower redshift object. A broad
  range of lens models give a satisfactory fit to the data. However,
  they predict very different time delays, making SDSS J0924+0219 an
  object of particular interest for photometric monitoring. In addition,
  the lens models reconstructed using exclusively the constraints from
  the Einstein rings, or using exclusively the astrometry of the quasar
  images, are not compatible. This suggests that multipole-like structures
  play an important role in SDSS J0924+0219. <BR />

Title: The Host Galaxies of the Brightest Quasars: Gas-Rich Galaxies,
    Mergers, and Young Stars
Authors: Courbin, Frédéric; Letawe, Géraldine; Meylan, Georges;
   Magain, Pierre; Jablonka, Pascale; Jahnke, Knud; Wisotzki, Lutz;
   Letawe, Yannick; North, Pierre
Bibcode: 2006Msngr.124...32C
Altcode:
  Because they are faint and hidden in the glare of a much
  brighter unresolved source, quasar host galaxies still challenge
  the most powerful telescopes, instrumentation and processing
  techniques. Determining their basic morphological parameters and
  their integrated colours is feasible, but difficult, from imaging
  alone. However, detailed information on their stellar and gas contents
  and on their dynamics is achievable with deep spectroscopy.

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational
    Lenses.  III. Redshift of the lensing galaxy in eight gravitationally
    lensed quasars
Authors: Eigenbrod, A.; Courbin, F.; Meylan, G.; Vuissoz, C.;
   Magain, P.
Bibcode: 2006A&A...451..759E
Altcode: 2005astro.ph.11026E
  Aims.We measure the redshift of the lensing galaxy in eight
  gravitationally lensed quasars in view of determining the Hubble
  parameter H0 from the time delay method. <BR />Methods.Deep VLT/FORS1
  spectra of lensed quasars are spatially deconvolved in order to
  separate the spectrum of the lensing galaxies from the glare of the
  much brighter quasar images. A new observing strategy is devised. It
  involves observations in Multi-Object-Spectroscopy (MOS) which allows
  the simultaneous observation of the target and of several PSF and
  flux calibration stars. The advantage of this method over traditional
  long-slit observations is a much more reliable extraction and flux
  calibration of the spectra. <BR />Results.For the first time we measure
  the redshift of the lensing galaxy in three multiply-imaged quasars:
  SDSS J1138+0314 (z_lens = 0.445), SDSS J1226-0006 (z_lens = 0.517),
  SDSS J1335+0118 (z_lens = 0.440), and we give a tentative estimate of
  the redshift of the lensing galaxy in Q 1355-2257 (z_lens = 0.701). We
  confirm four previously measured redshifts: HE 0047-1756 (z_lens =
  0.407), HE 0230-2130 (z_lens = 0.523), HE 0435-1223 (z_lens = 0.454)
  and WFI J2033-4723 (z_lens = 0.661). In addition, we determine the
  redshift of the second lensing galaxy in HE 0230-2130 (z_lens =
  0.526). The spectra of all lens galaxies are typical for early-type
  galaxies, except for the second lensing galaxy in HE 0230-2130 which
  displays prominent [OII] emission. <BR />

Title: High precision determination of the atmospheric parameters
    and abundances of the COROT main targets
Authors: Gillon, M.; Magain, P.
Bibcode: 2006A&A...448..341G
Altcode: 2005astro.ph.11099G
  Context: .One of the main goals of the COROT mission is to get precise
  photometric observations of selected bright stars in order to allow
  the modelling of their interior through asteroseismology. However,
  in order to interpret the asteroseismological data, the effective
  temperature, surface gravity, and chemical composition of the stars
  must be known with sufficient accuracy.Aims.To carry out this task,
  we have developed a spectroscopic method called APASS (Atmospheric
  Parameters and Abundances from Synthetic Spectra) which allows precise
  analysis of stars with a moderate to high rotational velocity,
  which is the case for most primary COROT targets.Methods.Our
  method is based on synthetic spectra in which individual lines
  are replaced by analysis units (isolated lines or line blends,
  depending on the crowding of the spectral region and on the rotational
  broadening). It works differentially with respect to the Sun and allows
  the atmospheric parameters and chemical abundances to be determined
  by considering analysis units with different sensitivities to these
  various parameters.Results.Using high signal-to-noise spectra and the
  APASS method, we determined the atmospheric parameters and chemical
  abundances of 13 primary COROT targets. Our results agree well with
  those obtained by Bruntt using his software VWA and with those obtained
  with the software TEMPLOGG. However, in both cases, our error bars
  are significantly smaller than those of other methods. Our effective
  temperatures are also in excellent agreement with those obtained
  with the IR photometry method. For five stars with relatively low
  rotational velocity, we also performed an analysis with a classical
  equivalent-width method to test agreement with APASS results. We show
  that equivalent-width measurements by Gaussian or Voigt profile-fitting
  are sensitive to the rotational broadening, leading to systematic errors
  whenever the projected rotation velocity is non-negligible. The APASS
  method appears superior in all cases and should thus be preferred.

Title: On the potential of extrasolar planet transit surveys
Authors: Gillon, M.; Courbin, F.; Magain, P.; Borguet, B.
Bibcode: 2005A&A...442..731G
Altcode: 2005astro.ph..8109G
  We analyse the respective benefits and drawbacks of ground-based
  and space-based transit surveys for extrasolar planets. Based on
  simple but realistic assumptions about the fraction of lower main
  sequence stars harboring telluric and giant planets within the outer
  limit of the habitable zone, we predict the harvests of fictitious
  surveys with three existing wide field optical and near-IR cameras:
  the CFHT-Megacam, SUBARU-Suprime and VISTA-IR. An additional promising
  instrument is considered, VISTA-Vis, currently under development. The
  results are compared with the harvests predicted under exactly the same
  assumptions, for the space missions COROT and KEPLER. We show that
  ground-based wide field surveys may discover more giant planets than
  space missions. However, space surveys seem to constitute the best
  strategy to search for telluric planets. In this respect, the KEPLER
  mission appears 50 times more efficient than any of the ground-based
  surveys considered here. KEPLER might even discover telluric planets
  in the habitable zone of their host star.

Title: Photometric monitoring of the doubly imaged quasar UM 673:
    possible evidence for chromatic microlensing
Authors: Nakos, Th.; Courbin, F.; Poels, J.; Libbrecht, C.; Magain,
   P.; Surdej, J.; Manfroid, J.; Burud, I.; Hjorth, J.; Germany, L.;
   Lidman, C.; Meylan, G.; Pompei, E.; Pritchard, J.; Saviane, I.
Bibcode: 2005A&A...441..443N
Altcode: 2005astro.ph..7164N
  We present the results of two-band CCD photometric monitoring of the
  gravitationally lensed quasar Q 0142-100 (UM 673). The data, obtained
  at ESO-La Silla with the 1.54 m Danish telescope in the Gunn i-band
  (October 1998-September 1999) and in the Johnson V-band (October 1998
  to December 2001), were analyzed using three different photometric
  methods. The light-curves obtained with all methods show variations,
  with a peak-to-peak amplitude of 0.14 mag in V. Although it was not
  possible to measure the time delay between the two lensed QSO images,
  the brighter component displays possible evidence for microlensing:
  it becomes bluer as it gets brighter, as expected under the assumption
  of differential magnification of a quasar accretion disk.

Title: Chemical abundances in 43 metal-poor stars
Authors: Jonsell, K.; Edvardsson, B.; Gustafsson, B.; Magain, P.;
   Nissen, P. E.; Asplund, M.
Bibcode: 2005A&A...440..321J
Altcode: 2005astro.ph..5118J
  We have derived abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Fe,
  Ni, and Ba for 43 metal-poor field stars in the solar neighbourhood,
  most of them subgiants or turn-off-point stars with iron abundances
  [Fe/H] ranging from -0.4 to -3.0. About half of this sample has not been
  spectroscopically analysed in detail before. Effective temperatures
  were estimated from uvby photometry, and surface gravities primarily
  from Hipparcos parallaxes. The analysis is differential relative to
  the Sun, and was carried out with plane-parallel MARCS models. Various
  sources of error are discussed and found to contribute a total error
  of about 0.1-0.2 dex for most elements, while relative abundances,
  such as [Ca/Fe], are most probably more accurate. For the oxygen
  abundances, determined in an NLTE analysis of the 7774 Å triplet
  lines, the errors may be somewhat larger. We made a detailed comparison
  with similar studies and traced the reasons for the, in most cases,
  relatively small differences. Among the results we find that [O/Fe]
  possibly increases beyond [Fe/H] = -1.0, though considerably less so
  than in results obtained by others from abundances based on OH lines. We
  did not trace any tendency toward strong overionization of iron, and
  find the excesses, relative to Fe and the Sun, of the α elements Mg,
  Si, and Ca to be smaller than those of O. We discuss some indications
  that also the abundances of different α elements relative to Fe vary
  and the possibility that some of the scatter around the trends in
  abundances relative to iron may be real. This may support the idea that
  the formation of Halo stars occurred in smaller systems with different
  star formation rates. We verify the finding by Gratton et al. (2003b,
  A&amp;A, 406, 131) that stars that do not participate in the rotation
  of the galactic disk show a lower mean and larger spread in [ α/Fe]
  than stars participating in the general rotation. The latter stars also
  seem to show some correlation between [ α/Fe] and rotation speed. We
  trace some stars with peculiar abundances, among these two Ba stars,
  <ASTROBJ>HD 17072</ASTROBJ> and <ASTROBJ>HD 196944</ASTROBJ>, the
  second already known to be rich in s elements. Finally we advocate
  that a spectroscopic study of a larger sample of halo stars with
  well-defined selection criteria is very important, in order to add to
  the very considerable efforts that various groups have already made.

Title: Discovery of a bright quasar without a massive host galaxy
Authors: Magain, Pierre; Letawe, Géraldine; Courbin, Frédéric;
   Jablonka, Pascale; Jahnke, Knud; Meylan, Georges; Wisotzki, Lutz
Bibcode: 2005Natur.437..381M
Altcode: 2005astro.ph..9433M
  A quasar is thought to be powered by the infall of matter onto a
  supermassive black hole at the centre of a massive galaxy. Because
  the optical luminosity of quasars exceeds that of their host galaxy,
  disentangling the two components can be difficult. This led in
  the 1990s to the controversial claim of the discovery of `naked'
  quasars. Since then, the connection between quasars and galaxies has
  been well established. Here we report the discovery of a quasar lying
  at the edge of a gas cloud, whose size is comparable to that of a small
  galaxy, but whose spectrum shows no evidence for stars. The gas in the
  cloud is excited by the quasar itself. If a host galaxy is present,
  it is at least six times fainter than would normally be expected for
  such a bright quasar. The quasar is interacting dynamically with a
  neighbouring galaxy, whose gas might be feeding the black hole.

Title: Time Delay in Gravitational Lenses: an Alternative Route to
    the Hubble Constant
Authors: Magain, P.
Bibcode: 2005ASPC..335..207M
Altcode:
  The gravitational lens phenomenon is briefly introduced. When several
  images of the same variable quasar are observed, a determination of
  the time delay, i.e. the difference in light travel time between
  these different images can lead to a determination of distances
  between the source, the lens and the observer and, thus, of the Hubble
  constant. These determinations are compared to the more classical ones
  based on standard candles (Cepheids and Type Ia Supernovae).

Title: COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses
Authors: Courbin, F.; Eigenbrod, A.; Vuissoz, C.; Meylan, G.;
   Magain, P.
Bibcode: 2005IAUS..225..297C
Altcode:
  We describe a new project aiming at measuring time delays for most
  known lensed quasars, from optical light curves obtained with five
  (almost) dedicated 1-2 m telescopes in the Northern and Southern
  hemispheres. The goal is to evaluate the Hubble constant H<SUB>0</SUB>
  with a precision below 2%. We present here numerical simulations in
  order to define the optimal temporal sampling in our observations as
  a function of typical quasar variations, object visibility, and for
  a given accuracy on the individual photometric points. It is also
  emphasized that the ongoing effort to obtain deep imaging using both
  space and ground based facilities must be continued, as illustrated
  by the comparison of HST and VLT near-IR images of the `cloverleaf':
  H 1413+117.

Title: VizieR Online Data Catalog: Chemical abundances in 43
    metal-poor stars (Jonsell+, 2005)
Authors: Jonsell, K.; Edvardsson, B.; Gustafsson, B.; Magain, P.;
   Nissen, P. E.; Asplund, M.
Bibcode: 2005yCat..34400321J
Altcode:
  Data from an analysis of 43 metal-poor field stars with iron abundances
  [Fe/H] ranging from -0.4 to -3.0dex are presented here. Photometric
  data, stellar velocities, masses, fundamental parameters, spectral
  classifications and notations of possible binarity are given. Tables
  with line data for O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Fe, Ni and
  Ba, equivalent widths and resulting abundances are also given. <P />(4
  data files).

Title: Abundance correlations in mildly metal-poor stars. II. Light
    elements (C to Ca)
Authors: Decauwer, H.; Jehin, E.; Parmentier, G.; Magain, P.
Bibcode: 2005A&A...433..285D
Altcode:
  Accurate relative abundances have been obtained for carbon, oxygen,
  sodium, aluminium, silicon, and calcium in a sample of mildly metal-poor
  stars. This analysis complements a previous study carried out by Jehin
  et al. ([CITE], A&amp;A, 341, 241), which provided the basis for the
  EASE scenario. This scenario postulates that field metal-poor stars
  were born in self-enriched proto-globular cluster clouds. By further
  investigating the correlations between the different α-element
  abundances, we propose a modified scenario for the formation of
  intermediate metallicity stars, in which the stars exhibiting lower than
  average α/Fe abundance ratios would form in low mass clouds, unable to
  sustain the formation of very massive stars (M ⪆ 30~M_⊙). Moreover,
  the carbon-to-iron ratio is found to decrease as one climbs the
  so-called Population IIb branch, i.e. when the s-element abundance
  increases. In the framework of the EASE scenario, we interpret this
  anticorrelation between the carbon and the s-element abundances as a
  signature of a hot bottom burning process in the metal-poor AGB stars
  which expelled the matter subsequently accreted by our Population IIb
  stars. <P />Based on observations collected at the European Southern
  Observatory, La Silla, Chile (ESO Programmes 56.E-0384, 57.E-0400
  and 59.E-0257).

Title: The Influence of Blends on the Potential of Extrasolar Planets
    Transit Surveys
Authors: Gillon, M.; Magain, P.; Guillot, T.; Fressin, F.
Bibcode: 2005prpl.conf.8151G
Altcode: 2005LPICo1286.8151G
  No abstract at ADS

Title: α-elements in mildly metal-poor stars
Authors: Decauwer, H.; Jehin, E.; Parmentier, G.; Magain, P.
Bibcode: 2005IAUS..228..393D
Altcode:
  Accurate relative abundances of light elements (C to Ca) have
  been obtained in a sample of mildly metal-poor stars (Decauwer et
  al. 2005). Combined with the results of a previous study (Jehin et
  al. 1999), we find different slopes in the correlations between the
  different α-elements. These results can be explained by postulating
  that the stars exhibiting lower than average α/Fe form in low mass
  clouds, unable to sustain the formation of very massive stars.

Title: Chemical abundances in 43 metal-poor stars
Authors: Gustafsson, Bengt; Asplund, Martin; Edvardsson, Bengt;
   Jonsell, Karin; Magain, Pierre; Nissen, Poul Erik
Bibcode: 2005IAUS..228..259G
Altcode:
  We have derived abundances of O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Fe,
  Ni and Ba for 43 metal-poor field stars, mostly stars at the turn-off
  point and on the subgiant branch, in the interval {-}3.0{[Fe/H]{. The
  analysis is differential relative to the Sun. Oxygen abundances,
  with consideration of NLTE effects, were derived from the OI 777.4 nm
  triplet lines. We find [O/Fe] to gradually increase with decreasing
  [Fe/H], though considerably slower than has earlier been obtained from
  OH lines in the UV. A scatter in [O,Mg,Ca,Ti/Fe] at a given [Fe/H] is
  found and we argue that this scatter is partly real. The deviations from
  the mean trends of abundance ratios vs [Fe/H] are found to correlate
  in non-trivial ways for different abundances. Similar trends are found
  from results of accurate studies by other groups. This seems to give
  further evidence for the hypothesis that the stars once formed in
  different subsystems, with different star-formation rates.The paper
  is in press in A&amp;A, may be obtained as astro-ph/0505118.

Title: Abundance analysis of targets for the COROT/MONS
    asteroseismology missions. II. Abundance analysis of the COROT
    main targets
Authors: Bruntt, H.; Bikmaev, I. F.; Catala, C.; Solano, E.; Gillon,
   M.; Magain, P.; Van't Veer-Menneret, C.; Stütz, C.; Weiss, W. W.;
   Ballereau, D.; Bouret, J. C.; Charpinet, S.; Hua, T.; Katz, D.;
   Lignières, F.; Lueftinger, T.
Bibcode: 2004A&A...425..683B
Altcode: 2004astro.ph..3464B
  One of the goals of the ground-based support program for the COROT
  and MONS/RÖMER satellite missions is to characterize suitable target
  stars for the part of the missions dedicated to asteroseismology. We
  present the detailed abundance analysis of nine of the potential
  COROT main targets using the semi-automatic software VWA. For two
  additional COROT targets we could not perform the analysis due to
  the high rotational velocity of these stars. For five stars with low
  rotational velocity we have also performed abundance analysis by a
  classical equivalent width method in order to test the reliability
  of the VWA software. The agreement between the different methods is
  good. We find that it is necessary to measure abundances extracted
  from each line relative to the abundances found from a spectrum of
  the Sun in order to remove systematic errors. We have constrained the
  global atmospheric parameters T<SUB>eff</SUB>, log g, and [Fe/H] to
  within 70-100 K, 0.1-0.2 dex, and 0.1 dex for five stars which are slow
  rotators (v sin i &lt; 15 km s<SUP>-1</SUP>). For most of the stars we
  find good agreement with the parameters found from line depth ratios,
  H α lines, Strömgren indices, previous spectroscopic studies, and also
  log g determined from the HIPPARCOS parallaxes. For the fast rotators
  (v sin i &gt; 60 km s<SUP>-1</SUP>) it is not possible to constrain
  the atmospheric parameters. <P />Based on observations obtained with
  the 193 cm telescope at Observatoire de Haute Provence, France.

Title: On-axis spectroscopy of the z =0.144 radio-loud quasar HE
1434-1600: an elliptical host with a highly ionized ISM
Authors: Letawe, G.; Courbin, F.; Magain, P.; Hilker, M.; Jablonka,
   P.; Jahnke, K.; Wisotzki, L.
Bibcode: 2004A&A...424..455L
Altcode: 2004astro.ph..5309L
  VLT on-axis optical spectroscopy of the z=0.144 radio-loud quasar
  HE 1434-1600 is presented. The spatially resolved spectra of the
  host galaxy are deconvolved and separated from those of the central
  quasar in order to study the dynamics of the stars and gas as well
  as the physical conditions of the ISM. We find that the host of
  HE 1434-1600 is an elliptical galaxy that resides in a group of at
  least 5 member galaxies, and that most likely experienced a recent
  collision with its nearest companion. Compared with other quasar host
  galaxies, HE 1434-1600 has a highly ionized ISM. The ionization state
  corresponds to that of typical Seyferts, but the ionized regions are
  not distributed in a homogeneous way around the QSO, and are located
  preferentially several kiloparsecs away from it. While the stellar
  absorption lines do not show any significant velocity field, the gas
  emission lines do. The observed gas velocity field is hard to reconcile
  with dynamical models involving rotating disk, modified Hubble laws or
  power laws, that all require extreme central masses (M&gt;10<SUP>9</SUP>
  M<SUB>⊙</SUB>) to provide only poor fit to the data. Power law models,
  which best fit the data, provide a total mass of M(&lt;10 kpc) = 9.2 ×
  10<SUP>10</SUP> M<SUB>⊙</SUB>. We conclude that the recent interaction
  between HE 1434-1600 and its closest companion has strongly affected
  the gas velocity and ionization state, from the center of the galaxy
  to its most external parts. <P />Based on observations made with the
  ESO Very Large Telescope ANTU/UT1 at ESO-Paranal observatory, Chile
  (program 65.P-0361(A)).

Title: Accretion of Gas by Globular Cluster Stars
Authors: Thoul, A.; Jehin, E.; Magain, P.; Noels, A.; Parmentier,
   G.; Jorissen, A.; Goriely, S.
Bibcode: 2003ASPC..296..315T
Altcode: 2003nhgc.conf..315T
  No abstract at ADS

Title: On-axis VLT spectroscopy of quasar host galaxies: HE 1503+0228,
    at z=0.135
Authors: Courbin, F.; Letawe, G.; Magain, P.; Wisotzki, L.; Jablonka,
   P.; Jahnke, K.; Kuhlbrodt, B.; Alloin, D.; Meylan, G.
Bibcode: 2003ASPC..290..491C
Altcode: 2003agnc.conf..491C
  No abstract at ADS

Title: p-mode Oscillations of α Cen A
Authors: Thoul, A.; Scuflaire, R.; Vatovez, B.; Noels, A.; Magain,
   P.; Briquet, M.; Dupret, M. -A.
Bibcode: 2003Ap&SS.284..241T
Altcode:
  Models of α Cen A &amp; B have been computed using the masses
  determined by Pourbaix et al. (2002) and the data derived from the
  spectroscopic analysis of Neuforge and Magain (1997). The seismological
  data obtained by Bouchy and Carrier (2001, 2002) do help improve
  our knowledge of the evolutionary status of the system. All the
  constraints are satisfied with a model which gives an age of about 6
  Gyr for the binary.

Title: Variable Blue Stragglers and the EASE Scenario
Authors: Noels, A.; Scuflaire, R.; Magain, P.; Parmentier, G.;
   Thoul, A.
Bibcode: 2003aahd.conf..437N
Altcode:
  No abstract at ADS

Title: On-axis spatially resolved spectroscopy of low redshift quasar
host galaxies: HE 1503+0228, at z=0.135
Authors: Courbin, F.; Letawe, G.; Magain, P.; Wisotzki, L.; Jablonka,
   P.; Jahnke, K.; Kuhlbrodt, B.; Alloin, D.; Meylan, G.; Minniti, D.;
   Burud, I.
Bibcode: 2002A&A...394..863C
Altcode: 2002astro.ph..8514C
  We present the first result of a comprehensive spectroscopic study
  of quasar host galaxies. On-axis, spatially resolved spectra of low
  redshift quasars have been obtained with FORS1, mounted on the 8.2 m ESO
  Very Large Telescope, Antu. The spectra are spatially deconvolved using
  a spectroscopic version of the ``MCS deconvolution algorithm''. The
  algorithm decomposes two dimensional spectra into the individual spectra
  of the central point-like nucleus and of its host galaxy. Applied
  to HE 1503+0228 at z=0.135 (M<SUB>B</SUB>=-23.0), it provides us
  with the spectrum of the host galaxy between 3600 Å and 8500 Å
  (rest-frame), at a mean resolving power of 700. The data allow us to
  measure several of the important Lick indices. The stellar populations
  and gas ionization state of the host galaxy of HE 1503+0228 are very
  similar to the ones measured for normal non-AGN galaxies. Dynamical
  information is also available for the gas and stellar components of
  the galaxy. Using deconvolution and a deprojection algorithm, velocity
  curves are derived for emission lines, from the center up to 4\arcsec
  away from the nucleus of the galaxy. Fitting a simple three-components
  mass model (point mass, spherical halo of dark matter, disk) to the
  position-velocity diagram, we infer a mass of M(r&lt;1 kpc) = (2.0 +/-
  0.3)x 10<SUP>10</SUP> M<SUB>sun</SUB> within the central kiloparsec
  of the galaxy, and a mass integrated over 10 kpc of M(r&lt;10 kpc) =
  (1.9 +/- 0.3) x 10<SUP>11</SUP> M<SUB>sun</SUB>, with an additional 10%
  error due to the uncertainty on the inclination of the galaxy. This,
  in combination with the analysis of the stellar populations indicates
  that the host galaxy of HE 1503+0228, is a normal spiral galaxy. Based
  on observations made with ANTU/UT1 at ESO-Paranal observatory in
  Chile (program 65.P-0361(A)), and with the ESO 3.5 m NTT, at La Silla
  observatory (program 62.P-0643(B)).

Title: Time delay and lens redshift for the doubly imaged BAL quasar
    SBS 1520+530
Authors: Burud, I.; Hjorth, J.; Courbin, F.; Cohen, J. G.; Magain,
   P.; Jaunsen, A. O.; Kaas, A. A.; Faure, C.; Letawe, G.
Bibcode: 2002A&A...391..481B
Altcode: 2002astro.ph..6084B
  We present optical R-band light curves of the gravitationally lensed
  quasar <ASTROBJ>SBS 1520+530</ASTROBJ> derived from data obtained at
  the Nordic Optical Telescope. A time delay of 130+/-3 days (1sigma
  ) is determined from the light curves. In addition, spectra of
  <ASTROBJ>SBS 1520+530</ASTROBJ> obtained at the Keck Observatory
  are spatially deconvolved in order to extract the spectrum of the
  faint lensing galaxy, free of any contamination by the light from
  the bright quasar images. This spectrum indicates a lens redshift
  z=0.717, in agreement with one of the absorption systems found in
  the quasar spectra. The best mass model of the system includes a
  second nearby galaxy and a cluster of galaxies in addition to the
  main lensing galaxy. Adopting this model and an Omega =0.3, Lambda
  =0.7 cosmology, our time-delay measurement yields a Hubble constant
  of H<SUB>0</SUB>=51 +/- 9 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> (1sigma
  error). Based on observations made with the Nordic Optical, operated on
  the island of La Palma jointly by Denmark, Finland, Iceland, Norway,
  and Sweden, in the Spanish Observatorio del Roque de los Muchachos of
  the Instituto de Astrofisica de Canarias and the W. M. Keck Observatory
  which is operated jointly by the California Institute of Technology,
  the University of California and the National Aeronautics and Space
  Administration. Table 2 is only available in electronic form at the
  CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via
  http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/391/481

Title: VizieR Online Data Catalog: R-band photometry of SBS1520+530
    (Burud+, 2002)
Authors: Burud, I.; Hjorth, J.; Courbin, F.; Cohen, J. G.; Magain,
   P.; Jaunsen, A. O.; Kaas, A. A.; Faure, C.; Letawe, G.
Bibcode: 2002yCat..33910481B
Altcode:
  The table lists the data points obtained at the Nordic Optical Telescope
  used to derive the time delay for the lensed quasar QSO1520+530. (1
  data file).

Title: Spectroscopy of quasar host galaxies at the VLT: stellar
    populations and dynamics down to the central kiloparsec
Authors: Courbin, F.; Letawe, G.; Magain, P.; Wisotzki, L.; Jablonka,
   P.; Alloin, D.; Jahnke, K.; Kuhlbrodt, B.; Meylan, G.; Minniti, D.
Bibcode: 2002Msngr.107...28C
Altcode:
  1. Scientific Context 2. VLT Spectroscopic Observations 3. Spectra
  Decomposition and Stellar Population 4. Dynamics of the Host 5. Towards
  2D Spectroscopy and High Spatial Resolution: GIRAFFE, SINFONI and FALCON

Title: Accretion of gas by globular cluster stars
Authors: Thoul, A.; Jorissen, A.; Goriely, S.; Jehin, E.; Magain,
   P.; Noels, A.; Parmentier, G.
Bibcode: 2002A&A...383..491T
Altcode: 2002astro.ph..1341T
  Some recent observations of the abundances of s-process, r-process,
  and alpha elements in metal-poor stars have led to a new scenario
  for their formation. According to this scenario, these stars were
  born in a globular cluster and accreted the s-process enriched gas
  expelled by cluster stars of higher-mass, thereby modifying their
  surface abundances. Later on, these polluted stars evaporated from the
  globular cluster to constitute an important fraction of the current
  halo population. In addition, there are now many direct observations
  of abundance anomalies not only in globular cluster giant stars but
  also in subgiant and main-sequence stars. Accretion again provides a
  plausible explanation for (at least some of) these peculiarities. Here
  we investigate further the efficiency of the accretion scenario. We find
  that in concentrated clusters with large escape velocities, accretion
  is very efficient and can indeed lead to major modifications of the
  stellar surface abundances.

Title: Metallicity Gradients in Globular Cluster Systems : the Trace
    of a Self-Enrichment Process ?
Authors: Parmentier, G.; Magain, P.; Noels, A.; Thoul, A.; Jehin, E.
Bibcode: 2002IAUS..207..733P
Altcode:
  We have developed a model of globular cluster self-enrichment, based
  on the ability of the globular cluster gaseous progenitors to retain
  the ejecta of a first generation of Type II Supernovae. The key point
  is that this ability depends on the pressure exerted on the progenitor
  cloud by the surrounding protogalactic medium and therefore on the
  location of the cloud in the protogalaxy. The model is able to explain
  the galactic halo metallicities and the metallicity gradient of the
  Old Halo which is thought to be the genuine galactic globular cluster
  system. The possibility that metallicity gradients are a common property
  of extragalactic globular cluster systems is also presented.

Title: Evidence For a Self-Enrichment Process in Galactic Halo
    Globular Clusters
Authors: Parmentier, G.; Jehin, E.; Magain, P.; Noels, A.; Thoul, A.
Bibcode: 2002ASPC..285..234P
Altcode: 2002msfo.conf..234P
  No abstract at ADS

Title: An optical time-delay for the lensed BAL quasar HE 2149-2745
Authors: Burud, I.; Courbin, F.; Magain, P.; Lidman, C.; Hutsemékers,
   D.; Kneib, J. -P.; Hjorth, J.; Brewer, J.; Pompei, E.; Germany, L.;
   Pritchard, J.; Jaunsen, A. O.; Letawe, G.; Meylan, G.
Bibcode: 2002A&A...383...71B
Altcode: 2001astro.ph.12225B
  We present optical V and i-band light curves of the gravitationally
  lensed BAL quasar HE 2149-2745. The data, obtained with the 1.5 m Danish
  Telescope (ESO-La Silla) between October 1998 and December 2000, are
  the first from a long-term project aimed at monitoring selected lensed
  quasars in the Southern Hemisphere. A time delay of 103+/-12 days is
  determined from the light curves. In addition, VLT/FORS1 spectra of HE
  2149-2745 are deconvolved in order to obtain the spectrum of the faint
  lensing galaxy, free of any contamination by the bright nearby two
  quasar images. By cross-correlating the spectrum with galaxy-templates
  we obtain a tentative redshift estimate of z=0.495+/-0.01. Adopting this
  redshift, a Omega =0.3, Lambda =0.7 cosmology, and a chosen analytical
  lens model, our time-delay measurement yields a Hubble constant of
  H<SUB>0</SUB>=66 +/- 8 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> (1sigma
  error) with an estimated systematic error of +/-3 km s<SUP>-1</SUP>
  Mpc<SUP>-1</SUP>. Using non-parametric models yields H<SUB>0</SUB>=65
  +/- 8 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> (1sigma error) and confirms
  that the lens exhibits a very dense/concentrated mass profile. Finally,
  we note, as in other cases, that the flux ratio between the two quasar
  components is wavelength dependent. While the flux ratio in the broad
  emission lines - equal to 3.7 - remains constant with wavelength,
  the continuum of the brighter component is bluer. Although the data do
  not rule out extinction of one quasar image relative to the other as a
  possible explanation, the effect could also be produced by differential
  microlensing by stars in the lensing galaxy. Based on observations
  made with the Danish 1.5-m telescope (ESO, La Silla, Chile) and at VLT
  UT1 Antu (ESO-Paranal, Chile) (Proposals: 64.O-0205(B), 65.O-0214(B),
  66.A-0203(B), 67.A-0115(B), 66.B-0139(A) and HST archives ID 8175).

Title: A novel approach for extracting time-delays from lightcurves
    of lensed quasar images
Authors: Burud, I.; Magain, P.; Sohy, S.; Hjorth, J.
Bibcode: 2001A&A...380..805B
Altcode: 2001astro.ph.10668B
  We present a new method to estimate time delays from light curves of
  lensed quasars. The method is based on chi <SUP>2</SUP> minimization
  between the data and a numerical model light curve. A linear variation
  can be included in order to correct for slow long-term microlensing
  effects in one of the lensed images. An iterative version of the method
  can be applied in order to correct for higher-order microlensing
  effects. The method is tested on simulated light curves. When
  higher-order microlensing effects are present, the time delay is best
  constrained with the iterative method. Analysis of a published data
  set for the lensed double Q 0957+561 yields results in agreement with
  other published estimates.

Title: Deconvolving Spectra: Near-IR Spectroscopy of the Lens and
    Source in HE 1104-1805
Authors: Courbin, F.; Lidman, C.; Meylan, G.; Magain, P.
Bibcode: 2001ASPC..237...85C
Altcode: 2001glrp.conf...85C
  No abstract at ADS

Title: What Happens to the Gas in Globular Clusters?
Authors: Thoul, A.; Jehin, E.; Magain, P.; Noels, A.; Parmentier, G.
Bibcode: 2001ASPC..228..571T
Altcode: 2001dscm.conf..571T
  No abstract at ADS

Title: An Optical Time Delay Estimate for the Double Gravitational
    Lens System B1600+434
Authors: Burud, I.; Hjorth, J.; Jaunsen, A. O.; Andersen, M. I.;
   Korhonen, H.; Clasen, J. W.; Pelt, J.; Pijpers, F. P.; Magain, P.;
   Østensen, R.
Bibcode: 2000ApJ...544..117B
Altcode: 2000astro.ph..7136B
  We present optical I-band light curves of the gravitationally
  lensed double QSO B1600+434 from observations obtained at the Nordic
  Optical Telescope (NOT) between 1998 April and 1999 November. The
  photometry has been performed by simultaneous deconvolution of all
  the data frames, involving a numerical lens galaxy model. Four
  methods have been applied to determine the time delay between
  the two QSO components, giving a mean estimate of Δt=51+/-4 days
  (95% confidence level). This is the fourth optical time delay ever
  measured. Adopting a Ω=0.3, Λ=0 universe and using the mass model
  of Maller et al., this time delay estimate yields a Hubble parameter
  of H<SUB>0</SUB>=52<SUP>+14</SUP><SUB>-8</SUB> km s<SUP>-1</SUP>
  Mpc<SUP>-1</SUP> (95% confidence level), where the errors include time
  delay as well as model uncertainties. There are time-dependent offsets
  between the two (appropriately shifted) light curves that indicate
  the presence of external variations due to microlensing. Based on
  observations made with the Nordic Optical Telescope, operated on the
  island of La Palma jointly by Denmark, Finland, Iceland, Norway, and
  Sweden, in the Spanish Observatorio del Roque de los Muchachos of the
  Instituto de Astrofisica de Canarias.

Title: The Old Halo metallicity gradient: the trace of a
    self-enrichment process
Authors: Parmentier, G.; Jehin, E.; Magain, P.; Noels, A.; Thoul, A. A.
Bibcode: 2000A&A...363..526P
Altcode: 2000astro.ph..9477P
  Based on a model of globular cluster self-enrichment published in a
  previous paper, we present an explanation for the metallicity gradient
  observed throughout the galactic Old Halo. Our self-enrichment model is
  based on the ability of globular cluster progenitor clouds to retain
  the ejecta of a first generation of Type II Supernovae. The key point
  is that this ability depends on the pressure exerted on the progenitor
  cloud by the surrounding protogalactic medium and therefore on the
  location of the cloud in the protoGalaxy. Since there is no significant
  (if any) metallicity gradient in the whole halo, we also present a
  review in favour of a galactic halo partly built via accretions and
  mergers of satellite systems. Some of them bear their own globular
  clusters and therefore ``contaminate'' the system of globular clusters
  formed ``in situ'', namely within the original potential well of the
  Galaxy. Therefore, the comparison between our self-enrichment model
  and the observational data should be limited to the genuine galactic
  globular clusters, the so-called Old Halo group.

Title: Lensed quasars: a matter of resolution
Authors: Courbin, F.; Lidman, C.; Burud, I.; Hjorth, J.; Magain, P.;
   Golse, G.; Castander, F.
Bibcode: 2000Msngr.101...20C
Altcode: 2000Msngr.101...17C
  The interest in studying lensed quasars amongst the astronomical
  community has always been somewhat fluctuating. Periods of great
  enthusiasm and of profound disappointment have regularly followed
  one another.

Title: Exploring the gravitationally lensed system HE 1104-1805:
    near-IR spectroscopy
Authors: Courbin, F.; Lidman, C.; Meylan, G.; Kneib, J. -P.; Magain, P.
Bibcode: 2000A&A...360..853C
Altcode: 2000astro.ph..6168C
  A new technique for the spatial deconvolution of spectra is applied to
  near-IR (0.95-2.50 μm) NTT/SOFI spectra of the lensed, radio-quiet
  quasar HE 1104-1805. The continuum of the lensing galaxy is revealed
  between 1.5 μm and 2.5 μm. Although the spectrum does not show strong
  emission features, it is used in combination with previous optical
  and IR photometry to infer a plausible redshift in the range 0.8 &lt;
  z &lt; 1.2. Modeling of the system shows that the lens is complex,
  probably composed of the red galaxy seen between the quasar images
  and a more extended component associated with a galaxy cluster with
  fairly low velocity dispersion (~ 575 km s<SUP>-1</SUP>). Unless
  more constrains can be put on the mass distribution of the cluster,
  e.g. from deep X-ray observations, HE 1104-1805 will not be a good
  system to determine H<SUB>0</SUB>. We stress that multiply imaged
  quasars with known time delays may prove more useful as tools
  for detecting dark mass in distant lenses than for determining
  cosmological parameters. The spectra of the two lensed images of the
  source are of great interest. They show no trace of reddening at the
  redshift of the lens nor at the redshift of the source. This supports
  the hypothesis of an elliptical lens. Additionally, the difference
  between the spectrum of the brightest component and that of a scaled
  version of the faintest component is a featureless continuum. Broad
  and narrow emission lines, including the FeII features, are perfectly
  subtracted. The very good quality of our spectrum makes it possible
  to fit precisely the optical Fe II feature, taking into account the
  underlying continuum over a wide wavelength range. HE 1104-1805 can be
  classified as a weak Fe II emitter. Finally, the slope of the continuum
  in the brightest image is steeper than the continuum in the faintest
  image and supports the finding by Wisotzki et al. (1993) that the
  brightest image is microlensed. This is particularly interesting in
  view of the new source reconstruction methods from multiwavelength
  photometric monitoring. While HE 1104- 1805 does not seem the best
  target for determining cosmological parameters, it is probably the
  second most interesting object after Q 2237+0305 (the Einstein cross),
  in terms of microlensing. Based on observations collected with the
  ESO New Technology Telescope (program 61.B-0413)

Title: Resolved stellar populations of super-metal-rich star clusters
    in the bulge of M 31
Authors: Jablonka, P.; Courbin, F.; Meylan, G.; Sarajedini, A.;
   Bridges, T. J.; Magain, P.
Bibcode: 2000A&A...359..131J
Altcode: 2000astro.ph..5040J
  We have applied the MCS image deconvolution algorithm (Magain et
  al. 1998) to HST/WFPC2 V, I data of three M 31 bulge globular clusters
  (G170, G177, and G198) and control fields near each cluster. All three
  clusters are clearly detected, with an increase in stellar density
  with decreasing radius from the cluster centers; this is the first time
  that stars have been resolved in bulge clusters in the inner regions of
  another galaxy. From the RGB slopes of the clusters and the difference
  in I magnitude between the HB and the top of the RGB, we conclude that
  these three clusters all have roughly solar metallicity, in agreement
  with earlier integrated-light spectroscopic measurements. Our data
  support a picture whereby the M 31 bulge clusters and field stars were
  born from the same metal-rich gas, early in the galaxy formation.

Title: Were the Old Halo globular clusters able to sustain a
    self-enrichment phase?
Authors: Parmentier, Geneviève; Jehin, Emmanuel; Magain, Pierre;
   Noels, Arlette; Thoul, Anne
Bibcode: 2000NewAR..44..351P
Altcode:
  It has been argued for a long time that the self-enrichment process
  could not occur within proto-globular clouds because of the supernova
  energetics. We revisit this argument and demonstrate that it may
  not be true. Since not all the kinetic energy of Type II Supernovae
  is deposited as kinetic energy of the ISM, we suggest comparing the
  binding energy of the progenitor cloud to the kinetic energy of the
  ISM instead of the kinetic energy of the Type II Supernova ejecta. This
  criterion is used to study the disruptive ability of Type II Supernovae
  onto proto-globular clouds. It is found that the early chemical history
  of globular clusters is greatly influenced by the pressure exerted by
  the external medium on their progenitor clouds.

Title: Observational Constraints on a Self-Enrichment Model in
    Galactic Halo Globular Clusters
Authors: Parmentier, G.; Jehin, E.; Magain, P.; Noels, A.; Thoul, A.
Bibcode: 2000ESASP.445..483P
Altcode: 2000sfsl.conf..483P
  No abstract at ADS

Title: A Method for Spatial Deconvolution of Spectra
Authors: Courbin, F.; Magain, P.; Kirkove, M.; Sohy, S.
Bibcode: 2000ApJ...529.1136C
Altcode: 1999astro.ph..9109C
  A method for spatial deconvolution of spectra is presented. It follows
  the same fundamental principles as the ``MCS image deconvolution
  algorithm'' recently developed by Magain, Courbin, &amp; Sohy and
  uses information contained in the spectrum of a reference point-spread
  function to spatially deconvolve spectra of very blended sources. An
  improved resolution rather than an infinite one is aimed at, overcoming
  the well-known problem of ``deconvolution artifacts.'' As in the
  MCS algorithm, the data are decomposed into a sum of analytical point
  sources and a numerically deconvolved background so that the spectrum of
  extended sources in the immediate vicinity of bright point sources may
  be accurately extracted and sharpened. The algorithm has been tested on
  simulated data including seeing variation as a function of wavelength
  and atmospheric refraction. It is shown that the spectra of severely
  blended point sources can be resolved while fully preserving the
  spectrophotometric properties of the data. Extended objects ``hidden''
  by bright point sources (up to 4-5 mag brighter) can be accurately
  recovered as well, provided the data have a sufficiently high total
  signal-to-noise ratio (200-300 per spectral resolution element). Such
  spectra are relatively easy to obtain, even down to faint magnitudes,
  within a few hours of integration time with 10 m class telescopes.

Title: POX 186: the ultracompact blue compact dwarf galaxy reveals
    its nature
Authors: Doublier, V.; Kunth, D.; Courbin, F.; Magain, P.
Bibcode: 2000A&A...353..887D
Altcode: 1999astro.ph..2294D; 1999astro.ph..2294V
  High resolution, ground based R and I band observations of the ultra
  compact dwarf galaxy POX 186 are presented. The data, obtained with
  the ESO New Technology Telescope (NTT), are analyzed using a new
  deconvolution algorithm which allows one to resolve the innermost
  regions of this stellar-like object into three Super-Star Clusters
  (SSC). Upper limits to both masses (M ~ 10<SUP>5</SUP> M<SUB>sun</SUB>)
  and physical sizes (&lt;=60pc) of the SSCs are set. In addition,
  and maybe most importantly, extended light emission underlying the
  compact star-forming region is clearly detected in both bands. The R-I
  color rules out nebular Hα contamination and is consistent with an old
  stellar population. This casts doubt on the hypothesis that Blue Compact
  Dwarf Galaxies (BCDG) are young galaxies. based on observations carried
  out at NTT in La Silla, operated by the European Southern Observatory,
  during Director's Discretionary Time.

Title: Abundance correlations in thick disk and halo stars
Authors: Jehin, E.; Magain, P.; Noels, A.; Parmentier, G.; Thoul, A.
Bibcode: 2000LIACo..35..151J
Altcode: 2000ghgc.conf..151J
  No abstract at ADS

Title: On the possibility of self-enrichement in globular clusters
Authors: Parmentier, G.; Jehin, E.; Magain, P.; Neuforge, C.; Noels,
   A.; Thoul, A. A.
Bibcode: 2000LIACo..35..561P
Altcode: 2000ghgc.conf..561P
  No abstract at ADS

Title: Puzzling locations of mildly metal-poor stars in the HR diagram
Authors: Jehin, E.; Noels, A.; Magain, P.; Parmentier, G.; Thoul, A.
Bibcode: 2000LIACo..35..231J
Altcode: 2000ghgc.conf..231J
  No abstract at ADS

Title: The metallicity gradient of the old halo
Authors: Parmentier, G.; Jehin, E.; Magain, P.; Noels, A.; Thoul, A.
Bibcode: 2000LIACo..35..623P
Altcode: 2000ghgc.conf..623P
  No abstract at ADS

Title: Accretion from AGB winds.
Authors: Thoul, A.; Jorissen, A.; Goriely, S.; Jehin, E.; Magain,
   P.; Noels, A.; Parmentier, G.
Bibcode: 2000MmSAI..71..791T
Altcode:
  No abstract at ADS

Title: The EASE Scenario: Dynamical Study of the Supernova Phase
Authors: Parmentier, Geneviève; Jehin, Emannuel; Magain, Pierre;
   Noels, Arlette; Thoul, Anne
Bibcode: 2000fist.conf..199P
Altcode:
  We revisit the most often encountered argument against self-enrichment
  in globular clusters, namely the ability of a few number of supernovae
  to disrupt the proto-globular cloud. We show that, within the context
  of the Fall and Rees theory, primordial proto-globular cluster clouds
  may sustain several hundreds of Type II supernovae. Furthermore, the
  corresponding self-enrichment level is in agreement with galactic halo
  globular cluster metallicities.

Title: The Galactic Halo : from Globular Clusters to Field Stars
Authors: Noels, A.; Magain, P.; Caro, D.; Jehin, E.; Parmentier, G.;
   Thoul, A. A.
Bibcode: 2000LIACo..35.....N
Altcode: 2000ghgc.conf.....N
  The following topics were dealt with: early galactic nucleosynthesis;
  chemical composition of metal-poor stars; metal-poor components of
  our Galaxy; HR diagrams of globular clusters; chemical and dynamical
  evolution of globular clusters.

Title: Accretion processes onto globular cluster stars
Authors: Thoul, A.; Jorissen, A.; Goriely, S.; Jehin, E.; Magain,
   P.; Noels, A.; Parmentier, G.
Bibcode: 2000LIACo..35..567T
Altcode: 2000ghgc.conf..567T
  No abstract at ADS

Title: What Happens to the Gas in Globular Clusters?
Authors: Thoul, A.; Jehin, E.; Magain, P.; Noels, A.; Parmentier, G.
Bibcode: 2000AGM....16..P86T
Altcode:
  Observations of globular clusters show that they contain much too
  little gas or dust, compared to what should be present due to the
  mass-losing stars in the cluster. Many authors have been intrigued
  by the fate of the gas in globular clusters. They have suggested
  various mechanisms by which the gas could escape from the cluster,
  such as stellar UV radiation, cluster winds driven by X-ray bursters,
  novae, or flare-stars, relativistic winds from millisecond pulsars,
  condensation into stars, accretion processes drawing upon a central
  gas reservoir, continuous sweeping of the cluster gas by the gaseous
  medium of the Galactic halo dots. Recent results also show that globular
  cluster stars show many abundance anomalies. Accretion of interstellar
  gas by the cluster stars has been suggested as a plausible mechanism
  to explain these anomalies. It is also a major ingredient of the EASE
  scenario linking halo field stars to globular clusters, which we have
  recently developed to explain strong r-and s-elements correlations
  in halo field dwarf stars. Here we will briefly review the status of
  gas and dust detection in globular clusters, as well as the possible
  gas removal mechanisms. We will explore in more details the gas and
  dust accretion processes onto main sequence stars. In particular,
  we will study the efficiency of this mechanism in removing gas from
  the globular clusters interstellar medium.

Title: The Galactic halo. From globular clusters to field
    stars. Proceedings.
Authors: Noels, A.; Magain, P.; Caro, D.; Jehin, E.; Parmentier, G.;
   Thoul, A.
Bibcode: 2000ghfg.book.....N
Altcode:
  The following topics were dealt with: early galactic nucleosynthesis;
  chemical composition of metal-poor stars; metal-poor components of
  our Galaxy; HR diagrams of globular clusters; chemical and dynamical
  evolution of globular clusters.

Title: The EASE Scenario: A New Origin for Metal-Poor Stars?
Authors: Jehin, Emmanuel; Magain, Pierre; Noels, Arlette; Parmentier,
   Geneviève; Thoul, Anne
Bibcode: 2000fist.conf..204J
Altcode:
  We have analysed high resolution and high signal-to-noise spectra
  of 21 mildly metal-poor stars. The correlations between the relative
  abundances of 16 elements have been studied, with a special emphasis
  on the neutron-capture ones. This analysis reveals the existence of two
  sub-populations of field metal-poor stars which differ by the behaviour
  of the s-process elements versus the α and r-process elements. We
  suggest a scenario for the formation of metal-poor stars, which closely
  relates the origin of these stars to the evolution of globular clusters.

Title: Deep Imaging of AX J2019+112: The Luminosity of a ``Dark
    Cluster''
Authors: Benítez, Narciso; Broadhurst, Tom; Rosati, Piero; Courbin,
   Fred; Squires, Gordon; Lidman, Chris; Magain, Pierre
Bibcode: 1999ApJ...527...31B
Altcode: 1998astro.ph.12218B
  We detect a distant cluster of galaxies centered on the
  QSO lens and luminous X-ray source AX J2019+112, a.k.a. the
  ``Dark Cluster.'' Using deep V and I Keck images and wide-field
  K<SUB>s</SUB> imaging from the New Technology Telescope (NTT),
  a tight red sequence of galaxies is identified within a radius
  of 0.2 h<SUP>-1</SUP> Mpc of the known z=1.01 elliptical lensing
  galaxy. The sequence, which includes the central elliptical galaxy,
  has a slope in good agreement with the model predictions of Kodama
  et al. for z~1. We estimate the integrated rest-frame luminosity
  of the cluster to be L<SUB>V</SUB>&gt;=3.2×10<SUP>11</SUP>
  h<SUP>-2</SUP> L<SUB>solar</SUB> (after accounting for significant
  extinction at the low latitude of this field), more than an order
  of magnitude higher than previous estimates. The central region
  of the cluster is deconvolved using the technique of Magain,
  Courbin, &amp; Sohy, revealing a thick central arc coincident with
  an extended radio source. All the observed lensing features are
  readily explained by differential magnification of a radio-loud
  active galactic nucleus by a shallow elliptical potential. The QSO
  must lie just outside the diamond caustic, producing two images;
  the arc is a highly magnified image formed from a region close to
  the center of the host galaxy, projecting inside the caustic. The
  mass-to-light ratio within an aperture of 0.4 h<SUP>-1</SUP> Mpc is
  M<SUB>X</SUB>/L<SUB>V</SUB>=224<SUP>+112</SUP><SUB>-78</SUB>h(M/L<SUB>V</SUB>)<SUB>solar</SUB>,
  using the X-ray temperature. The
  strong lens model yields a compatible value,
  M/L<SUB>V</SUB>=372<SUP>+94</SUP><SUB>-94</SUB>h(M/L<SUB>V</SUB>)<SUB>solar</SUB>,
  whereas an independent weak-lensing analysis sets an upper limit of
  M/L<SUB>V</SUB>&lt;520h(M/L<SUB>V</SUB>)<SUB>solar</SUB>, typical of
  massive clusters. <P />Based on observations collected at the European
  Southern Observatory, La Silla, Chile, proposal number 61.A-0676.

Title: The self-enrichment of galactic halo globular clusters. A
    clue to their formation?
Authors: Parmentier, G.; Jehin, E.; Magain, P.; Neuforge, C.; Noels,
   A.; Thoul, A. A.
Bibcode: 1999A&A...352..138P
Altcode: 1999astro.ph.11258P
  We present a model of globular cluster self-enrichment. In the
  protogalaxy, cold and dense clouds embedded in the hot protogalactic
  medium are assumed to be the progenitors of galactic halo globular
  clusters. The massive stars of a first generation of metal-free stars,
  born in the central areas of the proto-globular cluster clouds, explode
  as Type II supernovae. The associated blast waves trigger the expansion
  of a supershell, sweeping all the material of the cloud, and the heavy
  elements released by these massive stars enrich the supershell. A second
  generation of stars is born in these compressed and enriched layers
  of gas. These stars can recollapse and form a globular cluster. This
  work aims at revising the most often encountered argument against
  self-enrichment, namely the presumed ability of a small number of
  supernovae to disrupt a proto-globular cluster cloud. We describe a
  model of the dynamics of the supershell and of its progressive chemical
  enrichment. We show that the minimal mass of the primordial cluster
  cloud required to avoid disruption by several tens of Type II supernovae
  is compatible with the masses usually assumed for proto-globular
  cluster clouds. Furthermore, the corresponding self-enrichment level
  is in agreement with halo globular cluster metallicities.

Title: Deconvolving spectra of lensing galaxies, QSO hosts, and
    more ...
Authors: Courbin, F.; Magain, P.; Sohy, S.; Lidman, C.; Meylan, G.
Bibcode: 1999Msngr..97...26C
Altcode:
  High spatial resolution undoubtedly plays a key role in most major
  advances in observational astrophysics. In this context, considerable
  effort has been devoted to the development of numerical methods aimed
  at improving the spatial resolution of astronomical images. However,
  the most commonly used techniques (e.g., Richardson 1972, Lucy
  1974, Skilling &amp; Bryan 1984) tend to produce the so-called
  “deconvolution artefacts” (oscillations in the vicinity of
  high spatial frequency structures) which alter the photometric
  and astrometric properties of the original data. Recently, Magain,
  Courbin &amp; Sohy (1998ab; hereafter MCS) proposed and implemented
  a new deconvolution algorithm which overcomes such drawbacks. Its
  success is mainly the consequence of a deliberate choice to achieve
  an improved resolution rather than an infinite one, hence avoiding
  retrieving spatial frequencies forbidden by the sampling theorem.

Title: Linking Field Metal-Poor Stars and Globular Clusters: the
    Ease Scenario
Authors: Jehin, E.; Magain, P.; Neuforge, C.; Noels, A.; Parmentier,
   G.; Thoul, A.
Bibcode: 1999Ap&SS.265..287J
Altcode:
  No abstract at ADS

Title: About the origin of extinction in the gravitational lens
    system MG J0414+0534
Authors: Angonin-Willaime, M. -C.; Vanderriest, C.; Courbin, F.;
   Burud, I.; Magain, P.; Rigaut, F.
Bibcode: 1999A&A...347..434A
Altcode:
  Photometric measurements of the highly reddened gravitational mirage
  MG J0414+0534 have been carried out either by PSF subtraction or
  by applying accurate deconvolution algorithms to optical (R, I) and
  near-infrared (K) images obtained at CFHT and NOT under sub-arcsecond
  seeing conditions. It is confirmed that the close pair of images
  A1-A2 suffers a larger extinction than B and C. While the colours
  of image A2 obtained from ground-based data seem inconsistent with
  a simple reddening law, higher resolution images available from
  HST archives reveal an additional extended component (arc) which
  introduces significant errors in the photometric decomposition. When
  the arc component is properly taken into account, the colours of the 4
  nucleus images do agree with a classical reddening law, with A2 being
  by far the most obscured component. Such a differential extinction
  (maximum difference Delta E(R-I) =~ 0.6) is likely due to the lensing
  galaxy. This does not mean that {all} the extinction occurs into the
  lens. Indeed, the fact that the arc is much less red than the images
  of the nucleus suggests that an important part of the reddening is
  intrinsic to the source. Finally, no significant variability is
  observed within this data set, i.e. between 1994 and 1997, while
  a discrepancy from earlier data is noticed for (A1 + A2). Based on
  observations collected with the Canada-France-Hawaii Telescope at
  Mauna Kea (Hawaii, USA), the Nordic Optical Telescope (Canary, Spain)
  and archive data from the Hubble Space Telescope (NASA/ESA)

Title: BIMA and Keck Imaging of the Radio Ring PKS 1830-211
Authors: Frye, B. L.; Courbin, F.; Broadhurst, T. J.; Welch, W. J. W.;
   Lidman, C.; Magain, P.; Pahre, M.; Djorgovski, S. G.
Bibcode: 1999ASPC..156..240F
Altcode: 1998astro.ph..2347F; 1999hrrl.conf..240F
  We discuss BIMA (Berkeley Illinois Maryland Association) data and
  present new h igh quality optical and near-IR Keck images of the
  bright radio ring PKS 1830-211. Applying a powerful new deconvolution
  algorithm we have been able to identify both images of the radio
  source. In addition we recover an extended source in the optical,
  consistent with the expected location of the lensing galaxy. The source
  counterparts are very red, I-K ~7 suggesting strong Galactic absorption
  with additional absorption by the lensing galaxy at z = 0.885, and
  consistent with the detection of high redshift molecules in the lens.

Title: Abundance correlations in mildly metal-poor stars
Authors: Jehin, E.; Magain, P.; Neuforge, C.; Noels, A.; Parmentier,
   G.; Thoul, A. A.
Bibcode: 1999A&A...341..241J
Altcode: 1998astro.ph..9405J
  Accurate relative abundances have been obtained for a sample of 21
  mildly metal-poor stars from the analysis of high resolution and
  high signal-to-noise spectra. In order to reach the highest coherence
  and internal precision, lines with similar dependency on the stellar
  atmospheric parameters were selected, and the analysis was carried out
  in a strictly differential way within the sample. With these accurate
  results, correlations between relative abundances have been searched
  for, with a special emphasis on the neutron capture elements. This
  analysis shows that the r elements are closely correlated to the
  alpha elements, which is in agreement with the generally accepted
  idea that the r-process takes place during the explosion of massive
  stars. The situation is more complex as far as the s elements are
  concerned. Their relation with the alpha elements is not linear. In a
  first group of stars, the relative abundance of the s elements increases
  only slightly with the alpha elements overabundance until the latter
  reaches a maximum value. For the second group, the s elements show a
  rather large range of enhancement and a constant (and maximum) value
  of the alpha elements overabundance. This peculiar behaviour leads
  us to distinguish between two sub-populations of metal-poor stars,
  namely Pop IIa (first group) and Pop IIb (second group). We suggest
  a scenario of formation of metal-poor stars based on two distinct
  phases of chemical enrichment, a first phase essentially consisting
  in supernova explosions of massive stars, and a second phase where
  the enrichment is provided by stellar winds from intermediate mass
  stars. More specifically, we assume that all thick disk and field
  halo stars were born in globular clusters, from which they escaped,
  either during an early disruption of the cluster (Pop IIa) or, later,
  through an evaporation process (Pop IIb). Based on observations obtained
  at the European Southern Observatory, La Silla, Chile.

Title: Image deconvolution of lensed QSOs observed with the NOT:
    Competing with the HST (poster)
Authors: Burud, I.; Courbin, F.; Magain, P.
Bibcode: 1999anot.conf..105B
Altcode:
  No abstract at ADS

Title: Linking Field Metal-Poor Stars and Globular Clusters: The
    Ease Scenario
Authors: Jehin, E.; Magain, P.; Neuforge, C.; Noels, A.; Parmentier,
   G.; Thoul, A.
Bibcode: 1999gecd.conf..287J
Altcode:
  No abstract at ADS

Title: Deep imaging of AXJ2019+112: The luminosity of a ``Dark
    Cluster''
Authors: Benitez, N.; Broadhurst, T.; Rosati, P.; Courbin, F.; Squires,
   G.; Lidman, C.; Magain, P.
Bibcode: 1998tx19.confE.504B
Altcode:
  We detect a distant cluster of galaxies at z ~1 centered on
  the QSO lens and luminous X-ray source AXJ2019+112 (Hattori et
  al 1997). The mass-to-light ratio within an aperture of 0.4 h
  ^{-1}Mpc determined using the X-ray temperature is M_x / L_V =
  190^{+95}_{-66}h(M/L_V)<SUB>sun</SUB>. The strong lens model yields
  a compatible value, M/L_V = 315^{+80}_{-80}h(M/L_V)<SUB>sun</SUB>,
  whereas an independent weak lensing analysis sets an upper limit of
  M/L_V &lt; 440 h(M/L_V)<SUB>sun</SUB>. This confirms that AXJ2019+112
  has a M/L ratio similar to that of z &lt; 1 massive clusters.

Title: Three photometric methods tested on ground-based data of
    Q 2237+0305
Authors: Burud, I.; Stabell, R.; Magain, P.; Courbin, F.; Ostensen,
   R.; Refsdal, S.; Remy, M.; Teuber, J.
Bibcode: 1998A&A...339..701B
Altcode: 1998astro.ph..9107B
  The Einstein Cross, Q 2237+0305, has been photometrically observed in
  four bands on two successive nights at NOT (La Palma, Spain) in October
  1995. Three independent algorithms have been used to analyse the data:
  an automatic image decomposition technique, a CLEAN algorithm and the
  new MCS deconvolution code. The photometric and astrometric results
  obtained with the three methods are presented. No photometric variations
  were found in the four quasar images. Comparison of the photometry from
  the three techniques shows that both systematic and random errors affect
  each method. When the seeing is worse than 1farcs0 , the errors from the
  automatic image decomposition technique and the Clean algorithm tend to
  be large (0.04-0.1 magnitudes) while the deconvolution code still gives
  accurate results (1sigma error below 0.04) even for frames with seeing
  as bad as 1farcs7 . Reddening is observed in the quasar images and is
  found to be compatible with either extinction from the lensing galaxy or
  colour dependent microlensing. The photometric accuracy depends on the
  light distribution used to model the lensing galaxy. In particular,
  using a numerical galaxy model, as done with the MCS algorithm,
  makes the method less seeing dependent. Another advantage of using
  a numerical model is that eventual non-homogeneous structures in the
  galaxy can be modeled. Finally, we propose an observational strategy
  for a future photometric monitoring of the Einstein Cross. Based on
  observations obtained at NOT, La Palma.

Title: High-Resolution Optical and Near-Infrared Imaging of the
    Quadruple Quasar RX J0911.4+0551
Authors: Burud, I.; Courbin, F.; Lidman, C.; Jaunsen, A. O.; Hjorth,
   J.; Østensen, R.; Andersen, M. I.; Clasen, J. W.; Wucknitz, O.;
   Meylan, G.; Magain, P.; Stabell, R.; Refsdal, S.
Bibcode: 1998ApJ...501L...5B
Altcode: 1998astro.ph..3175B
  We report the detection of four images in the recently discovered
  lensed QSO RX J0911.4+0551. With a maximum angular separation of
  3.1", it is the quadruply imaged QSO with the widest known angular
  separation. Raw and deconvolved data reveal an elongated lens
  galaxy. The observed reddening in at least two of the four QSO images
  suggests differential extinction by this lensing galaxy. We show that
  both an ellipticity of the galaxy (ɛ<SUB>min</SUB>=0.075) and an
  external shear (γ<SUB>min</SUB>=0.15) from a nearby mass have to be
  included in the lensing potential in order to reproduce the complex
  geometry observed in RX J0911.4+0551. A possible galaxy cluster is
  detected about 38" from RX J0911.4+0551 and could contribute to the
  X-ray emission observed by ROSAT in this field. The color of these
  galaxies indicates a plausible redshift in the range of 0.6-0.8. <P
  />Based on observations obtained at NOT and ESO La Silla.

Title: Image Deconvolution of the Radio Ring PKS 1830-211
Authors: Courbin, F.; Lidman, C.; Frye, B. L.; Magain, P.; Broadhurst,
   T. J.; Pahre, M. A.; Djorgovski, S. G.
Bibcode: 1998ApJ...499L.119C
Altcode: 1998astro.ph..2156C
  New high-quality Keck and ESO images of PKS 1830-211 are presented. By
  applying a powerful new deconvolution algorithm to these optical and
  infrared data, both images of the flat spectrum core of the radio
  source have been identified. An extended source is also detected in
  the optical images which is consistent with the expected location of
  the lensing galaxy. The source counterparts are very red at I-K~7,
  which suggests strong Galactic absorption with additional absorption
  by the lensing galaxy at z=0.885 and is consistent with the detection
  of high-redshift molecules in the lens. <P />Based on observations
  obtained at the ESO La Silla Observatory, Chile and at the W. M. Keck
  Observatory, Hawaii, which is operated jointly by the California
  Institute of Technology and the University of California.

Title: RX J0911.4+0551: a complex quadruply imaged gravitationally
    lensed QSO.
Authors: Burud, I.; Courbin, F.; Lidman, C.; Meylan, G.; Magain, P.;
   Jaunsen, A. O.; Hjorth, J.; Østensen, R.; Andersen, M. I.; Clasen,
   J. W.; Stabell, R.; Refsdal, S.
Bibcode: 1998Msngr..92...29B
Altcode:
  The authors present their first observations of RX J0911.4+0551 at
  the 2.2-m ESO/MPI IRAC 2b in K-band which made them suspect that the
  QSO might be quadruple. This was confirmed on the optical data from
  the 2.56-m Nordic Optical Telescope, and on the NTT/SOFI data of the
  object. Careful deconvolution of the data allows to clearly resolve
  the object into four QSO components and a lensing galaxy.

Title: Deconvolution with Correct Sampling
Authors: Magain, P.; Courbin, F.; Sohy, S.
Bibcode: 1998ApJ...494..472M
Altcode: 1997astro.ph..4059M
  A new method for improving the resolution of astronomical images
  is presented. It is based on the principle that sampled data cannot
  be fully deconvolved without violating the sampling theorem. Thus,
  the sampled image should be deconvolved not by the total point-spread
  function but by a narrower function chosen so that the resolution of
  the deconvolved image is compatible with the adopted sampling. <P />Our
  deconvolution method gives results that are, in at least some cases,
  superior to those of other commonly used techniques: in particular, it
  does not produce ringing around point sources superposed on a smooth
  background. Moreover, it allows researchers to perform accurate
  astrometry and photometry of crowded fields. These improvements
  are a consequence of both the correct treatment of sampling and the
  recognition that the most probable astronomical image is not a flat
  one. <P />The method is also well adapted to the optimal combination
  of different images of the same object, as can be obtained, e.g.,
  from infrared observations or via adaptive optics techniques.

Title: Heavy elements abundances in metal-poor stars
Authors: Magain, P.; Jehin, E.; Neuforge, C.; Noels, A.
Bibcode: 1998AIPC..425..592M
Altcode:
  A sample of 21 metal-poor stars have been analysed on the basis
  of high resolution and high signal-to-noise spectra. Correlations
  between relative abundances of 16 elements have been studied, with a
  special emphasis on the neutron-capture ones. This analysis reveals the
  existence of two sub-populations of field halo stars, namely Pop IIa and
  Pop IIb. They differ by the behaviour of the s-process elements versus
  the α and r-process elements. We suggest a scenario of formation of
  these stars, which closely relates the field halo stars to the evolution
  of globular clusters. The two sub-populations would have evaporated
  the clusters during two different stages of their chemical evolution.

Title: Detection of the lensing galaxy in HE 1104-1805
Authors: Courbin, F.; Lidman, C.; Magain, P.
Bibcode: 1998A&A...330...57C
Altcode: 1997astro.ph..7183C
  We report on deep IR imaging of the double quasar HE 1104-1805. A new
  image deconvolution technique has been applied to the data in order to
  optimally combine the numerous frames obtained. The resulting J and K'
  images allow us to detect and study the lensing galaxy between the two
  lensed QSO images. The near infrared images not only confirm the lensed
  nature of this double quasar, but also support the previous redshift
  estimate of z=1.66 for the lensing galaxy. No obvious overdensity of
  galaxies is detected in the immediate region surrounding the lens, down
  to limiting magnitudes of J=22 and K=20. The geometry of the system,
  together with the time delays expected for this lensed quasar, make
  HE 1104-1805 a remarkable target for future photometric monitoring
  programs, for the study of microlensing and for the determination of
  the cosmological parameters in the IR and optical domains. Based on
  observations obtained at ESO, La Silla, Chile

Title: Field halo stars: the globular cluster connection
Authors: Jehin, E.; Magain, P.; Neuforge, C.; Noels, A.; Thoul, A. A.
Bibcode: 1998A&A...330L..33J
Altcode:
  High resolution and high signal-to-noise spectra of about 20 metal-poor
  stars have been analysed. The correlations between the relative
  abundances of 16 elements have been studied, with a special emphasis on
  the neutron-capture ones. This analysis reveals the existence of two
  subpopulations of field halo stars, namely Pop IIa and Pop IIb. They
  differ by the behaviour of the s-process elements versus the alpha
  and r-process elements. A scenario for the formation of these stars
  is presented, which closely relates the origin of field halo stars
  to the evolution of globular clusters. According to this scenario,
  the two sub-populations originate from two different stages in the
  globular cluster's chemical evolution. Based on observations carried
  out at the European Southern Observatory (La Silla, Chile)

Title: The impact of AGB stars on the chemical evolution of globular
    clusters
Authors: Jehin, E.; Magain, P.; Neuforge, C.; Noels, A.; Parmentier,
   G.; Thoul, A. A.
Bibcode: 1998IAUS..191P.603J
Altcode:
  We have analyzed high resolution and high signal-to-noise spectra
  of about 20 metal-poor stars. The correlations between the relative
  abundances of 16 elements have been studied, with a special emphasis on
  the neutron-capture ones. This analysis reveals the existence of two
  sub-populations of field halo stars, namely Pop IIa and Pop IIb. They
  differ by the behaviour of the s-process elements versus the alpha
  and r-process elements. We present a scenario for the formation of
  these stars, which closely relates the origin of field halo stars
  to the evolution of globular clusters. According to this scenario,
  the two sub-populations originate from two different stages in the
  globular cluster's chemical evolution. In the first stage, the massive
  stars of the globular cluster's first stellar generation evolve,
  ending their lives as supernovae and ejecting alpha-elements and
  r-process elements into the interstellar medium. A second generation
  of stars forms out of this enriched ISM. In the second stage, the
  intermediate mass stars reach the end of the main sequence and the
  AGB stage, ejecting s-elements into the ISM through stellar winds or
  superwinds events. The matter released in the ISM by the AGB stars
  will be accreted by the lower-mass stars, enriching those stars in
  s-elements and accounting for PopIIb stars. We calculate the rates
  of interstellar gas production by stellar winds and the rates of
  gas accretion to estimate the changes in the globular cluster stars
  abundances. We compare those results to our observations.

Title: ESO &amp; NOT photometric monitoring of the Cloverleaf quasar
Authors: Ostensen, R.; Remy, M.; Lindblad, P. O.; Refsdal, S.; Stabell,
   R.; Surdej, J.; Barthel, P. D.; Emanuelsen, P. I.; Festin, L.; Gosset,
   E.; Hainaut, O.; Hakala, P.; Hjelm, M.; Hjorth, J.; Hutsemekers, D.;
   Jablonski, M.; Kaas, A. A.; Kristen, H.; Larsson, S.; Magain, P.;
   Pettersson, B.; Pospieszalska-Surdej, A.; Smette, A.; Teuber, J.;
   Thomsen, B.; van Drom, E.
Bibcode: 1997A&AS..126..393O
Altcode:
  The Cloverleaf quasar, H1413+117, has been photometrically monitored
  at ESO (La Silla, Chile) and with the NOT (La Palma, Spain) during the
  period 1987--1994. All good quality CCD frames have been successfully
  analysed using two independent methods (i.e. an automatic image
  decomposition technique and an interactive CLEAN algorithm). The
  photometric results from the two methods are found to be very similar,
  and they show that the four lensed QSO images vary significantly in
  brightness (by up to 0.45 mag), nearly in parallel. The lightcurve of
  the $D$ component presents some slight departures from the general trend
  which are very likely caused by micro-lensing effects. Upper limits,
  at the 99% confidence level, of 150 days on the absolute value for the
  time delays between the photometric lightcurves of this quadruply imaged
  variable QSO, are derived. This is unfortunately too large to constrain
  the lens model but there is little doubt that a better sampling of the
  lightcurves should allow to accurately derive these time delays. Pending
  a direct detection of the lensing galaxy (position and redshift),
  this system thus constitutes another good candidate for a direct and
  independent determination of the Hubble parameter. Based on observations
  collected at the European Southern Observatory (La Silla, Chile) and
  with the Nordic Optical Telescope (La Palma, Spain). Table 1. Logbook
  for the ESO and NOT observations together with photometric results for
  the Cloverleaf quasar. This long table can be accessed on the WWW at the
  URL address: http://vela.astro.ulg.ac.be/grav_lens/glp_homepage.html}

Title: Spectroscopic analysis of the Alpha Centauri system
Authors: Neuforge-Verheecke, C.; Magain, P.
Bibcode: 1997A&A...328..261N
Altcode:
  A detailed spectroscopic analysis of the two components of the binary
  system alpha Centauri has been carried out on the basis of extensive
  high resolution and high signal-to-noise spectra. The temperatures of
  the stars have been determined from the Fei excitation equilibrium and
  checked from the H_α line wings. The abundances of 17 elements have
  been obtained and indicate a general overabundance of 0.24 dex relative
  to the Sun, with no significant difference between the two stars. All
  elements analysed, from CNO to the iron peak, show basically the same
  overabundance. Only nickel seems to be significantly more overabundant,
  while the neutron capture elements appear less enhanced. Based on
  observations carried out at the European Southern Observatory (La
  Silla, Chile)

Title: The LMC transition star R 84 and the core of the LH 39 OB
    association.
Authors: Heydari-Malayeri, M.; Courbin, F.; Rauw, G.; Esslinger, O.;
   Magain, P.
Bibcode: 1997A&A...326..143H
Altcode: 1997astro.ph..6052H
  On the basis of sub-arcsecond imaging obtained at the ESO NTT with
  SUSI and the ESO ADONIS adaptive optics system at the 3.6m telescope,
  we resolve and study the core components of the LMC OB association LH
  39. The central star of the association, the rare transition object
  R 84, is also investigated using CASPEC echelle spectroscopy at
  the ESO 3.6m telescope. A new, powerful image restoration code that
  conserves the fluxes allows us to obtain the magnitudes and colors of
  the components. We bring out some 30 stars in a ~16"x16" area centered
  on R 84. At a resolution of 0.19"(FWHM), the closest components to R 84
  are shown to be stars #21 and #7 lying at 1.1"NW and 1.7"NW respectively
  of the transition star. The former is possibly a blue star of V=16.7mag
  and the latter with its V=17.5mag is the reddest star of the field,
  after R 84. Star #7 turns out to be too faint to correspond to the
  red M2 supergiant previously reported to contaminate the spectrum of
  R 84. If the late-type spectrum is due to a line-of-sight supergiant
  with a luminosity comparable to R 84, it should lie closer than 0.12"
  to R 84. The transition star shows spectral variability between 1982
  and 1991. We also note some slight radial velocity variations of the Of
  emission lines over timescales of several years. Furthermore, we derive
  the spectral types of two of the brightest stars of the cluster, using
  long slit spectra obtained at the NTT telescope equipped with EMMI,
  and discuss the apparent absence of O type stars in this association.

Title: The geometry of the quadruply imaged quasar PG 1115+080:
    implications for H_0_.
Authors: Courbin, F.; Magain, P.; Keeton, C. R.; Kochanek, C. S.;
   Vanderriest, C.; Jaunsen, A. O.; Hjorth, J.
Bibcode: 1997A&A...324L...1C
Altcode: 1997astro.ph..5093C
  Time delay measurements have recently been reported for the lensed
  quasar PG 1115+080. These measurements can be used to derive H_0_,
  but only if we can constrain the lensing potential. We have applied a
  recently developed deconvolution technique to analyze sub-arcsecond I
  band images of PG 1115+080, obtained at the Nordic Optical Telescope
  (NOT) and the Canada France Hawaii Telescope (CFHT). The high
  performance of the deconvolution code allows us to derive precise
  positions and magnitudes for the four lensed images of the quasar,
  as well as for the lensing galaxy. The new measurement of the galaxy
  position improves its precision by a factor of 3 and thus strengthens
  the constraints on the lensing potential. With the new data, a range
  of models incorporating some of the plausible systematic uncertainties
  yields H_0_=53^+10^_-7_km/s/Mpc.

Title: VizieR Online Data Catalog: Spectroscopy of Alpha Cen
    (Neuforge-Verheecke+ 1997)
Authors: Neuforge-Verheecke, C.; Magain, P.
Bibcode: 1997yCat..33280261N
Altcode:
  This table presents the results of a spectroscopic analysis
  (differentially to the Sun) of the two components of the binary system
  Alpha Centauri. This analysis has been carried out on the basis of
  extensive high resolution and high signal-to-noise spectra taken at
  the European Southern Observatory (La Silla, Chile). (1 data file).

Title: Deconvolution with correct sampling.
Authors: Magain, P.; Courbin, F.; Sohy, S.
Bibcode: 1997Msngr..88...28M
Altcode:
  The authors briefly describe the basic ideas behind a new deconvolution
  technique which overcomes some of the drawbacks of the traditional
  methods and which gives results of high photometric and astrometric
  accuracy. The authors also show how it can be combined with other
  techniques (e.g. adaptive optics) to give even better results.

Title: Sub-arcsecond imaging and spectroscopy of the radio-loud
    highly polarized quasar PKS 1610-771.
Authors: Courbin, F.; Hutsemekers, D.; Meylan, G.; Magain, P.;
   Djorgovski, S. G.
Bibcode: 1997A&A...317..656C
Altcode: 1996astro.ph..6114C
  We report on imaging and spectroscopic observations of the radio-loud,
  highly polarized quasar PKS 1610-771 (z=1.71). Our long-slit
  spectroscopy of the companion 4.55" NW of the quasar confirms the
  stellar nature of this object, so ruling out the previously suspected
  gravitationally lensed nature of this system. PKS 1610-771 looks
  fuzzy on our sub-arcsecond R and I images and appears located in a
  rich environment of faint galaxies. Possible magnification, without
  image splitting of the quasar itself, by some of these maybe foreground
  galaxies cannot be excluded. The continuum fuzz (made of the closest
  two objects, viz. A and D) is elongated in a direction orthogonal
  to the E vector of the optical polarization, as in high-redshift
  radio-galaxies. The spectrum of PKS 1610-771 appears strongly curved,
  in a convex way, with a maximum of intensity at ~7,600Å (2,800AÅ rest
  frame), possibly indicating a strong ultraviolet absorption by dust.

Title: PKS 1610-771: a highly reddened quasar?
Authors: Courbin, F.; Hutsemékers, D.; Meylan, G.; Magain, P.;
   Djorgovski, S. G.
Bibcode: 1996Msngr..85...27C
Altcode:
  No abstract at ADS

Title: WR22: the most massive Wolf-Rayet star ever weighed.
Authors: Rauw, G.; Vreux, J. -M.; Gosset, E.; Hutsemekers, D.; Magain,
   P.; Rochowicz, K.
Bibcode: 1996A&A...306..771R
Altcode:
  The results of an extensive spectroscopic campaign on the eclipsing
  binary WR22 are presented. A new radial velocity curve is deduced for
  the WN7 component, allowing us to improve the parameters of the orbit,
  formerly determined on the basis of photographic spectra. The high
  signal-to-noise ratio of our data also allows the detection of some weak
  absorption lines which, for the first time, can definitely be attributed
  to the companion. A study of their radial velocities gives a mass ratio
  of m_WR_/m_O_=2.78 leading to a minimum mass of 72M<SUB>sun</SUB>_ for
  the WN7 star. The companion can be classified as a "late O" (O6.5-O8.5)
  star with a luminosity ratio of the system q=L_WR_^y^/L_O_^y^ at 5500A
  of about 8. The exceptionally high mass of the WN7 star and its high
  hydrogen mass-fraction suggest that WR22 is at the beginning of its
  Wolf-Rayet evolution. As a matter of fact, with such a high mass, WR22
  most probably is still a hydrogen burning object. Therefore, the WN7
  component is much closer to a main sequence O star with a "Wolf-Rayet
  clothing" than to the other members of the Wolf-Rayet family, which
  are rather highly evolved He-burning descendants of massive progenitors.

Title: Chemical composition of solar-type stars
Authors: Neuforge, C.; Magain, P.
Bibcode: 1996ASPC..109..695N
Altcode: 1996csss....9..695N
  No abstract at ADS

Title: Empirical study of departures from the excitation equilibrium
    of FeI in metal-poor stars.
Authors: Magain, P.; Zhao, G.
Bibcode: 1996A&A...305..245M
Altcode:
  A detailed analysis of neutral iron lines in a sample of 13 metal-poor
  dwarfs and subgiants is carried out on the basis of high resolution
  spectra obtained with the ESO Coude Echelle Spectrometer. The deduced
  iron abundance is found to depend on the excitation potential
  of the line used, higher excitation lines generally indicating
  higher abundances. This could be caused by departures from the local
  thermodynamic equilibrium (LTE) or by temperature inhomogeneities in
  the stellar atmospheres. The dependency of this effect on the stellar
  atmospheric parameters is investigated. From the comparison of iron
  lines with lines of other elements, it is concluded that the low
  excitation FeI lines are much more affected than the high excitation
  lines. The consequences of these effects for the classical abundance
  analyses are examined. It is found that they may explain, at least in
  part, some previously reported discrepancies between the results of
  different authors.

Title: Photometric monitoring (1987 to 1994) of the gravitational
    lens candidate UM 425.
Authors: Courbin, F.; Magain, P.; Remy, M.; Smette, A.; Claeskens,
   J. F.; Hainaut, O.; Hutsemekers, D.; Meylan, G.; van Drom, E.
Bibcode: 1995A&A...303....1C
Altcode: 1995astro.ph..4053C
  We present the results of a 7 year long photometric monitoring of two
  components (A and B) of UM 425, thought to be images, separated by 6.5",
  of the same z=1.47 quasar. These components have been imaged through
  an R filter in order to obtain their light curves. The photometry was
  obtained by simultaneously fitting a stellar two-dimensional profile
  on each component. The brightest image (component A, m_R_=15.7) shows a
  slow and smooth increase in brightness of 0.2 magnitude in seven years,
  while the faintest one (component B, m_R_=20.1) displays an outburst
  of 0.4 magnitude which lasts approximately two years. The variation
  of component B may be interpreted in two ways, assuming UM 425 is
  gravitationally lensed. If it is due to an intrinsic variation of
  the quasar, we derive a lower limit of 3 years on the time delay from
  the fact that it is not observed in component A. On the other hand,
  if it is a microlensing "High Amplification Event", we estimate the
  size of the source to be ~10^-3^pc, in agreement with standard models
  of AGNs. These observations are consistent with the gravitational lens
  interpretation of the object. Furthermore, all the CCD frames obtained
  under the best seeing conditions have been co-added, in an attempt to
  detect the deflector. The final R image reveals a rich field of faint
  galaxies in the magnitude range m_R_~22-24. No obvious deflector,
  nor any system of arcs or arclets is detected, down to a limiting
  magnitude of m_R_~24.

Title: VizieR Online Data Catalog: Fe I in metal-poor stars (Magain+,
    1996)
Authors: Magain, P.; Zhao, G.
Bibcode: 1995yCat..33050245M
Altcode:
  A detailed analysis of neutral iron lines in a sample of 13 metal-poor
  dwarfs and subgiants is carried out on the basis of high resolution
  spectra obtained with the ESO Coude Echelle Spectrometer. The deduced
  iron abundance is found to depend on the excitation potential
  of the line used, higher excitation lines generally indicating
  higher abundances. This could be caused by departures from the local
  thermodynamic equilibrium (LTE) or by temperature inhomogeneities in
  the stellar atmospheres. The dependency of this effect on the stellar
  atmospheric parameters is investigated. From the comparison of iron
  lines with lines of other elements, it is concluded that the low
  excitation Fe I lines are much more affected than the high excitation
  lines. The consequences of these effects for the classical abundance
  analyses are examined. It is found that they may explain, at least in
  part, some previously reported discrepancies between the results of
  different authors. (1 data file).

Title: Heavy elements in halo stars: the r/s-process controversy.
Authors: Magain, P.
Bibcode: 1995A&A...297..686M
Altcode:
  It has been suggested by Truran (1981) that rapid neutron captures
  (the r-process) dominate the production of heavy elements in very
  metal-poor stars. Several spectroscopic works analyzing that hypothesis
  are reviewed and rediscussed and it is shown that there is, in fact,
  no secure observational evidence in support of Truran's suggestion. A
  method to determine the odd-to-even isotopic ratio of barium, and thus
  to estimate the relative contributions of the r and s-processes, is
  presented. It takes advantage of the hyperfine structure affecting the
  spectral lines of the odd isotopes to distinguish them from the even
  isotopes. This method, applied to the classical metal-poor subgiant
  HD 140283, shows that the barium isotopic ratio in that star is in
  agreement with a pure s-process production, and excludes any significant
  enhancement of the r-process contribution, in disagreement with previous
  works based on elemental abundances.

Title: Stellar Atmospheres : The Link between Theory and Observation
Authors: Magain, P.
Bibcode: 1995LIACo..32..139M
Altcode: 1995sews.book..139M
  No abstract at ADS

Title: Barium Abundances of 20 Metal Deficient Stars
Authors: Zhao, G.; Magain, P.
Bibcode: 1995ASPC...81..574Z
Altcode: 1995lahr.conf..574Z
  No abstract at ADS

Title: A seven year campaign on WR 22
Authors: Rauw, G.; Vreux, J. -M.; Gosset, E.; Hutsemekers, D.; Magain,
   P.; Manfroid, J.; Remy, M.; Rochowicz, K.
Bibcode: 1995IAUS..163..241R
Altcode:
  No abstract at ADS

Title: Vhrs - the Very High Resolution Spectrograph for the VLT
Authors: Magain, P.; Dekker, H.; Delabre, B.
Bibcode: 1995ESOSR..15....1M
Altcode:
  No abstract at ADS

Title: Elemental and Isotopic Abundances in Metal-Poor Stars
Authors: Magain, P.
Bibcode: 1995svlt.conf...79M
Altcode:
  No abstract at ADS

Title: WR22 as a core hydrogen-burning Wolf-Rayet star
Authors: Rauw, G.; Vreux, J. M.; Gosset, E.; Hutsemekers, D.;
   Magain, P.
Bibcode: 1995LIACo..32..463R
Altcode: 1995sews.book..463R
  The analysis of an extensive sample of high resolution spectra of
  the Wolf-Rayet binary WR22 recently allowed us to determine a minimum
  mass of 72 M_solar for the WN7 star. With such a high mass, WR22 is
  expected to be a core H-Burning star which has just evolved from a
  progenitor of at least 90-110 M_solar.

Title: VHRS: the Very High Resolution Spectrograph for the VLT.
Authors: Magain, P.; Dekker, H.; Delabre, B.
Bibcode: 1994fvlt.conf...37M
Altcode:
  No abstract at ADS

Title: (Erratum) Further observational evidence that MG J0414+0534
    is a gravitational mirage.
Authors: Angonin-Willaime, M. -C.; Vanderriest, C.; Hammer, F.;
   Magain, P.
Bibcode: 1994A&A...292..722A
Altcode:
  In Sect. 3.3, the identifications of components A1 and A2 for
  the optical data were inadvertently inverted. This does not change
  substantially the discussion; just read A1 for A2 and vice versa. In
  particular, the ratio A2/A1 = 0.3 cannot be made compatible with the
  radio value without one or several of the mechanisms we suggested. We
  apologize for the error and thank Dr S. Mao for bringing it to our
  attention. Erratum to Astron. Astrophys. 281, 388-394 (1994)

Title: Further observational evidence that MG J0414+0534 is a
    gravitational mirage.
Authors: Angonin-Willaime, M. -C.; Vanderriest, C.; Hammer, F.;
   Magain, P.
Bibcode: 1994A&A...281..388A
Altcode:
  Deep imaging of MG J0414+0534 with R and I filters reveals a faint,
  fuzzy and red object at the exact location expected for a lensing
  galaxy in the gravitational mirage hypothesis. Furthermore, the
  (extremely red and almost featureless) spectra of the 2 brightest
  components are very similar. These are strong indications that
  the system results from multiple gravitational imaging of a single
  source, but the nature of this source is not yet clear. It could
  be the nucleus of a low metallicity galaxy at a high redshift or a
  new type of object. Significant differences are observed between the
  flux ratios of the images at radio and optical wavelengths. The most
  likely explanation for this effect is a differential amplification of
  the image pair A_1_-A_2_ because of the large magnification gradient
  near a caustic.

Title: On the linearity of ESO CCD#9 at CAT+CES.
Authors: Gosset, E.; Magain, P.
Bibcode: 1993Msngr..73...13G
Altcode:
  No abstract at ADS

Title: Gravitational Lensing Statistics Based on a Large Sample of
    Highly Luminous Quasars
Authors: Surdej, J.; Claeskens, J. F.; Crampton, D.; Filippenko,
   A. V.; Hutsemekers, D.; Magain, P.; Pirenne, B.; Vanderriest, C.;
   Yee, H. K. C.
Bibcode: 1993AJ....105.2064S
Altcode:
  Results on gravitational lensing statistics applied to a sample of 469
  highly luminous quasars are reported. The objects were directly imaged,
  either from the ground (ESO, CFH) under optimal seeing conditions,
  or using the Hubble Space Telescope. We have derived values for the
  effectiveness parameter F of galaxies, modeled by means of singular
  isothermal spheres, to produce macrolensed images of distant quasars,
  and upper limits on the density parameter {OMEGA}_L_ of compact objects
  with masses ~10^10^ - 10^12^ M_sun_. Adopting H_0_ = 50 km/s/Mpc,
  {OMEGA}_0_= 1 and λ = 0, we find that at the 99.7% confidence level,
  0.005 &lt; F &lt; 0.478 and that {OMEGA}_L_ &lt; 0.02. A critical
  discussion of these results is presented. Finally, comparing the
  efficiencies of ground-based and space instruments used to search for
  gravitational lens systems among highly luminous quasars, we conclude
  that for the near future, ground based direct imaging characterized by a
  good dynamical range still constitutes the best observational strategy.

Title: Erratum - Q:1208+1011 - the Most Distant Multiply Imaged
    Quasar or a Binary
Authors: Magain, P.; Surdej, J.; Vanderriest, C.; Pirenne, B.;
   Hutsemekers, D.
Bibcode: 1993A&A...272..383M
Altcode:
  In the title of this Letter, the word "multiply" was accidentally
  omitted. The correct title is shown above.

Title: Barium isotopes in the very metal-poor star HD 140283.
Authors: Magain, P.; Zhao, G.
Bibcode: 1993A&A...268L..27M
Altcode:
  The fractions of odd and even isotopes of barium in the metal-poor
  star HD140283 are determined from an analysis of the profile of the
  Ba II resonance line, taking advantage of the differences in hyperfine
  structure splitting between the different isotopes. Although one would
  expect an increased contribution of the r-process in very metal-poor
  stars, it is found that the isotopic ratio is very close to solar.

Title: Search for gravitational lenses in a large sample of highly
    luminous quasars and statistical determination of cosmological
    parameters
Authors: Claeskens, J. F.; Crampton, D.; Filippenko, A. V.;
   Hutsemekers, D.; Magain, P.; Pirenne, B.; Surdej, J.; Vanderriest,
   C.; Yee, H. K. C.
Bibcode: 1993LIACo..31..263C
Altcode: 1993glu..conf..263C
  Results on gravitational lensing statistics applied to a sample of
  469 highly luminous quasars are reported.

Title: Barium isotopes in metal-poor stars.
Authors: Magain, P.; Zhao, G.
Bibcode: 1993oee..conf..480M
Altcode:
  No abstract at ADS

Title: Coincidences
Authors: Magain, P.; Remy, M.
Bibcode: 1993LIACo..31..137M
Altcode: 1993glu..conf..137M
  No abstract at ADS

Title: Two new very close pairs of quasars with discordant redshifts
    and a gravitational lens candidate.
Authors: Surdej, J.; Remy, M.; Smette, A.; Claeskens, J. -F.; Magain,
   P.; Refsdal, S.; Swings, J. -P.; Veron-Cetty, M.
Bibcode: 1993Lie93..31..153S
Altcode:
  No abstract at ADS

Title: The cloverleaf quasar H1413+117: a preliminary light curve
Authors: Arnould, P.; Remy, M.; Gosset, E.; Hainaut, O.; Hutsemekers,
   D.; Magain, P.; Smette, A.; Surdej, J.; van Drom, E.
Bibcode: 1993LIACo..31..169A
Altcode: 1993glu..conf..169A
  The cloverleaf quasar H1413+117 was discovered to be a gravitational
  lens system in 1988. Since then, it has been photometrically monitored
  essentially as part of the ESO key-program Gravitational lensing: we
  present here a first preliminary lightcurve for its four individual
  images.

Title: Galaxies statistics around highly luminous quasars: the
    ESO Sample
Authors: van Drom, E.; Surdej, J.; Magain, P.; Hutsemekers, D.;
   Gosset, E.; Claeskens, J. F.; Shaver, P.; Melnick, J.
Bibcode: 1993LIACo..31..301V
Altcode: 1993glu..conf..301V
  We present observational evidence on the correlation between the
  positions of Highly Luminous Quasars and those of galaxies for a sample
  of 136 objects, observed under good seeing conditions.

Title: The relative photometric lightcurve of UM673 A&amp;B
Authors: Daulie, G.; Hainaut, O.; Hutsemekers, D.; Magain, P.; Remy,
   M.; Smette, A.; Surdej, J.; van Drom, E.
Bibcode: 1993LIACo..31..181D
Altcode: 1993glu..conf..181D
  From 1987 to 1993, we have carried out at ESO a photometric monitoring
  of the gravitationally lensed quasar UM673. The main result is that
  the two lensed images of UM673 did not show any significant relative
  variation during more than five years.

Title: ESO key programme, gravitational lensing: quasars and radio
    galaxies; a status report
Authors: Surdej, J.; Angonin, M. C.; Arnaud, J.; Bauer, T.; Borgeest,
   U.; Hainaut, O.; Hammer, F.; Hutsemekers, D.; Le Fevre, O.; Nottale,
   L.; Magain, P.; Meylan, G.; Remy, M.; Shaver, P.; Smette, A.; Swings,
   J. P.; van Drom, E.; Veron-Cetty, M.; Veron, P.
Bibcode: 1992daec.conf...97S
Altcode:
  The scientific background and objectives of our ESO Key Programme are
  first recalled. A brief account of our research activities (observing
  runs at ESO and elsewhere, meetings, etc.) is then given. Preliminary
  scientific results are presented concerning 1) our observational
  database for highly luminous quasars and distant powerful radiogalaxies;
  2) speckle observations of highly luminous quasars; 3) the photometric
  monitoring and 4) detailed studies of several known gravitational
  lenses; 5) optical observations of 3C and 4C radio galaxies and 6)
  of the well known Einstein ring MG 1131+0456.

Title: A Spectroscopic Study of UM 673 A and B: On the Size of
    Lyman-Alpha Clouds
Authors: Smette, A.; Surdej, J.; Shaver, P. A.; Foltz, C. B.; Chaffee,
   F. H.; Weymann, R. J.; Williams, R. E.; Magain, P.
Bibcode: 1992ApJ...389...39S
Altcode:
  We present a study of the Lyα forest spectra (2 A resolution) obtained
  for the A and B images of the gravitationally lensed high- redshift
  quasar UM 673. We also present higher resolution data of the brightest
  (A) image. In the 2 A resolution spectra, all the absorption lines
  detected at 5 σ in the spectrum of the fainter B image are present in
  the A image; however, we find two anticoincidences, i.e., two lines in
  A which do not have a counterpart in B at more than a 3 σ confidence
  level. Given the fact that corresponding Lyα lines in the spectra of
  A and B have their equivalent widths well correlated, this proves that
  both light beams actually cross the same clouds. Most of the velocity
  differences between corresponding lines are compatible with 0 km s^-1^
  within the error bars, with a standard deviation of 17 km s^-1^. As
  the comoving linear separation increases from virtually 0h^-1^_50_ kpc
  (H_0_ = 50h_50_ km s^-1^ Mpc^-1^, q_0_ = 0) at the redshift of the QSO
  to 2h^-1^_50_ kpc, we derive a best value of 12h^-1^_50_1 kpc for the
  2 σ lower limit and of 160h^-1^_50_ kpc for the 2 σ upper limit of
  the diameter of spherical Lyα clouds in the redshift range 2.1-2.7,
  by means of Monte Carlo simulations. However, if we interpret the two
  anticoincidences as due to a Mg II doublet at z = 0.4261, we find in
  this case a best value of 23h^-1^_50_ kpc to the 2 σ lower limit of
  the Lyα cloud diameter, but we cannot derive any upper limit. For the
  two major heavy-element systems detected in the spectrum of UM 673,
  we do not find any significant difference between the corresponding
  lines in the two spectra, indicating that these systems do not show
  dramatic variations over scales of 0.8h^-1^_50_ and 2.1h^-1^_50_
  kpc, respectively.

Title: The new gravitational lens candidate Q 1208+1011 and the
    importance of high quality data.
Authors: Magain, P.; Surdej, J.; Vanderriest, C.; Pirenne, B.;
   Hutsemékers, D.
Bibcode: 1992Msngr..67...30M
Altcode: 1992Mgr....67...30M
  No abstract at ADS

Title: Using the HST Archive - gravitational lenses from the
    Snapshop Survey
Authors: Pirenne, B.; Surdej, J.; Magain, P.
Bibcode: 1992STECF..17...22P
Altcode:
  No abstract at ADS

Title: Search for gravitational lensing in a sample of highly
    luminous quasars
Authors: Magain, P.; Hutsemekers, D.; Surdej, J.; Vandrom, E.
Bibcode: 1992LNP...406...88M
Altcode: 1992grle.conf...88M
  The status of the ESO survey for gravitational lensing among highly
  luminous quasars (HLQs) is briefly reviewed. The statistics of lensing,
  both concerning the multiple images and the associations of galaxies
  with quasars, are examined. We find a significant overdensity of
  galaxies very close to the line-of-sight to the HLQs. We also report
  the discovery of a new multiply lensed quasar candidate.

Title: Magain P., Surdej J., Vanderriest C., Pirenne B., Hutsemekers
Authors: Magain, P.; Surdej, J.; Vanderriest, C.; Pirenne, B.;
   Hutsemekers, D.
Bibcode: 1992A&A...253L..13M
Altcode:
  We report the discovery of a new gravitational lens candidate: the
  high redshift (z = 3.803) and highly luminous (V = 17.5, M_V_ = - 30.3)
  quasar Q 1208+1011. As derived from the analysis of direct CCD frames
  taken with the ESO/MPI 2.2m telescope, this multiple quasar consists
  of two point-like images, separated by 0.45" and characterized by a
  brightness ratio of 3.5, in red light. Existing spectroscopic data
  support the gravitational lens interpretation for this system but
  cannot exclude the hypothesis of a binary quasar. In the former case,
  the spectrum suggests that, if the metallic absorption line system
  reported by Steidel (1990) at a redshift z = 2.9157 is associated
  with the deflector, the mass of the lens should be of the order of M
  = 7.8 10^11^M_sun_(q_0_ = 0, H_0_ = 50 km s^-1^ Mpc^-1^). Evaluation
  of a recent HST PC frame obtained for Q 1208+1011 within the snapshot
  survey for gravitational lenses confirms the above results.

Title: Gravitational lensing statistics based on a large sample of
    highly luminous quasars observed with ground-based telescopes and HST
Authors: Surdej, J.; Claeskens, J. F.; Crampton, D.; Filippenko,
   A. V.; Hutsemekers, D.; Magain, P.; Pirenne, B.; Vanderriest, C.;
   Yee, H. K. C.
Bibcode: 1992ESOC...44..111S
Altcode: 1992swhs.conf..111S
  We present here some recent results on gravitational lensing statistics
  as applied to a sample of 470 highly luminous quasars.

Title: Optical observations of gravitational lenses
Authors: Surdej, J.; Claeskens, J. F.; Hutsemekers, D.; Magain, P.;
   Pirenne, B.
Bibcode: 1992LNP...406...27S
Altcode: 1992grle.conf...27S
  We report here on some of the major developments achieved on optical
  observations of gravitational lenses since the last conference devoted
  to 'Gravitational Lensing'.

Title: Calibration of the alpha Centauri system : metallicity and age.
Authors: Noels, A.; Grevesse, N.; Magain, P.; Neuforge, C.; Baglin,
   A.; Lebreton, Y.
Bibcode: 1991A&A...247...91N
Altcode:
  The binary system Alpha Cen A and B, with its well known parallax,
  its high quality orbit and the reasonable hypothesis of a common
  origin and age for both components, is a useful test of stellar
  evolution models. Evolutionary sequences are computed for 1.085
  and 0.9 solar masses with different values of Z, Y and alpha (=
  l/Hp). Adopting luminosities and effective temperatures as derived from
  the observations, Z = 0.04, Y = 0.32, alpha = 1.6 and t = 5 Gyr. The
  Z-value derived from evolutionary sequences is very sensitive to the
  difference in effective temperature between the two components.

Title: Abundances of neutron capture elements in metal-poor dwarfs. I
    Yttrium and zirconium.
Authors: Zhao, G.; Magain, P.
Bibcode: 1991A&A...244..425Z
Altcode:
  The yttrium and zirconium abundances are determined in a sample
  of 20 metal-poor stars on the basis of high resolution, high SNR
  spectra. Significant differences between the behaviors of these two
  neighboring elements are found, zirconium being less deficient than
  yttrium in Population II stars. Moreover, there is a genuine cosmic
  scatter in the abundances of these two elements relative to iron, of
  the order of 20 percent. The scatter is lower when these elements are
  compared to titanium, which might indicate that a significant fraction
  of the lighter neutron-capture elements are produced in massive stars.

Title: A Spectroscopic Study of UM673 A &amp;B: on the size of Lyman-
    αClouds
Authors: Smette, A.; Surdej, J.; Shaver, P. A.; Foltz, C. B.; Chaffee,
   F. H.; Weymann, R. J.; Williams, R. E.; Magain, P.
Bibcode: 1991qal..work...37S
Altcode:
  No abstract at ADS

Title: Miscellaneous spectroscopic observations of quasars and
    quasar candidates.
Authors: Veron, P.; Veron-Cetty, M. -P.; Djorgovski, S.; Magain, P.;
   Meylan, G.; Surdej, J.
Bibcode: 1990A&AS...86..543V
Altcode:
  We report about new spectroscopic observations of 11 quasar candidates,
  19 quasars with uncertain redshift and three BL Lac candidates, and
  11 objects located within few arcseconds from a quasar.

Title: The chemical composition ofthe extreme halo
    stars. III. Equivalent widths of 20.
Authors: Zhao, G.; Magain, P.
Bibcode: 1990A&AS...86...85Z
Altcode:
  In the first two papers of this series the chemical composition of
  20 extreme halo stars was discussed. The abundances of a number of
  elements were determined using model atmosphere analysis of equivalent
  widths. In this paper a tabulation of the equivalent width data is
  presented. A comparison of the measurements with the equivalent widths
  from different sources is used to assess the quality of the data.

Title: New Observations and Gravitational Lens Models of the
    Cloverleaf Quasar H1413+117
Authors: Kayser, R.; Surdej, J.; Condon, J. J.; Kellermann, K. I.;
   Magain, P.; Remy, M.; Smette, A.
Bibcode: 1990ApJ...364...15K
Altcode:
  New optical and radio observations of the quadruple quasar H1413 + 117,
  the Cloverleaf, carried out with the 1.54 m Danish telescope at ESO
  and with the VLA at NRAO are presented. The VLA data, obtained in the
  A configuration at 3.6 cm, show radio counterparts at the positions of
  the four optical images and an additional strong radio source between
  images B and D. Gravitational lens models of H1413 + 117 using (a) a
  single elliptical galaxy and (b) two spherical galaxies are presented,
  which fit the positions of the four images of the quasar remarkably
  well. The models suggest that the strong radio source is a feature of
  the quasar, e.g., an ejected blob, which lies right on the caustic of
  the lens and is thereby strongly amplified. The time delays predicted
  by our models are sufficiently short to allow for their determination
  within one observational season, making H1413 + 117 an exceptionally
  well suited object for gravitational lens research.

Title: Core velocity dispersion and mass-to-light ratio of the old
    Magellanicglobular cluster NGC 1835.
Authors: Dubath, P.; Meylan, G.; Mayor, M.; Magain, P.
Bibcode: 1990A&A...239..142D
Altcode:
  The projected velocity dispersion in the core of the old Large
  Magellanic Cloud globular cluster NGC 1835 is deduced from integrated
  light spectra obtained at the European Southern Observatory (ESO)
  with CASPEC, the Cassegrain ESO Echelle Spectrograph mounted on the
  ESO 3.6-m telescope at La Silla, Chile. A numerical cross-correlation
  technique gives a projected velocity dispersion σ_p_(core) = 10.1 + 0.2
  km s^-1^. Multimass anisotropic King-Michie dynamical models are applied
  to the observational constraints given by the surface brightness profile
  and the above central projected velocity dispersion. Depending on the
  model, the values obtained for the total mass of the cluster range
  from 0.70 to 1.55 10^6^ M_sun_, with a mean total mass &lt;M_tot_&gt;
  = 1.0 +/- 0.3 10^6^ M_sun_, corresponding to a global mass-to-light
  ratio &lt;M/L_V_&gt; = 3.4 +/- 1.0 (M/L_V_). The present study
  shows that when the same kind of dynamical models (King-Michie)
  constrained by the same kind of observations (surface brightness
  profile and central value of the projected velocity dispersion) are
  applied to an old rich Magellanic globular cluster, viz., NGC 1835,
  the results seem similar to those obtained in the case of galactic
  globular clusters. Consequently, the rich old globular clusters in
  the Magellanic clouds could be quite similar (in mass and M/L_V_)
  to the rich globular clusters in the Galaxy.

Title: The chemical composition of the extreme halo stars. II. Green
    spectra of 20 dwarfs.
Authors: Zhao, G.; Magain, P.
Bibcode: 1990A&A...238..242Z
Altcode:
  The abundances of nine elements in the atmospheres of 20 extreme
  metal-poor stars are derived from green spectra obtained with the
  ESO Cassegrain Echelle Spectrograph (CASPEC). Sodium is found to be
  overabundant with respect to aluminum by as much as one dex. There
  is some scatter in Ca/Fe which cannot be accounted for by random
  errors in equivalent widths or atmospheric parameters. Scandium is
  overabundant relative to iron. Some barium lines may be affected
  by strong departures from local thermodynamic equilibrium. The
  nitrogen-rich metal-poor star HD 74000, which was found in previous
  work to be also Al-rich, also presents higher than usual abundances
  of Na and of s-process elements. It can thus be considered as a mild
  barium dwarf of Population II.

Title: High-Resolution Spectroscopy of the C 2 Swan 0--0 Band from
    Comet P/Halley
Authors: Lambert, D. L.; Sheffer, Y.; Danks, A. C.; Arpigny, C.;
   Magain, P.
Bibcode: 1990ApJ...353..640L
Altcode:
  High-resolution spectra of the C2 Swan system's 0-0 band from Comet
  P/Halley in March 1986 show that the populations of the upper state's
  rotational levels may be described by two rotational temperatures. The
  low rotational levels provide a low temperature, Trot = about 600 -
  700 K. The higher levels correspond to about 3200 K. If a contribution
  from the 3200-K molecules is subtracted from the populations of the
  low-J-prime levels, the latter are characterized by Trot = about 190
  K. A comparison with recent predictions for C2 molecules fluorescing
  in sunlight shows that the observed and predicted level populations
  are in good agreement for J-prime greater than about 15, but there is
  a sharp disagreement for the low rotational levels.

Title: A search for gravitational lensing among highly luminous
quasars : observational strategy and survey
Authors: Swings, J. P.; Magain, P.; Remy, M.; Surdej, J.; Smette,
   A.; Hutsemekers, D.; van Drom, E.
Bibcode: 1990LNP...360...83S
Altcode: 1990grle.work...83S
  The observational technique used for our search for gravitational
  mirages is presented : recent results, as well as future observations,
  are outlined.

Title: Preliminary analysis of high-resolution spectra for UM 673
    A &amp; B
Authors: Smette, A.; Surdej, J.; Shaver, P. A.; Foltz, C. B.; Chaffee,
   F. H., Jr.; Magain, P.
Bibcode: 1990LNP...360..122S
Altcode: 1990grle.work..122S
  No abstract at ADS

Title: A Search for Gravitational Lensing Among Highly Luminous
Quasars: New Results
Authors: Magain, P.; Remy, M.; Surdej, J.; Swings, J. -P.; Smette, A.
Bibcode: 1990LNP...360...88M
Altcode: 1990grle.work...88M
  Images of highly luminous QSOs are analyzed to determine whether
  the gravitational magnification of the background QSO by matter
  associated with the foreground galaxies accounts for the excess of
  galaxies in the fields of distant QSOs. Galaxy detection is increased
  by utilizing red-filter images, 40 taken with the EFOSC at the ESO
  3.6-m telescope and 43 taken with a direct CCD camera at the ESO/MPI
  2.2-m telescope. The R-magnitude ranges from 22.5 to 23.0 for the
  sample, for which the number of galaxies is counted by eye, showing
  45 galaxies of radio and optical type. The overdensity found is not as
  pronounced as that of Fugmann (1988) or that of Webster et al. (1988). A
  systematic subtraction of the point spread function is also described to
  investigate the idea that some galaxies responsible for the QSO light
  magnification are within the inner 3-arcsec circle. The galaxies very
  close to the line-of-sight are theorized to contribute significantly
  to the magnification of these QSOs.

Title: Two more very massive stars resolved.
Authors: Heydari-Malayeri, M.; Magain, P.; Remy, M.
Bibcode: 1989A&A...222...41H
Altcode:
  We present new evidence against the existence of very massive stars in
  the Magellanic Clouds. Using high resolution CCD images and appropriate
  image restoration methods, we show that Sk 157 and Sk-69^deg^253
  (Sanduleak, 1968, 1969), lying in the SMC and LMC respectively, are
  not single, very massive, but multiple systems. Thus, two of the most
  massive stars in existence, with the estimated masses of ~ 85 _sun_
  and &gt; 120 M_sun_, vanish from astronomy. The results presented
  here have important implications for star formation models and the
  extragalactic distance scale.

Title: A study of the interstellar medium in line to NGC 5128 from
    high resolution observations of the supernova 1986G.
Authors: D'Odorico, S.; di Serego Alighieri, S.; Pettini, M.; Magain,
   P.; Nissen, P. E.; Panagia, N.
Bibcode: 1989A&A...215...21D
Altcode: 1989A&A...215...21O
  We present new high resolution, high S/N ratio spectra of supernova
  1986G in NGC 5128 (Cen A). These data allow a detailed study of the
  rich interstellar absorption spectrum originating in the line of sight
  to the SN. At least 12 distinct Ca II and Na I absorbing clouds are
  identified. The gas associated with NGC 5128 is spread over a velocity
  range of 178 km s^-1^ and it is split in at least 7 components. A
  new result unique to NGC 5128 is the presence of 3 components with
  Ca^+^/Na^0^ column densities ratios smaller than 1, that is typical
  of cool disc gas. This is interpreted as a further indication of the
  existence of an extended warped disc or a ring of cool gas. From the
  discussion of the velocities of the absorption components seen in its
  spectrum it is inferred that the SN was at least half way within the
  dust and gaseous disc of the galaxy. An intriguing result of this work
  is the discovery of two absorption components at v_H_ = 236 and 257 km
  s^-1^, which cannot be easily explained within the velocity field of
  either the Galaxy or NGC 5128, and may be related to high velocity
  clouds of neutral hydrogen observed at nearby lines of sight. We
  detected and measured several diffuse interstellar bands at galactic
  and NGC 5128 velocities. This is the first time that such a detailed
  study has been done in a galaxy beyond the Magellanic Cloud. At NGC 5128
  velocities, we also detected, for the first time beyond the Local Group,
  molecular absorption lines of CH and CH^+^ at optical wavelengths.

Title: What is the mass-to-light ratio of the old Magellanic globular
    cluster NGC 1835?
Authors: Meylan, G.; Dubath, P.; Mayor, M.; Magain, P.
Bibcode: 1989Msngr..55...55M
Altcode: 1989Mgr....55...55M
  We astronomers are lucky: our Galaxy as two companion galaxies, the
  Large and Small Magellanic Clouds, situated weil above the galactic
  plane, which Contain a huge potential of astrophysical information. For
  example, concern: ng star clusters, the realm of the globuar clusters
  is much richer and more Varied in the Magellanic Clouds than in the
  Galaxy: rich clusters of all ages are observed, from the youngest,
  having ages of a few tens 10^6 yr to the oldest 1haV'lng ages of the
  order"or larger than 10 10^9 yr. In this paper, only old Magellanic
  and galactic globular clusters are considered.

Title: Absolute dimensions of eclipsing binaries. XIV. UX Mensae.
Authors: Andersen, J.; Clausen, J. V.; Magain, P.
Bibcode: 1989A&A...211..346A
Altcode:
  Spectroscopic orbits are determined for the 4-day, F8 V eclipsing binary
  UX Mensae. The masses of the binary components are 1.24 and 1.20 solar
  masses with errors of + or - 0.5 percent. The results of the analysis of
  the uvby light curves by Clausen and Gronbech (1976) are confirmed. The
  metal abundance is found to be Fe/H = +0.04 + or - 0.10. Absolute
  dimensions are computed for the binary. Theoretical evolutionary
  sequences for the masses and metal abundance are interpolated from
  the models of VandenBerg (1988) and Andersen et al. (1988).

Title: IRC +10216: a peanut nebula!
Authors: Le Bertre, T.; Magain, P.; Remy, M.
Bibcode: 1989Msngr..55...25L
Altcode:
  Carbon stars with low effective temperature (2,000-3,000 K) are thought
  to be long-period variables evolving on the Asymptotic Giant Branch
  (AGB). These objects are burning alternately hydrogen and helium
  in different shells around a degenerate core of carbon and oxygen
  [1]. Material processed during the helium burning phase is dredged-up by
  convection to the surface and enriches it in carbon relative to oxygen.

Title: Profiles of a Key Programme: Gravitational Lensing
Authors: Surdej, J.; Arnaud, J.; Borgeest, U.; Djorgovski, S.;
   Fleischmann, F.; Hammer, F.; Hutsemekers, D.; Kayser, R.; Le Fevre,
   O.; Nottale, L.; Magain, P.; Meylan, G.; Refsdal, S.; Remy, M.;
   Shaver, P.; Smette, A.; Swings, J. P.; Vanderriest, C.; van Drom,
   E.; Véron-Cetty, M.; Véron, P.; Weigelt, G.
Bibcode: 1989Msngr..55....8S
Altcode: 1989Mgr....55....8S
  Prior to Professor van der Laan's enquiry, in the March 1988 issue
  of the Messenger, on the general interest among astronomers from the
  European community to possibly participate in Key Programmes (KPs)
  at the European 80uthern Observatory, at least three distinct groups
  (including more than half of the above authors) were already involved
  in the study of "gravitational lensing" effects (see box on pages
  10-11). Observations were being performed with the help of various
  telescopes on La 8illa as weil as at other observatories (VLA, CFHT,
  Palomar, Kitt Peak, etc.).

Title: Core Velocity Dispersion of the LMC Globular Cluster NGC 1835
Authors: Meylan, G.; Dubath, P.; Mayor, M.; Magain, P.
Bibcode: 1989BAAS...21..711M
Altcode:
  No abstract at ADS

Title: A Simple Deconvolution Algorithm
Authors: Magain, P.
Bibcode: 1989ESOC...31..205M
Altcode: 1989daan.work..205M
  A very simple image deconvolution algorithm is described in three
  cases. It is first established in the case of noise-free data. Then, a
  method for taking noise into account is presented. Finally, a smoothing
  constraint is included in the algorithm.

Title: The chemical composition of the extreme halo stars. I. Blue
    spectra of 20 dwarfs
Authors: Magain, P.
Bibcode: 1989A&A...209..211M
Altcode:
  Spectra obtained with the ESO Cassegrain echelle spectrograph are
  used to determine the abundances of 13 elements in the atmospheres of
  20 extreme halo dwarfs. It is found that the alpha elements Mg, Ca,
  and Ti are overabundant with respect to Fe, that the Cr/Fe ratio is
  solar at all metallicities, and that Al is overdeficient relative to
  Mg. The results also indicate that the s elements Sr, Y, and Ba are
  overdeficient with respect to Fe in stars with Fe/H ratios of less
  than 2.3, and that for ratios greater than 2.3 the s element abundances
  relative to Fe are roughly constant (at either solar or higher values).

Title: New evidence against the existence of very massive stars.
Authors: Heydari-Malayeri, M.; Magain, P.; Remy, M.
Bibcode: 1988A&A...201L..41H
Altcode:
  The most luminous stars are our first probes for exploring the
  stellar content of distant galaxies. They have also been used as
  standard candles for extragalactic distance determinations. We
  show that Sk-66^deg^ 41, one of the brightest stars in the Large
  Magellanic Cloud (LMC), is a multiple system consisting of at least six
  components. This result has important consequences for the understanding
  of star formation mechanisms, especially the upper limit to stellar
  masses. Moreover, when primary distance indicators are not available,
  care should be taken in using the brightest blue stars. The derived
  distances, depending on the number of cluster members, can easily be
  underestimated by more than a factor 2, leading to larger values for
  the Hubble constant.

Title: Discovery of a quadruply lensed quasar: the 'clover leaf
    H1413 + 117
Authors: Magain, P.; Surdej, J.; Swings, J. -P.; Borgeest, U.;
   Kayser, R.
Bibcode: 1988Natur.334..325M
Altcode: 1988Nat...334..325M
  In November 1986 we began an optical search for examples of
  gravitational lensing in a sample of highly luminous quasars (HLQs,
  M<SUB>v</SUB> &lt; -29), with the aims of improving our knowledge of
  the quasar luminosity function, studying the dark matter content of the
  Universe, and redetermining some important cosmological parameters. This
  survey has found one new case of lensing<SUP>1,2</SUP> and the general
  implications of the search have been summarized<SUP>3</SUP>. Here we
  report the discovery of a second gravitational lens system in the
  broad absorption line quasar H1413 + 117 (refs 4-6). Four images
  of comparable brightness are seen, separated by ~1 arcsec. Spectra
  obtained of two of the images are identical apart from the presence
  of sharp absorption lines in one component, which are presumably due
  to gas clouds along the line of sight. The unique configuration of
  the images, together with the fairly rare occurrence of this type of
  quasar, makes it incontrovertible that this is a lensed system, not a
  cluster of quasars, and this second discovery made by imaging bright
  quasars establishes the power of the method for finding systems with
  small separations.

Title: Observations of the new gravitational lens system UM 673 =
    Q 0142-100.
Authors: Surdej, J.; Magain, P.; Swings, J. -P.; Borgeest, U.;
   Courvoisier, T. J. -L.; Kayer, R.; Kellermann, K. I.; Kuhr, H.;
   Refsdal, S.
Bibcode: 1988A&A...198...49S
Altcode:
  In order to better understand the effects of gravitational lensing
  on the observed quasar luminosity function, on the source counts
  of extragalactic objects, etc., we have recently initiated a high
  resolution direct imaging survey of a selected sample of Highly
  Luminous Quasars (HLQs). The observations are being carried out
  with the 2.2 m telescope at ESO, and with the VLA at the NRAO, New
  Mexico. Following a first observing run at ESO, we have reported the
  discovery of a new gravitational lens system for the HLQ UM 673 =
  Q0142-100. Additional observations supporting this interpretation
  are discussed here. We confirm that UM 673 is resolved into two
  quasi-stellar images A(m_V_=17.0) and B(m_V_=19.1) separated by 2.22"
  and having essentially the same redshift (z_e_=2.719 with z_e_(A)-
  z_e_(B)=-0.0002 +/-0.0008). Their emission (Lyα, N V, Si IV, C IV,
  etc.) as well as absorption (including a high ionization system at
  z_a_=2.3564) line spectra also appear to be quite identical. Further
  evidence for the presence of a lensing galaxy (m_R_=19, z_g_=0.49)
  between the two QSO images is given by the detection of faint absorption
  lines due to Ca II H and K, and possibly Na I D1 and D2, at a redshift
  z=0.493 in the spectrum of UM 673 B. Application of gravitational
  optometry to this system is given in the present article: a value of
  M_0_ = 2.4 10^11^ M_sun_ is derived for the mass of the lensing galaxy
  located between UM 673 A and B and a most likely estimate of {DELTA}t =
  7 weeks is found for the expected delay between the arrival times of
  a similar variability event in the two lensed images of the quasar
  (H_0_=75 km s^-1^ Mpc^-1^, q_0_=0). A VLA observation of UM 673 has
  been obtained at 6 cm in the hybrid C/D-array configuration. This
  radio map indicates the presence of a faint elongated structure which
  is possibly associated with the UM 673 gravitational lens system.

Title: The SMC compact blob N 81 : a detailed multi-wavelength
    investigation.
Authors: Heydari-Malayeri, M.; Le Bertre, T.; Magain, P.
Bibcode: 1988A&A...195..230H
Altcode:
  This paper is devoted to an extensive investigation of the compact Small
  Magellanic Cloud H II region N81. Several observational techniques with
  various telescopes at ESO have been employed to acquire a multi-aspect
  view of the physical characteristics of this interesting nebula:
  CCD, IDS and Reticon high, medium and low resolution spectroscopy
  (range 3700-10000 A), CCD imaging using 17 different filters,
  optical and infrared photometry at UBVRI and JHK. We also use the H I
  emission observations reported in the literature. The nebula N81 is
  probably excited by one star of about 60 M_sun_, (T_eff_ = 47500 K)
  accompanied by a cluster of about 10 B0 stars (M = 15 M_sun_, T_eff_
  = 32000 K). We derive the absolute visual magnitude of the exciting
  star to be -5.1, corresponding to a bolometric magnitude of M_bol_=
  -9.1 and a luminosity of 3.5 10^5^ L_sun_. This nebula is a young H II
  region. From the equivalent width of the Hβ emission line we derive an
  age of 2.5 10^6^yr for N81. We stress the importance of correcting the
  continuum emission around Hβ for the nebular contribution. We derive
  the gas electron density and temperature and compute the chemical
  abundances of He, O, N, Ne, S, and Ar. The results are compared with
  the mean values available for the SMC. The high resolution profile
  of N81 at Hβ was decomposed into its various components. We find
  the most probable three dimensional turbulent velocity in N81 to
  be about 3 km s^-1^. We observationally confirm the proposition by
  Koornneef and Israel (1985) that the H_2_ emission may be produced by
  the action of a mild shock moving through the ambient cloud of this
  nebula. Interestingly, unlike other representatives of this category
  of H II regions in the Magellanic Clouds, N81 is not affected by the
  local dust. The nebula N81 is associated with the SMC H I cloud of
  radial velocity +167 km s^-1^, observed by McGee and Newton (1981). The
  neighboring H II complexes N83 are associated with a density peak of
  this H I cloud. N 88 A, another SMC H II blob, lying in the vicinity of
  N 81, is associated with another H I cloud. We speculate that N 81 and
  N 88 A may have been formed due to a collision between these two clouds.

Title: Very low upper limits on the strength of interstellar lithium
    lines toward SN 1987A.
Authors: Baade, D.; Magain, P.
Bibcode: 1988A&A...194..237B
Altcode:
  Seven CCD and eleven Reticon spectra of high spectral resolution and
  low noise have been carefully analysed in search for faint absorption
  lines due to neutral interstellar lithium λ 6708 A along the line
  of sight to SN 1987A in the Large Magellanic Cloud (LMC). At the
  velocities of the strongest interstellar Ca II and Na I lines,
  no evidence of any interstellar feature has been found. An upper
  limit for the strongest components expected is 0.15 mA for both the
  Galaxy and the LMC. From these we infer elemental column densities
  N_Galaxy_ &lt;= 2.6 10^11^ cm^-2^ and N_LMC_ &lt;= 1.4 10^11^ cm^-2^
  and gaseous elemental abundances (Li/H I)_Galaxy_ &lt;= 7.7 10^-10^
  and (Li/H I)_LMC_ &lt;= 1.0 10^-10^ with an estimated uncertainty of
  the abundance limits of a factor of 4 (0.6 dex).

Title: Pre- and post-perihelion spectrographic and photometric
    observations of Comet Wilson (1986 l)
Authors: Arpigny, C.; Dossin, F.; Manfroid, J.; Magain, P.; Haefner, R.
Bibcode: 1988Msngr..51...27A
Altcode:
  The behavior of Comet Wilson before and after its passage through
  perihelion, which occurred on April 21, 1987, was studied on the basis
  of spectrographic and photometric observations. Results pertaining to
  spectra in the UV, blue, and red regions, and to photometry through
  narrow-band filters are presented. It is suggested that the fading of
  Comet Wilson might reflect some general trend in the comet's evolution,
  or that it could be the result of a geometrical effect associated with
  the rotation of the comet's nucleus and the presence of discrete active
  areas on its surface.

Title: Search for Gravitational Lensing from a Survey of Highly
    Luminous Quasars
Authors: Surdej, J.; Swings, J. -P.; Magain, P.; Borgeest, U.; Kayser,
   R.; Refsdal, S.; Courvoisier, T. J. -L.; Kellermann, K. I.; Kuhr, H.
Bibcode: 1988ASPC....2..183S
Altcode: 1988osq..conf..183S
  The authors have shown that their search for gravitational lensing
  from a survey of optically selected highly luminous quasars (HLQ)
  appears very promising. Observational features (multiple images,
  image elongation, jet-like feature, fuzz, etc.) possibly associated
  with the HLQ phenomenon have been detected for more than 20% of the
  objects under study. While it is not yet known how many of the HLQs
  are gravitational mirages, at least 5 (out of 111) of the investigated
  quasars appear to be highly luminous because of amplification of their
  brightness by gravitational lensing.

Title: Could the gravitational lensing alter the observational data
    in the extragalactic field?
Authors: Surdej, J.; Magain, P.; Swings, J. P.; Remy, M.; Borgeest,
   U.; Kayser, R.; Refsdal, S.; Kühr, H.
Bibcode: 1988lsso.conf...95S
Altcode:
  No abstract at ADS

Title: Non-Lte Effects and Abundance Analyses of Halo Stars
Authors: Magain, P.
Bibcode: 1988IAUS..132..485M
Altcode:
  The possible existence of departures from LTE affecting the abundance
  analyses of halo dwarfs and subgiants is analysed from the observational
  point of view, and illustrated by the case of the intermediate halo
  subgiant HD 76932.

Title: A new CCD camera for the Echelec spectrograph.
Authors: Gilliotte, A.; Magain, P.
Bibcode: 1987Msngr..50...46G
Altcode:
  The Echelec spectrograph, installed at La Silla in 1973, was designed
  to be used with an electronographic camera. However, by adding a
  flatfield corrector, it can be operated with other detectors, such as
  CCD's. As part of the upgrading programme of the 1.52-m telescope, and
  in order to improve the spectroscopic capabilities of that instrument,
  the Echelec spectrograph has been modified and is now working with
  the same CCD detector as used on the Boiler and Chivens spectrograph.

Title: Resolution of the OI + NH2 Blend in Comet p/ Halley
Authors: Arpigny, C.; Magain, P.; Manfroid, J.; Dossin, F.; Danks,
   A. C.; Lambert, K. L.
Bibcode: 1987A&A...187..485A
Altcode:
  Spectra of comet P/Halley have been taken at very high resolution
  (0.015 nm) with a view to evaluating the contamination of
  the forbidden oxygen doublet at 630 nm by NH<SUB>2</SUB>
  features at low resolution. Comparison is made with a few other
  bright comets. Appreciable variations are found not only in the
  NH<SUB>2</SUB>/[O I] ratio but also in the relative intensities of the
  various NH<SUB>2</SUB> emissions themselves. The authors comment upon
  the accuracy obtained on the oxygen abundance derived from the [O I]
  lines. Mapping of these emissions over the coma is required in order
  to correctly remove any important NH<SUB>2</SUB> contribution at low
  resolution. This should in addition provide information bearing upon
  the origin of the oxygen atoms in the <SUP>1</SUP>D level.

Title: A new case of gravitational lensing
Authors: Surdej, J.; Magain, P.; Swings, J. -P.; Borgeest, U.;
   Courvoisier, T. J. -L.; Kayser, R.; Kellermann, K. I.; Kuhr, H.;
   Refsdal, S.
Bibcode: 1987Natur.329..695S
Altcode: 1987Nat...329..695S
  Even before the discovery of the first gravitational lens
  system<SUP>1</SUP> in 1979 (see ref. 2 for a recent review of the
  other published candidates), it was recognized that a statistical
  evaluation of the occurrence of gravitational lensing within a
  well-defined sample of quasars is important to understand better
  the quasar luminosity function and possibly the QSO phenomenon
  itself<SUP>3</SUP>, to test cosmological models<SUP>4,5</SUP> and to
  probe the luminous and dark matter distribution on various scales in
  the Universe<SUP>4-6</SUP>. A year ago, we began a systematic search
  from the European Southern Observatory (ESO) at La Silla, Chile, for
  gravitational lens systems in a selected sample of highly luminous
  quasars; M<SUB>v</SUB>&lt;-29.0. These objects are promising candidates
  for gravitationally lensed QSO images with arc-second and sub-arc-second
  separations (J.S. et al., manuscript in preparation and refs 7 and
  8). Since December 1986, we have identified four possible cases. Here
  we give a brief description of our first identified gravitational
  lens system UM673 = Q0142-100 =PHL3703<SUP>9-11</SUP>. It consists
  of two images, A (m<SUB>R</SUB> = 16.9) and B (m<SUB>R</SUB> = 19.1),
  separated by 2.2arcs at a redshift z<SUB>q</SUB> = 2.719. The lensing
  galaxy (m<SUB>R</SUB>~ 19, Z<SUB>L</SUB>~0.49) has also been found. It
  lies very near the line connecting the two QSO images, ~0.8 arc s
  from the fainter one. Application of gravitational optometry to this
  system leads to a value M<SUB>0</SUB>~2.4×10<SUP>11</SUP>Msolar for
  the mass of the lensing galaxy and to δt~7 weeks for the most likely
  travel-time difference between the two light paths to the QSO (assuming
  H<SUB>0</SUB>= 75 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>,q<SUB>0</SUB> = 0).

Title: Detection of interstellar CH and CH+ towards SN 1987A.
Authors: Magain, P.; Gillet, D.
Bibcode: 1987A&A...184L...5M
Altcode:
  The authors report the detection of interstellar CH and CH<SUP>+</SUP>
  towards supernova 1987A. For both of these molecules, one component is
  detected at a heliocentric velocity of about 280 km/s, corresponding
  to material inside the LMC. Some implications of the authors' results
  with regards to the H<SUB>2</SUB>-to-dust ratio are briefly discussed.

Title: Interstellar calcium towards supernova 1987A in the Large
    Magellanic Cloud
Authors: Magain, Pierre
Bibcode: 1987Natur.329..606M
Altcode: 1987Nat...329..606M
  We present high-resolution and high signal-to-noise spectra of
  interstellar calcium towards SN1987A in the Large Magellanic Cloud
  (LMC). They supplement previously published observations<SUP>1,2</SUP>
  for Ca II and provide completely new results for the Ca I spectrum,
  in which eleven components are detected, not only at velocities
  corresponding to our Galaxy and the LMC, but also at intermediate
  velocities. Our spectra, that allow us to estimate the ionization
  balance in these interstellar clouds, provide some clues about their
  physical state and location. In particular, the components between
  150 and 200 km s<SUP>-1</SUP> show a much lower ionization degree than
  other components. This may be due to recent compression of the gas by
  a shock, possibly associated with a former supernova explosion. This
  interpretation would require the corresponding clouds to be located
  inside the LMC, indicating that at least some intermediate velocity
  components are not of halo origin.

Title: On the interpretation of the CH cometary spectrum.
Authors: Arpigny, C.; Zeippen, C. J.; Klutz, M.; Magain, P.;
   Hutsemekers, D.
Bibcode: 1987ESASP.278..607A
Altcode: 1987dsc..proc..607A
  A procedure to compute cometary spectra taking into account radiative
  processes and collisional effects is described. The populations of the
  rotational levels are determined by solving the statistical equilibrium
  equations at a certain number of locations within the coma (which can be
  modelled with n(R), T(R), v(R) laws) and the emerging intensity is then
  evaluated by integrating the emissions along the line of sight. Such
  a program was applied to the CH radical. The importance of collisions
  in exciting the lower rotational levels of CH is confirmed.

Title: On the forbidden red lines of oxygen in comets.
Authors: Arpigny, C.; Manfroid, J.; Magain, P.; Haefner, R.
Bibcode: 1987ESASP.278..571A
Altcode: 1987dsc..proc..571A
  Eighteen spectra of 8 different comets observed at high and medium
  resolution were analyzed in the 627 to 637 nm region to determine the
  contributions of the (OI) red doublet and of the various NH2 lines
  present in this wavelength interval. Results confirm that there exist
  appreciable variations not only in the (OI)/NH2 ratio, but also in the
  relative intensities of the NH2 features among themselves, therefore,
  it is not justified to derive the (OI) line flux from the 630.0 blend,
  as was done in previous low-resolution work, by assuming a fixed
  relative strength of the NH2 emission contained in this blend. Mapping
  of these emissions over the coma is recommended.

Title: High Resolution Spectroscopy and Analysis of the
    C<SUB>2</SUB>(0,0) Band in Comet P/Halley
Authors: Danks, A. C.; Lambert, D. L.; Sheffer, Y.; Arpigny, C.;
   Dossin, F.; Magain, P.
Bibcode: 1987BAAS...19.1124D
Altcode:
  No abstract at ADS

Title: The missing opacity and the temperature calibration of
    solar-type stars.
Authors: Magain, P.
Bibcode: 1987A&A...181..323M
Altcode:
  The novel temperature calibration of some color indices presented for
  G and F dwarfs is based on the IR flux method and extends the work of
  Saxner and Hammarback (1985) to the Population II stars. Attention
  is given to the discrepancy between theoretical and empirical
  temperature calibrations. It is suggested that the most straightforward
  interpretation of the disagreement between empirical colors and some
  model predictions is that of the 'missing opacity' due to a veil of
  faint metal lines, present in the blue and UV regions of the spectra
  of solar-type and cooler stars, but excluded from the model.

Title: HD 151932 variability revisited.
Authors: Vreux, J. M.; Magain, P.; Manfroid, J.; Scuflaire, R.
Bibcode: 1987A&A...180L..17V
Altcode:
  The observation of variations in the blue absorption component of the
  He I lines as well as in the Si IV 4089 emission line of HD 151932 is
  reported. Possible explanations for these variations are addressed,
  and it is concluded that none is satisfactory. The possibility of a
  periodicity in the variations is briefly considered.

Title: Abundances of light elements in halo dwarfs : a re-analysis.
Authors: Magain, P.
Bibcode: 1987A&A...179..176M
Altcode:
  The abundances of a few light elements in the atmospheres of halo
  dwarfs are redetermined on the basis of literature data reanalysed in
  an homogeneous way. It is shown that the scatter of the resulting Mg
  and Al abundances is strongly reduced and that no discrepancy remains
  between the abundances deduced from blue and red lines. Mg, Si and
  Ca show constant overabundances while the Al overdeficiency seems in
  agreement with the predictions of explosive carbon burning.

Title: Photometric Observations of WR78 = HD 151932
Authors: Magain, P.; Vreux, J. M.; Manfroid, J.
Bibcode: 1987IBVS.3022....1M
Altcode:
  No abstract at ADS

Title: BD +03 deg 740 - A new extreme metal-poor dwarf
Authors: Magain, P.
Bibcode: 1987Msngr..47...18M
Altcode:
  The results of a preliminary analysis of BD +03 deg 740 are
  presented. The analysis was based on the blue spectrum which was
  obtained with an exposure time of 40 min, giving a good S/N ratio
  for this 9.8-mag star. Graphs are presented which reveal the extreme
  weakness of the metal lines in the spectrum. The analysis of BD +03 deg
  740, which is the most metal-poor dwarf in which s element abundances
  have been determined, confirms the presence of secondary elements in
  the atmospheres of the extreme halo dwarfs.

Title: Supernova 1987A in the Large Magellanic Cloud
Authors: Cristiani, S.; Gouiffes, C.; Hanuschik, R.; Magain, P.;
   Dawe, J.; McNaught, R. H.; Beresford, T.
Bibcode: 1987IAUC.4350....1C
Altcode: 1987IAUC.4350....0C
  S. Cristiani and C. Gouiffes, European Southern Observatory;
  R. Hanuschik, Bochum University; and P. Magain, ESO, report: "Spectra
  taken at intermediate resolution (0.2-0.3 nm) between Mar. 14 and
  22, with the spectrum scanner attached to the Bochum University
  0.61-m telescope and with the ESO 1.5-m telescope at La Silla,
  showed changes in the P-Cyg profile of H-alpha. On Mar. 15, a weak
  bump at 647 nm appeared on the previously-very-smooth P-Cyg profile
  (near the bottom of the absorption) which developed in the following
  days, assuming a peaked structure and reaching the continuum level
  about Mar. 20. A comparison with previous spectra suggests that this
  is an additional emission feature. Spectra taken with the CAT 1.4-m
  telescope (resolution 80000) do not show smaller- scale structures. The
  precise wavelength of the relative maximum in the spectrum is 647.0 nm,
  followed by a minimum at 648.8 nm. The FWHM of the two features is 1.45
  and 2.10 nm, respectively. If identified with H-alpha, the emission
  corresponds to a velocity of -4500 km/s. No corresponding structures
  have been observed in the P-Cyg profiles of H-beta and Ca 860-nm. Those
  observations suggest a distortion in the spherical symmetric outflow of
  the explosion, which can be confirmed by polarization observations of
  the H-alpha profile." Provisional photoelectric photometry by J. Dawe
  and R. H. McNaught with the Australian National University 0.61-m
  reflector at Siding Spring Observatory: Mar. 20.456 UT, V = 4.12, B-V
  = +1.58, U-B = +2.04. Further visual magnitude estimates: Mar. 19.39,
  4.1 (McNaught); 19.52, 4.0 (T. Beresford, Adelaide, South Australia);
  20.45, 4.0 (McNaught); 20.48, 3.9 (Beresford).

Title: Supernova 1987A in the Large Magellanic Cloud
Authors: Cristiani, S.; Gouiffes, C.; Hanuschik, R.; Magain, P.;
   Dawe, J.; McNaught, R. H.; Beresford, A.
Bibcode: 1987IAUC.4350.....C
Altcode:
  No abstract at ADS

Title: Resolution of the [O I]+NH<SUB>2</SUB> blend in comets.
Authors: Arpigny, C.; Magain, P.; Manfroid, J.; Dossin, F.; Haefner, R.
Bibcode: 1987LIACo..27..315A
Altcode:
  No abstract at ADS

Title: Very Low Upper Limits on the Strength of Interstellar Lithium
    Lines Toward Supernova 1987A
Authors: Baade, D.; Magain, P.
Bibcode: 1987ESOC...26..537B
Altcode: 1987sn...work..537B
  No abstract at ADS

Title: CES+CCD Observations of Interstellar Lines Towards Supernova
    1987A
Authors: Magain, P.
Bibcode: 1987ESOC...26..533M
Altcode: 1987sn...work..533M
  No abstract at ADS

Title: High resolution spectroscopy with the E.S.O. Coudé Echelle
    Spectrometer.
Authors: Magain, Pierre
Bibcode: 1987LIACo..27...15M
Altcode: 1987oahp.proc...15M
  Various applications of high resolution spectroscopy with the ESO Coude
  Echelle Spectrometer (CES) are discussed. The aim of this paper is not
  to present a complete survey of the CES capabilities, but to illustrate
  some possible applications, with emphasis on rather unusual aspects. In
  all the observations presented here, the CES has been used with the new
  short camera and a CCD detector (high resolution RCA SID 503, 640 x 1024
  pixels, 15x15 microns each). Compared to the long camera and Reticon
  detector, this new combination represents an increase of efficiency
  of 2 to 3 magnitudes with only a moderate loss of resolving power.

Title: Resolution of the (OI)+NH<SUB>2</SUB> Blend in Comet P/halley
Authors: Arpigny, C.; Magain, P.; Manfroid, J.; Dossin, F.; Danks,
   A. C.; Lambert, D. L.
Bibcode: 1986ESASP.250c..81A
Altcode:
  Spectra of P/Halley were taken at very high resolution (0.15A)
  to evaluate contamination of the forbidden oxygen doublet by NH2
  features at low resolution. Comparison is made with other bright
  comets. Appreciable variations are found in the NH2/(OI) ratio and
  in the relative intensities of the NH2 emissions themselves. The
  accuracy obtained on the oxygen abundance derived from the (OI) lines
  is discussed. Mapping of these emissions over the coma is required to
  correctly remove any important NH2 contribution at low resolution. This
  should also provide information on the origin of the oxygen atoms in
  the 1D level.

Title: Spectroscopy, Photometry and Direct Filter Imagery of Comet
    P/Halley
Authors: Arpigny, C.; Dossin, F.; Manfroid, J.; Magain, P.; Danks,
   A. C.; Lambert, D. L.; Sterken, C.
Bibcode: 1986Msngr..45....8A
Altcode: 1986Msngr..45....8S
  Observational techniques and instrumentation applied in ground-based
  studies of the cometary coma during the post-perihelion phase of
  the recent passage of Comet Halley are summarized. Applications of
  a 1.5 m telescope equipped with a coude spectrograph for long slit
  investigations of spectral intensity distributions, a 1.4 m CAT,
  coude echelle spectrometer and reticon to evaluate the C-12/C-13
  isotopic abundance ratio, and a 50 cm photometric telescope for
  narrow bandwidth spectroscopy are described. Finally, the 1.5 m Danish
  telescope, equipped with a CCD camera, collected high spatial resolution
  photographs of the various coma components when the comet was 0.42 AU
  from the sun.

Title: Contribution functions and the depths of formation of
    spectral lines
Authors: Magain, P.
Bibcode: 1986A&A...163..135M
Altcode:
  A rigorous expression is derived for the contribution function to the
  spectral line depression in a stellar atmosphere; this, in effect, gives
  the contribution of the different atmospheric layers to the formation of
  the line depression. This contribution function is the solution of the
  transfer equation for the line depression. It is the only appropriate
  distribution function for the computation of the depths of formation of
  spectral lines. It indicates, in contrast to some earlier contribution
  functions, that a faint spectral line is not necessarily formed in
  the same layers as the continuum. The response function of the line
  depression to a given perturbation is briefly discussed.

Title: Spectroscopic analysis of extreme metal-poor
    ''dwarfs''. II. Improvedmodel atmospheres and detailed abundances.
Authors: Magain, P.
Bibcode: 1985A&A...146...95M
Altcode:
  High resolution spectrophotometric data were obtained for the stellar
  objects HD 19445 and HD 140283. The spectra gathered were well-matched
  by model stellar atmospheres for the continuous flux and Fe I excitation
  equilibrium. HD 19445 was identified as a dwarf star and HD 140283
  as a subgiant. Abundance analyses indicated an Fe abundance lower
  than previously estimated, oxygen overabundant relative to C and Fe,
  Mg, Si and Ca overabundant relative to Fe, and deficiencies of Al and
  Mn. Sr was overabundant relative to Ba. The abundance discrepancies are
  in disagreement with the standard nucleosynthesis model. Further such
  spectroscopic data are needed to develop accurate galactic chemical
  evolution models.

Title: A comment on systematic errors in determinations of
    microturbulent velocities
Authors: Magain, P.
Bibcode: 1984A&A...134..189M
Altcode:
  It is shown that the usual method of microturbulent velocity
  determination from the "abundance versus equivalent width" plot leads
  to a systematic overestimate of the microturbulent velocity when
  the observd equivalent widths are affected by random errors. This
  overestimate is due to the correlation between errors in observed
  equivalent widths and in line abundances. This error rises rapidly with
  decreasing quality of the observational material and may be avoided
  by using theoretical equivalent widths instead of observed ones as
  abscissa of the "abundance versus equivalent width" plot.

Title: Spectroscopic analysis of extreme metal-poor
    'dwarfs'. I. Observational material, Fe lines, and model atmospheres.
Authors: Magain, P.
Bibcode: 1984A&A...132..208M
Altcode:
  Fe lines are analysed in the spectra of the two extreme metal-poor
  stars MD 19445 and MD 140283 on the basis of new observational
  material. It is shown that the use of accurate equivalent widths
  and very accurate oscillator strengths improves significantly the
  quality of the analysis. In particular, these stars are found to be
  more metal-deficient than precedingly thought. This result may imply a
  significant revision of the adopted abundance scale. It is shown that
  differential analyses of such stars relative to the Sun are subject to
  important systematic errors due to the very large difference between
  the stellar and solar equivalent widths. Finally, the temperature
  criteria are analysed and it is argued that the criteria linked to deep
  atmospheric layers, such as the B - V colour or the hydrogen line wings,
  should not be used to select a model representing satisfactorily the
  line-forming layers.

Title: Etude détaillée d'étoiles froides pauvres en métaux Title:
Etude détaillée d'étoiles froides pauvres en métaux Title:
    Detailed study of cold metal-poor stars;
Authors: Magain, Pierre
Bibcode: 1984PhDT.......162M
Altcode:
  No abstract at ADS

Title: A Test of the Planck-Larkin Partition Function
Authors: Magain, P.
Bibcode: 1984LIACo..25..234M
Altcode: 1984trss.conf..234M; 1984tpss.conf..234M
  No abstract at ADS

Title: The A1/Mg abundance ratio in halo stars.
Authors: Arpigny, C.; Magain, P.
Bibcode: 1983A&A...127L...7A
Altcode:
  The Al to Mg abundance ratio is redetermined in two extreme metal-poor
  stars, HD 19445 and HD 140283, on the basis of accurate spectral
  material. It is found that: (1) one of the two lines used for the
  Al abundance determination is blended by CH lines; (2) no anomalous
  difference appears between the hotter and the cooler star, both showing
  an Al overdeficiency; (3) the observations are in fair agreement with
  predictions from the theory of explosive carbon burning.

Title: The missing UV opacity and the colours of solar-type stars.
Authors: Magain, P.
Bibcode: 1983A&A...122..225M
Altcode:
  A simple method is proposed to take into account the "missing UV
  opacity" in solar-type stars. It is shown that the mere inclusion of
  that UV opacity through a very simple formula is sufficient to bring
  the theoretical colours in agreement with observed ones for stars of
  different metal abundances and belonging to the spectral range from
  mid-F to late-G. Synthetic colours computed in the Geneva and UBV
  systems reproduce the various observed relations satisfactorily. The
  relations based on these colours allow reliable estimates of effective
  temperatures, surface gravities and metal abundances of stars. In
  addition, solar colours are obtained and three more solar twin
  candidates are proposed.

