Author name code: muench
ADS astronomy entries on 2022-09-14
author:"Munch, Guido" 
------------------------------------------------------------------------  

Title: Capturing Software Citations in Astronomy and Planetary
    Sciences
Authors: Henneken, E. A.; Muench, G.; Holm Nielsen, L.;
   Blanco-Cuaresma, S.; Accomazzi, A.
Bibcode: 2019LPI....50.1569H
Altcode:
  This poster discusses the importance of capturing software citations
  and how this has been implemented in the Asclepias project of the AAS,
  ADS, and Zenodo.

Title: Turbulence in the Interstellar Medium: a Retrospective Review
Authors: Münch, Guido
Bibcode: 1999intu.conf....1M
Altcode:
  No abstract at ADS

Title: The Universe at Large
Authors: Münch, Guido; Mampaso, Antonio; Sánchez, Francisco
Bibcode: 1997unla.book.....M
Altcode:
  The Universe at Large presents a unique survey of key questions
  outstanding in contemporary astronomy and cosmology. In this
  timely volume, eleven of the world's greatest living astronomers and
  cosmologists present personal views of what problems must be addressed
  by future research. Allan Sandage presents a 23-point plan to reach
  a full understanding of the large-scale structure in the Universe;
  Geoffrey Burbidge looks at the future of the Quasi Steady State
  alternative to the Big Bang; E. Margaret Burbidge, Donald Osterbrock
  and Malcolm Longair discuss active galactic nuclei (AGN); Igor Novikov,
  Donald Lynden-Bell, Martin Rees and Rashid Sunyaev look at the physics
  of black holes; and Bernard Pagel and Hubert Reeves concentrate on
  what we don't yet understand about elements in the cosmos. This book
  provides a unique review of our current understanding in astronomy
  and cosmology and a host of profitable research ideas for graduate
  students and researchers.

Title: The Universe at Large
Authors: Münch, Guido; Mampaso, Antonio; Sánchez, Francisco
Bibcode: 1997ual..book.....M
Altcode:
  Preface; 1. Astronomical problems for the next three decades
  Allan Sandage; 2. New vistas in cosmology and cosmogony Geoffrey
  Burbidge; 3. Omega, dark mass and galactic history Donald Lynden-Bell;
  4. Observations of QSOs which are critical for cosmology E. Margaret
  Burbidge; 5. Nature, structure, refuelling and evolution of AGNs
  Donald Osterbrock; 6. The high energy radiation of active galactic
  nuclei Malcolm S. Longair; 7. Physics and astrophysics of black holes
  Igor Novikov; 8. Galaxy formation and quasars - progress and prospects
  Martin J. Rees; 9. Cosmic abundances Bernard E. J. Pagel; 10. Clues
  to early development of galaxies Hubert Reeves; 11. The observational
  appearance of accreting black holes in X-ray binaries Rashid Sunyaev;
  12. Reflections on the key problems Malcolm S. Longair; Index.

Title: The Universe at large. Key issues in astronomy and cosmology.
Authors: Münch, G.; Mampaso, A.; Sánchez, F.
Bibcode: 1997ualk.book.....M
Altcode:
  This book provides a unique review of our current understanding in
  astronomy and cosmology, and a host of ideas for profitable future
  research.

Title: Obituary: Jerome Kristian, 1934-1996
Authors: Munch, Guido
Bibcode: 1997BAAS...29.1476M
Altcode:
  No abstract at ADS

Title: The Universe at Large, Key Issues in Astronomy and Cosmology
Authors: Munch, Guido; Mampaso, Antonio; Sánchez, Francisco
Bibcode: 1997ulki.book.....M
Altcode:
  The Universe at Large presents a unique survey of key questions
  outstanding in contemporary astronomy and cosmology. In this
  timely volume, eleven of the world's greatest living astronomers
  and cosmologists present their personal views of what problems must
  be addressed by future research. Allan Sandage presents a 23-point
  plan to reach a full understanding of the largescale structure in
  the Universe; Geoffrey Burbidge looks at the future of the Quasi
  Steady State alternative to the Big Bang; active galactic nuclei
  (AGN) are discussed by E. Margaret Burbidge, Donald Osterbrock and
  Malcolm Longair; Igor Novikov, Donald Lynden-Bell, Martin Rees and
  Rashid Sunyaev look at the physics of black holes; and Bernard Pagel
  and Hubert Reeves concentrate on what we don't yet understand about
  elements in the cosmos. This book provides a unique review of our
  current understanding in astronomy and cosmology, and a host of ideas
  for profitable future research - for graduate students and researchers.

Title: Complex interstellar absorption lines of C_2_ in the Cygnus
    OB association
Authors: Gredel, R.; Muench, G.
Bibcode: 1994A&A...285..640G
Altcode:
  Measurements of interstellar absorption lines in the (1,0) band of
  the C_2_ Phillips system, around 1.015 μm, are reported for the
  stars Nos. 12 and 5 of the Cyg OB2 association. The R(0), Q(2), and
  Q(4) lines, at a resolving power of 65,000, show a complex structure,
  with four discrete components in No. 12 and three in No. 5. The radial
  velocities of the various components, spread over a range of 22 km/s ,
  agree in both stars, suggesting their origin in similar spatio-kinematic
  structures. The relative intensities between the various components are
  not the same in the two stars, but the net C_2_ column densities derived
  for the two stars result nearly proportional to their respective B-V
  color excesses, as it has been found in stars of smaller reddening. A
  typical clump of absorbing gas, in the close neighborhood or within
  the association, has been characterized by an upper limit of 5 pc in
  linear dimensions and a mass of 200 M<SUB>sun</SUB>_. The low emission
  of the association in the free-free radio continuum is suggested to
  be a result of the removal of HII-gas by the powerful winds known to
  be emitted by its members.

Title: Detection of Hα Emission on High Velocity 21-CENTIMETER Clouds
Authors: Muench, Guido; Pitz, Eckhart
Bibcode: 1990IAUS..139..193M
Altcode:
  The measurement of H-alpha emission on two high galactic latitude clouds
  known to emit 21 cm lines with local standard of rest velocities of -50
  and -85 km/s is reported. The H-alpha lines have been found nearly at
  the velocities of the 21 cm features and have emission rates of 0.2
  Rayleigh. The diffuse Lyman continuum intensity required to produce
  H I ionization at the measured rate is in agreement with the direct
  measurements made with the ultraviolet spectrometer of the Voyager
  2 spacecraft.

Title: Highly excited molecular hydrogen in M 42 and other nebulae.
Authors: Hippelein, H. H.; Muench, G.
Bibcode: 1989A&A...213..323H
Altcode:
  Measurements of the S(5), S(7), S(10), and S(11) quadrupole lines of
  the (2,0) band of H2 in the Orion Nebula (M 42) are presented. These
  measurements showed the following features: (1) the radial velocity
  characteristics consistent with those of microwave lines emitted by the
  Orion Molecular Cloud (OMC); (2) an intrinsic line width of 4.7 km/sec,
  exceeding that measured in microwave lines; (3) a surface brightness
  distribution in S(11) with a nearly circular symmetry around and a
  maximum at the Trapezium; (4) and a net column density of vibrationally
  excited H2 that can be accounted for by fluorescent excitation models
  with parameters appropriate for the OMC. A rotational temperature of
  about 11,000 K was observed, in excess of that predicted by radiative
  excitation.

Title: H<SUB>α</SUB>-emission in directions toward high velocity
    21cm clouds
Authors: Münch, Guido; Pitz, Eckhart
Bibcode: 1989LNP...350..373M
Altcode: 1989IAUCo.120..373M; 1989sdim.conf..373M
  Measurements of H<SUB>α</SUB>-emission in fields known to emit 21cm
  radiation at intermediate and high velocities are presented. The
  observations are partial results of a survey being carried out at
  the Calar Alto Observatory with a dedicated Fabry-Perot spectrometer
  of 15cm aperture, providing velocity and angular resolutions of 11km
  s<SUP>-1</SUP> and 0.5 deg<SUP>2</SUP>. The limited material available
  indicates that the H<SUB>α</SUB>-emission, when detected at a radial
  velocity nearly the same as that measured in 21cm, appears more extended
  in the sky than the HI-radiation.

Title: Highly excited molecular hydrogen in orion
Authors: Hippelein, Hans H.; Münch, Guido
Bibcode: 1989LNP...350..323H
Altcode: 1989IAUCo.120..323H; 1989sdim.conf..323H
  No abstract at ADS

Title: Rotational structure of the (2, 0) Phillips band of C2 in
    Comet P/Halley
Authors: Appenzeller, I.; Muench, G.
Bibcode: 1987A&A...187..465A
Altcode:
  The results of the study of a digital echellogram of the nuclear region
  of comet Halley, containing the (2,0) Phillips band of C<SUB>2</SUB>
  fully resolved, are presented. The intensities of individual lines,
  measured from the R-branch head up to R36, Q30, and P24, indicate a very
  high degree of rotational excitation. The population of the levels from
  where the lines arise, when approximated by a Boltzmann distribution,
  is found to be characterized by a temperature higher than that obtained
  from the Swan bands in other comets. An absolute calibration of the
  line fluxes has been obtained from narrow band CCD-imagery, to make
  feasible their comparison with measurements in the Swan system,
  probably carried out by other observers of comet Halley.

Title: Photometry of comet P/Halley at near post-perihelion phases
Authors: Neckel, T.; Muench, G.
Bibcode: 1987A&A...187..581N
Altcode:
  Photometric measurements of Halley's comet at phases around its recent
  perigee are presented. Narrow band filters isolating the C<SUB>2</SUB>
  Swan band emission and a neighboring continuum, besides the standard
  UBV, have been used with 4 nucleus centered field stops subtending
  angles between 41arcsec and 1050arcsec. The brightness fluctuations
  detected, especially conspicuous in C<SUB>2</SUB> and the nearby
  continuum, indicate a period of 7.3 days. Some evidence for the double
  peaked nature of the periodic variation is marginally present.

Title: Geschwindigkeits-Schnitte von Planetarischen Nebeln
Authors: Hippelein, H.; Münch, G.
Bibcode: 1987MitAG..68..258H
Altcode:
  No abstract at ADS

Title: GIOTTO Flights Dynamics Report No. 1 part 4
Authors: Morley, Trevor A.; Hechler, Friedhelm; Münch, G.
Bibcode: 1986gfd..rept....4M
Altcode:
  Details of the Orbit determination of Comet Halley during the GIOTTO
  Flyby in March 1986 are discussed

Title: Periodic Comet Halley (1982i)
Authors: Munch, G.; Hippelein, H.; Hessmann, F.; Gredel, R.; Celnik,
   W. E.; Schulz, R.; Weissbauer, K.; West, R. M.; Pedersen, H.; Gelly,
   B.; Le Bertre, T.; Sheffer, Y.; Fleet, R.; Bennett, J. C.; Campos, J.
Bibcode: 1986IAUC.4183....1M
Altcode:
  G. Munch, H. Hippelein, F. Hessmann and R. Gredel, Max-Planck- Institut
  fur Astronomie, report measurements of [C I] 985-nm emission with
  the 1.2-m telescope of the Calar Alto Observatory and a 2-etalon
  spectrometer at 0.04-nm resolution in field integrated mode. On
  1985 Dec. 14, through a 2' stop centered on the nucleus, an emission
  rate of E = 8 +/- 1 Ray and a radial velocity within 1 km/s of the
  ephemeris value (IHW orbit No. 22) were found. At 4' tailward from
  the nucleus E ~ 2 Ray, only 5 percent of that in airglow OH(3,0)P2(2)
  at 984.848 nm. The corresponding metastable production rate along
  the sampled nucleus centered column is Q = 10**26.7/s. Essentially
  the same results were found on Dec. 22. W. E. Celnik, R. Schulz and
  K. Weissbauer, European Southern Observatory, report tail lengths on
  Feb. 20.4 UT of 59' (red), 20' (blue), 40' (CO+) and 33' (CN), and an
  intense antitail in p.a. 90. On Feb. 21.4 the tail lengths were 2.5 deg
  (red), 4.3 deg (blue), 2.6 deg (CO+) and 0.75 deg (CN). On Feb. 22.4
  there were ion tails in p.a. 106 and 92, and dust tails in p.a. 65,
  50, 34, 358 and 322; maximum tail lengths were 4.1 deg (red, blue),
  1.8 deg (CO+) and 0.57 deg (CN). On Feb. 24.4 the CO+ tail length was
  9.2 deg; a bright CO+ core of diameter 15" was embedded in a faint,
  diffuse coma 9'2 in diameter; in red light concentric bow shocks were
  detected at distances 14", 60" and 140" from the core. CCD observations
  by R. M. West, H. Pedersen and B. Gelly on Feb. 23 showed the tail
  structure reported on IAUC 4179 changed as follows: 1, broad, diffuse
  to 75' in p.a. 270, strong kink at 225, maximum length 240', additional
  sharp loop to south 45' in 260; 2, stong, diffuse, to 130' in 277;
  3, diffuse to 100' in 286; 4, diffuse to 135' in 317; 5, diffuse,
  stubby, to 100' in 333; 6, strong, narrow to 95' in 0 at west edge
  of broad, diffuse, with other extreme 55' in 30; 7, sharp edge to 25'
  in 67. T. le Bertre reports that infrared photometry shows variations
  of up to 1.5 mag from day to day; representative are the data in L
  (diaphragm 30", uncertainty generally 0.05 mag): Feb. 16.4 UT, -0.19;
  17.4, +0.74; 18.4, -0.73; 19.4, +0.16; 20.4, -0.54; 22.4, +0.37;
  23.4, +0.04. Total visual magnitude estimates: Feb. 21.51 UT, 3.0
  (Y. Sheffer, Austin, TX, 7 x 50 binoculars); 22.13, 3.9 (R. Fleet,
  Harare, Zimbabwe, 11 x 80 binoculars); 23.11, 3.5 (Fleet); 24.10, 3.0
  (J. C. Bennett, Pretoria, South Africa, 0.13-m refractor); 25.11, 3.0
  (J. Campos, Durban, South Africa, 0.13-m refractor).

Title: Interstellar molecular carbon in distant supergiants.
Authors: Gredel, R.; Muench, G.
Bibcode: 1986A&A...154..336G
Altcode:
  The results of a search for interstellar C<SUB>2</SUB> lines in
  the spectrum of southern reddened supergiants are reported. The
  C<SUB>2</SUB> excitation parameters along the lines of sight to
  HD 169454 and BD -14°5037, both in the Sct OB3 association, have
  been determined. Radiative excitation effects of high rotational
  levels were found in HD 169454. The C<SUB>2</SUB> lines in BD
  -14°5037 are clearly double. A spectrum of HD 92693, in Car OB1,
  shows C<SUB>2</SUB> lines weak in proportion to its color excess
  E<SUB>B-V</SUB>, but otherwise the column densities N(C<SUB>2</SUB>)
  for all stars so far observed appear linearly correlated to
  E<SUB>B-V</SUB>. Through the known relation of E<SUB>B-V</SUB> with
  molecular hydrogen column density N(H<SUB>2</SUB>), a mean columnar
  abundance N(C<SUB>2</SUB>)/N(H<SUB>2</SUB>) = 3.0×10<SUP>-8</SUP>
  has been estimated, which agrees with theoretical predictions for the
  C<SUB>2</SUB> abundance in dense molecular clouds.

Title: GIOTTO Flights Dynamics Report No. 1 part 3
Authors: Morley, Trevor A.; Hechler, Friedhelm; Münch, G.
Bibcode: 1986gfd..rept....3M
Altcode:
  Details of the Orbit determination of Comet Halley for the GIOTTO
  Flyby in March 1986 are discussed

Title: Die Linien der 2-0 Vibrationsbande des molekularen Wasserstoffs
    im Orion-Nebel
Authors: Hippelein, H. H.; Münch, G.
Bibcode: 1986MitAG..67..358H
Altcode:
  No abstract at ADS

Title: Internal Dust in H II Regions
Authors: Münch, G.
Bibcode: 1985MitAG..63...65M
Altcode:
  A review is given of the observable effects that scattering dust
  internal to H II-regions may have on their characteristic visual
  spectrum. The intrinsic color of optically thin lines is discussed, with
  special reference to the Balmer decrement. The effects of scattering
  on the transmission of line radiation formed in the deep interior of
  H II-regions is considered. Recent observations of He I λλ10829-30
  emission line profiles in M42 are discussed, together with their
  interpretation through radiative transfer calculations. Absorption
  line observations of He I λλ10829-30 on θ<SUP>1</SUP>Ori C and
  θ<SUP>2</SUP>Ori A are presented and discussed in relation to the
  corresponding emission lines.

Title: Internal reddening of H II-regions and HH-objects, with
    special reference to NGC 896(W3).
Authors: Gomez Garrido, P.; Muench, G.
Bibcode: 1984A&A...139...30G
Altcode:
  The effect of scattering by dust internal to H II regions on their
  spectral characteristics has been studied on the basis of simple
  analytical models, for assumed universal optical parameters of the
  dust. A procedure to determine the external interstellar extinction
  and the internal gas to dust abundance ratio of H II regions has been
  developed and applied as a test to the Orion Nebula. Newly acquired
  observations of the H II region NGC 896 have been analyzed to identify
  the effects of internal dust on its spectrum and to establish its
  relationship to the background radio source W3 (cont.). Finally, the
  effects that the probable existence of scattering dust internal to
  HH-objects might have on the color of their spectrum has been included.

Title: GIOTTO Flights Dynamics Report No. 1 part 2
Authors: Morley, Trevor A.; Hechler, Friedhelm; Münch, G.
Bibcode: 1984gfd..rept....2M
Altcode:
  Details of the observation strategy and Orbit determination of Comet
  Halley for the GIOTTO Flyby in March 1986 are discussed

Title: Detection of H2 emission at 1.064 MU M in the Orion Nebula.
Authors: Muench, G.; Hippelein, H.; Pitz, E.
Bibcode: 1984A&A...135L..11M
Altcode:
  Emission of H<SUB>2</SUB> in the S7 line of the (2,0) band at 1.064
  μm, from regions of M42 emitting H<SUB>2</SUB> lines in the IR, is
  reported. The line profile is asymmetric, with an extended violet
  wing, similar to that of (1,0)S1 at 2.1 μm. Regions not emitting
  (1,0)S1 show a sharp symmetric line centered at the wavelength
  expected for H<SUB>2</SUB>(2,0)S7, which is, nevertheless, considered
  as unidentified. The extinction optical depth at (1,0)S1, derived from
  a comparison of its violet shifted flux with that at S7, is nearly in
  agreement with the value obtained from IR data, when the scattering
  of S7 radiation by internebular dust is taken into account. It is
  estimated that over 60% of the measured (2,0)S7 emission has undergone
  scattering in its transport through the nebula.

Title: GIOTTO Flights Dynamics Report No. 1 part 1
Authors: Morley, Trevor A.; Hechler, Friedhelm; Münch, G.
Bibcode: 1984gfd..rept....1M
Altcode:
  Details of the Orbit determination of Comet Halley for the GIOTTO
  Flyby in March 1986 are discussed

Title: The Effects of Scattering by Internal Dust on the Spectra of
    Emission Nebulae
Authors: Munch, G.
Bibcode: 1983RMxAA...7..229M
Altcode:
  No abstract at ADS

Title: NGC 2359 : the HII-region driven by the WR-star HD 56925.
Authors: Goudis, C.; Hippelein, H.; Muench, G.
Bibcode: 1983A&A...117..127G
Altcode:
  The results of a kinematic study of NGC 2359, from 21 interferometric
  profiles of [O III] λ5007 and [N II] λ6583, are presented. All
  profiles share a component at V<SUB>LSR</SUB>=54 km s<SUP>-1</SUP>,
  identified with the systemic velocity. Over the central core, [O III]
  shows components at ±30 km s<SUP>-1</SUP> from the centroid, not
  seen in [N II]. The relative intensities of the displaced components
  indicates their origin in tenuous gas seen pervading bright filaments,
  which move nearly with the systemic velocity. It is proposed that the
  tenuous gas is an expanding shell driven by the stellar wind from the
  exciting WR-star, while the filaments are post-shock manifestations of
  density fluctuations in the external medium overrun by the shell. The
  problems offered by the joint interpretation of optical and microwave
  CO line data are reconsidered and possible avenues to their solution
  are suggested.

Title: Der Cassegrain-Doppelspektrograph für das 3.5m-Teleskop
Authors: Solf, J.; Münch, G.
Bibcode: 1983MitAG..60..473S
Altcode:
  No abstract at ADS

Title: Physik-Nobelpreis 1983 für W. A. Fowler und S. Chandrasekhar.
Authors: Münch, G.
Bibcode: 1983S&W....22R.572M
Altcode:
  No abstract at ADS

Title: Physik-Nobelpreis 1983 für S. Chandrasekhar und W. A. Fowler.
Authors: Münch, G.
Bibcode: 1983S&W....22Q.572M
Altcode:
  No abstract at ADS

Title: Observations of forbidden C I emission in Orion A (M42)
    and Orion B (NGC 2024)
Authors: Munch, G.; Hippelein, H.
Bibcode: 1982NYASA.395..170M
Altcode:
  A map of Orion A in radiation of forbidden C I wavelength 9850, with
  a resolution of 80 arcsec, down to a level of intensity 20 Ray, is
  obtained. The brightness distribution in forbidden C I is found to
  be flatter than that in H-alpha, with the apparent intensity ratio
  forbidden C I/H-alpha varying between 0.006-0.0004. A similar map of
  Orion B, with a resolution of 2 arcmin, down to a level of 7 Ray, is
  found to demonstrate that the visually conspicuous central obscuration
  lane, behind which the maximum continuum radio emission arises, appears
  to be bright in forbidden C I. A high-resolution profile of forbidden
  C I wavelength 9850 in Orion A indicates that its FWHM is 6.1 km/s,
  significantly smaller than that of any other nonradio nebular line. It
  is concluded that the forbidden C I emission likely arises either by
  recombination in cool C II regions or by being excited by shocks.

Title: Max-Planck-Institut für Astronomie, D-6900
    Heidelberg-Königstuhl, Federal Republic of Germany. Centro
    Astronómico Hispano-Alemán, Almeria, Spain. Report for the period
    1 January - 31 December 1980.
Authors: Münch, G.
Bibcode: 1982BAAS...14..279M
Altcode:
  No abstract at ADS

Title: S 106 - an H II-region driven by a stellar wind
Authors: Hippelein, H.; Muench, G.
Bibcode: 1981A&A....99..248H
Altcode:
  High resolution interferometric observations of the forbidden S
  III 9531 A line emitted by the peculiar emission nebula S 106 are
  presented. Observations were carried out with a Fabry-Perot scanner
  attached to the 1.2 m telescope of the Calar Alto Observatory in
  June and October 1979. Obtained profiles are broad, some covering a
  radial velocity range exceeding 100 km/s, and asymmetric around their
  peak intensity. Profiles in the north emission lobe show an excess
  of positive over negative velocity, while those in the south lobe
  exhibit the reverse asymmetry; velocity centroids define a kinematic
  distance between 0.5 and 1.0 kpc. Measured line intensities and 6-cm
  flux densities show the line formation path length to be 1/100 of the
  nebular dimensions on the plane of the sky. It is suggested that the
  nebular spectrum originates in a thin layer of gas confined by stellar
  wind from the exciting star to the surface of a two-lobe cavity. The
  nearly symmetric appearance of the nebula is attributed to the density
  distribution prevailing within the disk-like complex of interstellar
  matter in which the single exciting star was formed.

Title: Wavelengths and profiles of the (SIII) 3p2,1-1d2 lines in
    some emission nebula.
Authors: Hippelein, H.; Muench, G.
Bibcode: 1981A&A....95..100H
Altcode:
  High resolution profiles of the nebular (S III) forbidden lines
  in the integrated light of a number of bright emission nebulae are
  presented. The radial velocities of the objects, determined in the
  past with slit spectrographs, have been adopted to transform apparent
  wavelengths of the profiles' centroids to the laboratory system. The
  strongest line 3P2-1D has been found 0.8 A bluewards from the wavelength
  predicted from term values.

Title: Scientific results from the pioneer Saturn infrared radiometer
Authors: Orton, G. S.; Ingersoll, A. P.; Froidevaux, L.; Neugebauer,
   G.; Munch, G.; Chase, S. C.
Bibcode: 1981AdSpR...1h.179O
Altcode: 1981AdSpR...1..179O
  The Pioneer 11 Infrared Radiometer instrument made observations of
  Saturn and its rings in broadband channels centered at 20 and 45 μm
  and obtained whole-disk information on Titan. A planetary average
  effective temperature of 96.5+/-2.5 K implies a total emission 2.8
  times the absorbed sunlight. Correlation with radio science results
  implies that the molar fraction of H<SUB>2</SUB> is 90+/-3% (assuming
  the rest is He). Temperatures at the 1 bar level are 137 to 140 K;
  regions appearing cooler may be overlain by a cloud acting as a 124
  K blackbody surface. A minimum temperature averaging 87 K is reached
  near 0.06 bars. Ring boundaries and optical depths are consistent
  with those at optical wavelengths. Ring temperatures are 64-86 K on
  the south (illuminated) side, ~54 K on the north (unilluminated) side,
  and at least 67 K in Saturn's shadow. There is evidence for a south to
  north drop in ring temperatures. Titan's 45 μm brightness temperature
  is 75+/-5 K.

Title: Max-Planck-Institut für Astronomie, D-6900
    Heidelberg-Königstuhl, Federal Republic of Germany. Centro
    Astronómico Hispano-Alemán, Almeria, Spain. Report for the period
    1 January - 31 December 1979.
Authors: Münch, G.
Bibcode: 1981BAAS...13Q.226M
Altcode:
  No abstract at ADS

Title: Max-Planck-Institut für Astronomie, D-6900
    Heidelberg-Königstuhl, Federal Republic of Germany. Centro
    Astronómico Hispano-Alemán, Almeria, Spain. Report for the period
    1 January to 31 December 1979.
Authors: Münch, G.
Bibcode: 1981BAAS...13R.226M
Altcode:
  No abstract at ADS

Title: Metallarme Subdwarfs der Spektraltypen F und G
Authors: Gehren, T.; Hippelein, H.; Münch, G.
Bibcode: 1981MitAG..52...68G
Altcode:
  No abstract at ADS

Title: Scientific results from the Pioneer Saturn Infrared Radiometer.
Authors: Orton, G. S.; Ingersoll, A. P.; Froidevaux, L.; Neugebauer,
   G.; Münch, G.; Chase, S. C.
Bibcode: 1981ppe..conf..179O
Altcode:
  No abstract at ADS

Title: Das Fabry-Perot-Interferometer des MPI für Astronomie
Authors: Hippelein, H.; Münch, G.
Bibcode: 1981MitAG..54..193H
Altcode:
  No abstract at ADS

Title: A study of the Jovian forbidden line S II nebula at high
    spectral resolution
Authors: Trauger, J. T.; Muench, G.; Roesler, F. L.
Bibcode: 1980ApJ...236.1035T
Altcode:
  Observations of forbidden line S II 6716-6731 A emissions from the
  Jovian magnetosphere have been carried out with a PEPSIOS spectrometer
  at the Hale 5 m telescope. Spectral resolving power was sufficient to
  resolve the forbidden line S II line widths. From measured 6716-6731
  A doublet ratios and spectral line widths a thermal plasma is found
  characterized by temperatures about 2 x 10 to the 4th K and electron
  densities about 2000 cu cm. The source of forbidden line S II emissions
  was centered within a toroidal region of radius 5 Jupiter radii
  (inside the orbit of Io), with tight latitudinal confinement near the
  equilibrium equator for ions in the tilted corotating Jovian magnetic
  field, and significant long-lived longitudinal structure.

Title: Saturn's Atmosphere and Energy Balance, Ring Temperatures,
    and Detection of Titan by the Pioneer Saturn Infrared Radiometer
Authors: Ingersoll, A. P.; Orton, G. S.; Neugebauer, G.; Munch, G.;
   Chase, S.
Bibcode: 1980BAAS...12..435I
Altcode:
  No abstract at ADS

Title: The effects of seeing on the reflected spectrum of Uranus
    and Neptune
Authors: Munch, G.; Hippelein, H.
Bibcode: 1980A&A....81..189M
Altcode:
  The results of a redetermination of the rotational periods of Uranus
  and Neptune, based on spectrograms obtained with the coude spectrograph
  of the 5 m Hale telescope, are presented. The effects of image motion
  on the shape of the spectral lines reflected by a planet rotating as
  a solid body and coherently scattering solar light, has been studied
  analytically. A general relation between the seeing transformed
  velocities at any point on the disk and those at the equator is
  established. It is shown that, for the case of Gaussian seeing, the
  brightness continuum of the smeared disk contains all the information
  required to derive the shape of the reflected lines. The shift, change
  in r.m.s. width, and asymmetry of the seeing transformed lines at the
  equator have been numerically evaluated for the brightness distribution
  of Uranus determined from Stratoscope II.

Title: Pioneer Saturn Infrared Radiometer: Preliminary Results
Authors: Ingersoll, A. P.; Orton, G. S.; Munch, G.; Neugebauer, G.;
   Chase, S. C.
Bibcode: 1980Sci...207..439I
Altcode:
  The effective temperature of Saturn, 94.4 + 3 K, implies a total
  emission greater than two times the absorbed sunlight. The infrared
  data alone give an atmospheric abundance of H<SUB>2</SUB> relative to
  H<SUB>2</SUB> + He of 0.85 ± 0.15. Comparison of infrared and radio
  occultation data will give a more precise estimate. Temperature at the
  1-bar level is 137 to 140 K, and 2.5 K differences exist between belts
  and zones up to the 0.06-bar level. Ring temperatures range from 60 to
  70 K on the south (illuminated) side and from &lt; 60 to 67 K in the
  planet's shadow. The average temperature of the north (unilluminated)
  side is ~ 55 K. Titan's 45-micrometer brightness temperature is 80 ±
  10 K.

Title: Max-Planck
Authors: Munch, G.
Bibcode: 1980BAAS...12..241M
Altcode:
  No abstract at ADS

Title: A Study of the Jovian [SII] and [SIII] Nebulae at High
    Spectral Resolution.
Authors: Trauger, J. T.; Munch, G.; Roesler, F.
Bibcode: 1979BAAS...11..591T
Altcode:
  No abstract at ADS

Title: Solar System Studies - Jupiter Imaging at 5-MICRONS - Jupiter
    Magnetosphere - Infrared Observations of Planets - Diameter of Pluto
Authors: Kowal, C.; Goldreich, P.; Terrile, R. J.; Westphal, J.;
   Trauger, J.; Munch, G.; Roesler, F. L.; Soifer, B. T.; Matthews, K.;
   Neugebauer, G.; Sargent, W. L. W.; Boksenberg, A.; Arnold, S. J.
Bibcode: 1979haob.rept..721K
Altcode:
  No abstract at ADS

Title: Guest Investigators
Authors: Madore, B. F.; Mekler, Y.; Miller, H. R.; Munch, G.;
   Hippelein, H. H.; Ney, E. P.; Hatfield, B. J.; Peach, J. V.; Godwin,
   J. G.; Dixon, K. L.; Pesch, P.; Phillips, M. M.; Rubin, V. C.;
   Burstein, D.; Shoemaker, E. M.; Helin, E. F.; Shorthill, R. W.;
   Smith, D. W.; Johnson, P. E.; Simkin, S. M.; Szkody, P.; Ulrich,
   R. K.; Usher, P. D.; van den Bergh, S.
Bibcode: 1979haob.rept..788M
Altcode:
  No abstract at ADS

Title: High-velocity Features in M 42 Driven by Stellar Winds
Authors: Taylor, K.; Munch, G.
Bibcode: 1978A&A....70..359T
Altcode:
  Summary. Interferometric Hoc and [N ii] line profiles for areas of M 42
  near 62 Ori A, containing small scale cloudlets with enhanced emission,
  are presented. The supersonic velocities, with respect to the nebula,
  found for the cloudlets are ascribed to shocks driven by the stellar
  wind emitted by 62 Ori A. The similarity solution for the equations
  describing the flow of a stellar wind through a uniform H il-medium
  has been generalized to allow for the presence of small scale density
  inhomogeneities. The short dynamical time scale, 400 yr, determined by
  the measured positions and velocities of the cloudlets, is interpreted
  as a manifestation of the variability of the pressure exerted by the
  shocked stellar wind. Key words: emission nebulae - stellar winds

Title: Neutral carbon emission in M42.
Authors: Hippelein, H.; Muench, G.
Bibcode: 1978A&A....68L...7H
Altcode:
  The detection and measurement of the forbidden C I lines at 9850
  and 8727 A emitted by the Orion Nebula are reported. Typical values
  for the electron density needed to excite the lines collisionally
  in the H II-H I transition layers and for the neutral carbon column
  density are evaluated. The carbon ionization equilibrium is accounted
  for by invoking the predominance of charge exchange over radiative
  processes. Implications for the topology of the transition layers
  are suggested.

Title: A redetermination of the Uranus rotation period.
Authors: Trauger, J. T.; Roesler, F. L.; Muench, G.
Bibcode: 1978ApJ...219.1079T
Altcode:
  The rotation velocity of Uranus has been measured by a comparison
  of spectroscopic profiles for the 5281.8 A Fraunhofer line reflected
  from Uranus and the moon. This method yields a rotation velocity which
  is insensitive to atmospheric seeing conditions. Our value for the
  equatorial velocity is 3.5 + or - 0.4 km/sec.

Title: High Resolution Measurement of Neutral Carbon Emission Lines
    in the Orion Nebula
Authors: Hippelein, H. H.; Münch, G.
Bibcode: 1978hrs..conf..394H
Altcode:
  No abstract at ADS

Title: Angular Dimension of the Circumstellar Envelope of µ Cephei
    Measured with a Pepsios Spectrometer
Authors: Münch, G.; Roesler, F.; Trauger, J.
Bibcode: 1978hrs..conf..660M
Altcode:
  No abstract at ADS

Title: (Abstract) Does Jupiter Have a "Mini-Corona"?
Authors: Munch, G.; Roesler, F.; Trauger, J.
Bibcode: 1977PASP...89..619M
Altcode:
  No abstract at ADS

Title: A search for the H<SUB>2</SUB> (3,0) S1 line in the spectrum
    of Titan.
Authors: Muench, G.; Trauger, J. T.; Roesler, F. L.
Bibcode: 1977ApJ...216..963M
Altcode:
  Results are reported for measurements of the quadrupole S1 line of the
  (3, 0) absorption band of H2 in spectra of Titan, which were performed
  at an effective resolution of 0.09 A by scanning with a PEPSIOS
  spectrometer over a range of 0.85 A centered at the expected position
  of the investigated line and sampling in 80 contiguous channels. No
  statistically significant H2 (3, 0) S1 feature is found in the spectra,
  but a three-sigma upper limit of 3 mA is set for the equivalent width
  of the S1 line that might be present in a co-added spectrum. It is
  concluded that these measurements do not provide any evidence for the
  presence of H2 in the atmosphere of Titan.

Title: Study of Jupiter's Corotating SII Nebula at High Spectral
    Resolution
Authors: Munch, G.; Trauger, J. T.; Roesler, F. L.
Bibcode: 1977BAAS....9..465M
Altcode:
  No abstract at ADS

Title: Io: morphology of its sodium emission region.
Authors: Muench, G.; Bergstralh, J. T.
Bibcode: 1977PASP...89..232M
Altcode:
  Results of experiments carried out to obtain two-dimensional images of
  the sodium emission region associated with Io are presented. Through
  multislit spectrograms and Perot-Fabry interferograms, the dependence
  of the Na-emission distribution on Jupiter's magnetic field is
  demonstrated. The time scale of the observed changes in the Na emission
  is shown to require electron fluxes in the Jovian magnetosphere one
  order of magnitude larger than those obtained by an extrapolation of
  the proton fluxes measured in situ from the Pioneer 10 spacecraft.

Title: Herbig-Haro object in the Orion Nebula.
Authors: Munch, G.
Bibcode: 1977ApJ...212L..77M
Altcode:
  Spectral and kinematic characteristics are reported for a double
  Herbig-Haro object originally observed in forbidden O I 6300-A emission
  in the Orion Nebula (M42). Spectral observations in forbidden lines
  of O I and S II indicate that one component has a heliocentric radial
  velocity of -240 km/s and the other component exhibits no significant
  velocity shift relative to the lines of M42. Rough estimates of some
  parameters of the two components are offered as evidence in favor
  of the hypothesis that the spectra of all Herbig-Haro objects are
  shock-excited.

Title: Infrared Thermal Mapping of the Martian Surface and Atmosphere:
    First Results
Authors: Kieffer, H. H.; Martin, T. Z.; Chase, S. C., Jr.; Miner,
   E. D.; Palluconi, F. D.; Muench, G.; Neugebauer, G.
Bibcode: 1976Sci...193..780K
Altcode:
  The Viking infrared thermal mapper measures the thermal emission of the
  martian surface and atmosphere and the total reflected sunlight. With
  the high resolution and dense coverage being achieved, planetwide
  thermal structure is apparent at large and small scales. The thermal
  behavior of the best-observed areas, the landing sites, cannot
  be explained by simple homogeneous models. The data contain clear
  indications for the relevance of additional factors such as detailed
  surface texture and the occurrence of clouds. Areas in the polar night
  have temperatures distinctly lower than the CO<SUB>2</SUB> condensation
  point at the surface pressure. This observation implies that the annual
  atmospheric condensation is less than previously assumed and that
  either thick CO<SUB>2</SUB> clouds exist at the 20-kilometer level or
  that the polar atmosphere is locally enriched by noncondensable gases.

Title: Mariner 10 Infrared Radiometer Results: Temperatures and
    Thermal Properties of the Surface of Mercury
Authors: Chase, S. C., Jr.; Miner, E. D.; Morrison, D.; Muench, G.;
   Neugebauer, G.
Bibcode: 1976Icar...28..565C
Altcode: 1976IAUCo..34..565C
  Mariner 10 infrared brightness temperatures of the surface of Mercury at
  11 and 45 μm are presented. The data were obtained during the first
  flyby along a nera-equatorial swath extending from 17 hours local
  time through local midnight to 9 hours local time. For an assumed
  emissivity of 0.9, derived surface thermal inertias are between
  0.0031 and 0.0031 cal cm<SUP>-2</SUP>sec<SUP>-1/2</SUP>K<SUP>-1</SUP>
  and the implied minimum predawn surface kinetic temperature for the
  warm pole at longitude 270° is near 93 K. Several pronounced thermal
  inhomogeneities were seen, one of which appears to coincide with a
  region of high radar reflectivity. The derived thermal properties and
  the electrical skin depth and loss tangent fall within the range of
  values found on the Moon.

Title: Velocity Structure in the Sodium Emission from Io
Authors: Trauger, J. T.; Roesler, F. L.; Münch, G.
Bibcode: 1976BAAS....8R.468T
Altcode:
  No abstract at ADS

Title: Interferometric studies of the emissions associated with Io
Authors: Münch, G.; Trauger, J.; Roesler, F.
Bibcode: 1976BAAS....8Q.468M
Altcode:
  No abstract at ADS

Title: Results of the infrared radiometer experiment on Pioneers 10
    and 11
Authors: Ingersoll, A. P.; Muench, G.; Neugebauer, G.; Orton, G. S.
Bibcode: 1976jsia.coll..197I
Altcode: 1976IAUCo..30..197I
  The infrared radiometers on the Pioneer 10 and 11 spacecraft have mapped
  Jupiter in two broad spectral channels centered at wavelengths of 20
  and 45 microns. Comparison of Pioneer 10 and 11 data and the results
  of in-flight and laboratory calibrations indicate an absolute accuracy
  of + or - 8% in the measured intensities. The relative accuracy for
  comparing different regions on the planet is + or - 2%. Within the
  precision of observations, the derived value of effective temperature
  is independent of assumptions about the Jovian emission spectrum. The
  global effective temperature is 125 + or - 3 K, implying a value of
  1.9 + or - 0.2 for the ratio of planetary thermal emission to solar
  energy absorbed. The effective temperatures of belts are greater than
  those of zones by as much as 3.5 K. On a global scale, the poles and
  equator have the same effective temperature.

Title: Results of the infrared radiometer experiment on Pioneers 10
    and 11.
Authors: Ingersoll, A. P.; Münch, G.; Neugebauer, G.; Orton, G. S.
Bibcode: 1976jupi.conf..197I
Altcode:
  No abstract at ADS

Title: Optical identification of the supersonic emission features
    in the Orion nebula.
Authors: Taylor, K.; Münch, G.
Bibcode: 1975PASP...87..509T
Altcode:
  No abstract at ADS

Title: Pioneer 11 Infrared Radiometer Experiment: The Global Heat
    Balance of Jupiter
Authors: Ingersoll, A. P.; Muench, G.; Neugebauer, G.; Diner, D. J.;
   Orton, G. S.; Schupler, B.; Schroeder, M.; Chase, S. C.; Ruiz, R. D.;
   Trafton, L. M.
Bibcode: 1975Sci...188..472I
Altcode:
  Data obtained by the infrared radiometers on the Pioneer 10 and Pioneer
  11 spacecraft, over a large range of emission angles, have indicated an
  effective temperature for Jupiter of 125 degrees ± 3 degrees K. The
  implied ratio of planetary thermal emission to solar energy absorbed
  is 1.9 ± 0.2, a value not significantly different from the earth-based
  estimate of 2.5 ± 0.5.

Title: AZ Cassiopeiae at the 1956 - 57 eclipse.
Authors: Méndez, R. H.; Münch, G.; Sahade, J.
Bibcode: 1975PASP...87..305M
Altcode:
  The spectrum of AZ Cas at the time of the 1956-57 eclipse can be
  described as a combination of an F8 Ib star and a main-sequence B0-I
  companion. The latter star is ejecting matter with approximately
  spherical symmetry at some 50-60 km/sec, while the former has a very
  extended atmosphere. The whole system seems to be also surrounded
  by an expanding envelope. Determinations of the spectral type of the
  red companion range from early-M, well before eclipse, to F8, in the
  present material, with a Ib-luminosity class sensibly constant. This
  variation is interpreted as indicating changes in the optical thickness
  of the envelope surrounding the late-type companion, either intrinsic
  (rho Cas episode) or related to the binary nature of the system.

Title: Sodium D-Line Emission from Io: Spatial Brightness Distribution
    from Multislit Spectra
Authors: Münch, G.; Bergstralh, J. T.
Bibcode: 1975BAAS....7..386M
Altcode:
  No abstract at ADS

Title: Pioneer 11 Infrared Radiometer Experiment: the Global Heat
    Balance of Jupiter
Authors: Ingersoll, A. P.; Munch, G.; Neugebauer, G.; Diner, D. J.;
   Orton, G. S.; Schupler, B.; Chase, S. C.; Ruiz, R. D.; Trafton, L. M.
Bibcode: 1975BAAS....7..388I
Altcode:
  No abstract at ADS

Title: Pioneer 11 Infrared Radiometer Experiment: the Global Heat
    Balance of Jupiter
Authors: Ingersoll, A. P.; Munch, G.; Neugebauer, G.; Diner, D. J.;
   Orton, G. S.; Schupler, B.; Chase, S. C.; Ruiz, R. D.; Trafton, L. M.
Bibcode: 1975BAAS....7..391I
Altcode:
  No abstract at ADS

Title: Highlights in planetary spectroscopy 1962 - 75.
Authors: Muench, G.
Bibcode: 1975MSRSL...9...87M
Altcode: 1975assp.conf...87M; 1975apes.conf...87M
  Recent advances in spectroscopic studies of the planets with
  ground-based telescopes in the photomultiplier and IR spectral ranges
  are reviewed. Results of spectroscopic observations of Venus and Mars
  are briefly summarized, noting that the crucial problem confronting the
  interpretation of the Venusian spectrum is the nature of the clouds and
  that the outstanding problem in understanding the Martian atmosphere is
  the N2 or Ar concentration that may be present. Spectroscopic results
  for Jupiter, Saturn, Uranus, and Neptune are discussed, emphasizing
  observations of molecular hydrogen, HD, water, (C-13)H4, other
  hydrocarbons, and deuterated hydrocarbons. IR and visual spectroscopic
  observations of Titan and Io are reviewed which show that the CH4 bands
  in Titan's spectrum are pressure broadened and that a flattened ring
  of sodium is situated around Jupiter in the orbital plane of Io.

Title: Multislit spectra of the sodium emission associated with Io.
Authors: Münch, G.; Bergstrahl, J. T.
Bibcode: 1975PASP...87Q.506M
Altcode:
  No abstract at ADS

Title: On the Spectrum of Neutral Oxygen in the Orion Nebula
Authors: Münch, Guido; Taylor, Keith
Bibcode: 1974ApJ...192L..93M
Altcode:
  Images of the Orion Nebula in radiation of the 0 1 permitted lines are
  shown to have a unique filamentary structure not apparent in the [0 1]
  X6300 or other nebular lines. High-resolution profiles for these same
  lines are also presented. The 0 1 X8446 structure is explained in terms
  of the L resonance with the oxygen 2 3P-2 3D transition. The absence
  of such filamentary structure in Ha, produced also by L decay, is
  hypothesized to be the result of a concentration of solid particles in
  the transition H ii-H I region of high density where fluctuations of the
  0 1 X8446 emission originate. headings: line formation - Orion Nebula

Title: Preliminary Infrared Radiometry of the Night Side of Mercury
    from Mariner 10
Authors: Chase, S. C.; Miner, E. D.; Morrison, D.; Munch, G.;
   Neugebauer, G.; Schroeder, M.
Bibcode: 1974Sci...185..142C
Altcode:
  The infrared radiometer on Mariner 10 measured the thermal emission from
  the planet with a spatial resolution element as small as 40 kilometers
  in a broad wavelength band centered at 45 micrometers. The minimum
  brightness temperature (near local midnight) in these near-equatorial
  scans was 100 degrees K. Along the track observed, the temperature
  declined steadily from local sunset to near midnight, behaving as would
  be expected for a homogeneous, porous material with a thermal inertia of
  0.0017 cal cm<SUP>-2</SUP> sec<SUP>-1/2</SUP> degrees K<SUP>-1</SUP>,
  a value only slightly larger than that of the moon. From near midnight
  to dawn, however, the temperature fluctuated over a range of about 10
  degrees K, implying the presence of regions having thermal inertia
  as high as 0.003 cal cm<SUP>-2</SUP> sec<SUP>-1/2</SUP> degrees
  K<SUP>-1</SUP>.

Title: Mariner Venus/Mercury: Results of Infrared Radiometer
    Experiment
Authors: Munch, G.
Bibcode: 1974BAAS....6S.386M
Altcode:
  No abstract at ADS

Title: Results from the Infrared Radiometer Experiment on Pioneer 10
Authors: Münch, G.; Neugebauer, G.; Schroeder, M.; Trafton, L.;
   Chase, S. C.; Ruiz, R.
Bibcode: 1974BAAS....6..388M
Altcode:
  No abstract at ADS

Title: Preliminary Infrared Radiometry of Venus from Mariner 10
Authors: Chase, S. C.; Miner, E. D.; Morrison, D.; Munch, G.;
   Neugebauer, G.
Bibcode: 1974Sci...183.1291C
Altcode:
  The intensity of emission at 45 micrometers, measured with high spatial
  resolution along a single crossing of the Venus disk, is presented. On
  the average, the observed darkening toward the limb varies nearly
  linearly with the cosine of the emission angle. The brightness
  temperature, extrapolated to normal emission, is 255 degrees K. The
  limb darkening curve, interpreted in a linear approximation, implies
  that the atmosphere is quite opaque, with an absorption coefficient of
  0.24 per kilometer. Changes in curvature present in the limb darkening
  curve suggest the existence of thermal inhomogeneities with scale
  comparable to that of the dark markings shown by ultraviolet images.

Title: Pioneer 10 Infrared Radiometer Experiment: Preliminary Results
Authors: Chase, S. C.; Ruiz, R. D.; Munch, G.; Neugebauer, G.;
   Schroeder, M.; Trafton, L. M.
Bibcode: 1974Sci...183..315C
Altcode:
  Thermal maps of Jupiter at 20 and 40 micrometers show structure
  closely related to the visual appearance of the planet. Peak brightness
  temperatures of 126 degrees and 145 degrees K have been measured on
  the South Equatorial Belt, for the 20- and 40-micrometer channels,
  respectively. Corresponding values for the South Tropical Zone are
  120 degrees and 138 degrees K. No asymmetries between the illuminated
  sunlit and nonilluminated parts of the disk were found. A preliminary
  discussion of the data, in terms of simple radiative equilibrium models,
  is presented. The net thermal energy of the planet as a whole is twice
  the solar energy input.

Title: Announcement
Authors: Jascheck, C.; Giclas, H. L.; Hayford, P.; Johnson, H. L.;
   Landolt, A. U.; Luyten, W.; Marlborough, J. M.; Mermilliod, J. -Cl.;
   Münch, G.; Stephenson, C. B.; Wallerstein, G.
Bibcode: 1973BICDS...5...26J
Altcode:
  No abstract at ADS

Title: The Helium Abundance on Jupiter (Article published in the Space
    Science Reviews special issue on 'Outer Solar System Exploration -
    An Overview', ed. by J. E. Long and D. G. Rea.)
Authors: Hunten, Donald M.; Münch, Guido
Bibcode: 1973SSRv...14..433H
Altcode:
  Methods of determining helium on Jupiter (and the Jovian planets)
  are critically surveyed. Current information is consistent with
  solar abundance, He/H<SUB>2</SUB> = 0.11 by number. The available
  lines of evidence are the mean density, spectral-line broadening, and
  stellar occultations. Methods usable from spacecraft flying by are
  discussed. Observation of far-infrared emission has great promise,
  but we may have to await the development of entry probes for the
  greatest assurance.

Title: On the Spectrum of Titan
Authors: Münch, Guido
Bibcode: 1973BAAS....5..305M
Altcode:
  No abstract at ADS

Title: A strategy for investigation of the outer solar system. Outer
    planets, their satellites, and particles and fields at great distances
    from the sun.
Authors: Münch, G.; Hunten, D. M.; Kliore, A. J.; Lewis, J. S.;
   McElroy, M. B.; Spencer, N. W.; Stone, P. H.; Wetherill, G. W.;
   Cameron, A. G. W.; Hubbard, W. B.; Murray, B. C.; Peale, S. J.; van
   Allen, J. A.; Axford, W. I.; Gulkis, S.; Kennel, C. F.; Montgomery,
   M. D.; Parker, E. N.; Sonett, C. P.; Stone, R. G.; Trainor, J. H.;
   Rea, D. G.; Long, J. E.; Padrick, B. D.
Bibcode: 1973SSRv...14..347M
Altcode:
  No abstract at ADS

Title: Preliminary report on infrared radiometric measurements from
    the Mariner 9 spacecraft.
Authors: Kieffer, H. H.; Chase, S. C., Jr.; Miner, E.; Münch, G.;
   Neugebauer, G.
Bibcode: 1973JGR....78.4291K
Altcode:
  Preliminary 10- and 20-μm brightness temperatures of Mars are
  presented. More than 35% of the Martian surface was observed with
  a resolution better than 100 km. On the whole, the results confirm
  the thermal properties derived from the Mariner 6 and 7 radiometers,
  although the temperatures, on the average, were cooler and shifted with
  respect to the Martian day during the dust storm. Thermal inertias and
  radiometric albedos were derived for many areas; no clear correlation
  exists between these properties. Thermal structure again was found at
  the spatial limit of the radiometer; no cases were found in which it
  was necessary to invoke internal heat sources.

Title: High resolution astronomical spectroscopy: its future.
Authors: Muench, G.
Bibcode: 1972ailt.conf...21M
Altcode:
  No abstract at ADS

Title: Infrared Thermal Mapping Experiment: The Viking Mars Orbiter
Authors: Kieffer, Hugh H.; Neugebauer, G.; Munch, G.; Chase, S. C.,
   Jr.; Miner, E.
Bibcode: 1972Icar...16...47K
Altcode:
  The Mars infrared thermal mapper (IRTM) will be carried on the scan
  platform of the orbiter of the Viking 1975 mission. The IRTM is a
  multichannel radiometer with several detectors in each of six spectral
  regions. This instrument will measure the reflected solar radiation and
  surface thermal emission from the area viewed by the orbiter imaging
  system with nominal 5 km resolution. Extensive additional areas will
  be covered for which simultaneous imaging will not be available. The
  spectral channels are selected to be sensitive to surface emissivity
  variations and provide good temperature resolution over the entire range
  of Martian temperatures. These observations will allow determination
  of the surface kinetic temperature and thermal balance, and by coverage
  of the dark hemisphere, a search for regions with anomalous cooling can
  be made. Observations of ground frosts or clouds will help to determine
  their composition, and in the case of extensive H <SUB>2</SUB>O frosts,
  will allow the local water vapor pressure to be estimated.

Title: Mariner 9 Science Experiments: Preliminary Results
Authors: Steinbacher, R. H.; Kliore, A.; Lorell, J.; Hipsher, H.;
   Barth, C. A.; Masursky, H.; Munch, G.; Pearl, J.; Smith, B.
Bibcode: 1972Sci...175..293S
Altcode:
  No abstract at ADS

Title: Infrared Radiometry Experiment on Mariner 9
Authors: Chase, S. C., Jr.; Hatzenbeler, H.; Kieffer, H. H.; Miner,
   E.; Munch, G.; Neugebauer, G.
Bibcode: 1972Sci...175..308C
Altcode: 1972Sci...175..398C
  The brightness temperatures at 10 and 20 micrometers measured by the
  Mariner 9 infrared radiometer differ substantially from those predicted
  by the radiometer results of Mariners 6 and 7. The results indicate
  a significant latitude-dependent contribution of the atmospheric dust
  to the observed thermal emission.

Title: Jupiter: An Unidentified Feature in the 5-Micron Spectrum of
    the North Equatorial Belt
Authors: Munch, G.; Neugebauer, G.
Bibcode: 1971Sci...174..940M
Altcode:
  Grating spectra of the North Equatorial Belt of Jupiter between 4.5
  and 5.1 microns, obtained with a nominal resolving power of 180, are
  presented. An absorption feature centered at 4.73 microns and not due
  to a known constituent has been found. Its possible identification
  is discussed.

Title: Mariner 1969 Infrared Radiometer Results: Temperatures and
    Thermal Properties of the Martian Surface
Authors: Neugebauer, G.; Münch, G.; Kieffer, H.; Chase, S. C., Jr.;
   Miner, E.
Bibcode: 1971AJ.....76..719N
Altcode:
  The reduced data of the Mariner 6 and 7 Infrared Radiometer Experiments
  are presented, along with a discussion of the reduction and calibration
  procedures. Evidence is presented showing that the surface of Mars is
  strongly nonhomogeneous in its thermal properties, on scales ranging
  from those of the classical light and dark areas to the limit of
  resolution of the radiometers. On the sunlit side, the mean thermal
  inertia, for admissible bolometric albedos, is 0.006 (cal cm sec
  0K-1). The dark areas Syrtis Major and Mare Tyrrhenum, observed at
  night, require thermal inertias as high as 0.010. The temperatures
  measured over the circular basin Hellas require a bolometric albedo of
  0.40 and also a high thermal inertia. The temperature measured over the
  south polar cap, 148 K, provides evidence that the major constituent
  of the frost deposit is CO2.

Title: The Distribution of Gas and Dust in the Orion Nebula
Authors: Münch, G.; Persson, S. E.
Bibcode: 1971ApJ...165..241M
Altcode:
  Photoelectric measurements of Balmer-line intensities at 4000 points
  on the Huyghenian region of the Orion Nebula, with an angular
  resolution of 3 arc sec, are analyzed to show the following: (1)
  The differential reddening that affects nebular radiation can be
  accounted for only if dust particles are mixed with the ionized gas
  and the wavelength dependence of the dust-absorption coefficient is
  the same as that determined for the Trapezium stars. (2) The intensity
  and reddening gradients, on the average, have the same sign. This fact
  indicates that dust is well mixed with the gas and that, statistically,
  fluctuations in gas density are positively correlated with variations
  in dust density. The behavior of the intensities of the He I lines at
  10830, 7065 and 5876 A, measured at 150 points covered by Balmer-line
  observations, can be understood only if dust, absorbing resonantly
  trapped X10830 photons, is mixed with the gas.

Title: The Distribution of Gas and Dust in the Orion Nebula
Authors: Münch, G.; Persson, S. E.
Bibcode: 1971BAAS....3...17M
Altcode:
  No abstract at ADS

Title: Mariner 1969: Results of the Infrared Radiometer Experiment
Authors: Münch, G.; Neugebauer, G.; Chase, S. C.
Bibcode: 1971IAUS...40..258M
Altcode:
  No abstract at ADS

Title: Selected Topics on the Physics of the Interstellar Medium
Authors: Münch, G.
Bibcode: 1970gaas.conf..191M
Altcode:
  No abstract at ADS

Title: Infrared Radiometry Experiment for Mariner Mars 1971
Authors: Chase, S., Jr.; Miner, E.; Münch, G.; Neugebauer, G.
Bibcode: 1970Icar...12...46C
Altcode:
  The infrared radiometer is designed to provide brightness temperatures
  of the surface of Mars by measuring the energy radiated in the 8 to
  12 and 18 to 25 μ wavelength bands. The instrument is essentially the
  same as that flown on the Mariner Mars 1969 missions, modified only to
  define more sharply the field of view. Because Mariner Mars 1971 will
  orbit Mars, a given area of the planet will be observed at a variety
  of local times, and the characterization of the various areas by their
  thermophysical properties will be more complete than that obtained by
  Mariner Mars 1969.

Title: Interstellar Gas
Authors: Münch, G.
Bibcode: 1970saac.book..295M
Altcode:
  No abstract at ADS

Title: Appearance of Jupiter in the thermal infrared.
Authors: Münch, G.; Neugebauer, G.
Bibcode: 1970TrAGU..51..771M
Altcode:
  No abstract at ADS

Title: Mariner 1969: Preliminary Results of the Infrared Radiometer
    Experiment
Authors: Neugebauer, G.; Munch, G.; Chase, S. C., Jr.; Hatzenbeler,
   H.; Miner, E.; Schofield, D.
Bibcode: 1969Sci...166...98N
Altcode:
  The thermal energy emitted by Mars was measured in the 8- to 12- and 18-
  to 25-micrometer bands. The minimum temperature derived for the southern
  polar cap is 150 degrees K, an indication that the cap is formed by
  frozen carbon dioxide. No significant temperature fluctuations were
  detected with a 100-kilometer scale.

Title: The structure of the atmospheres of the major planets.
Authors: Trafton, L. M.; Münch, G.
Bibcode: 1969JAtS...26..813T
Altcode:
  No abstract at ADS

Title: Internal Motions in the Planetary Nebula NGC 6543
Authors: Münch, Guido
Bibcode: 1968IAUS...34..259M
Altcode:
  No abstract at ADS

Title: Interstellar Absorption Lines
Authors: Münch, Guido
Bibcode: 1968S&SS....7..365M
Altcode:
  No abstract at ADS

Title: Small-Scale Thermal Homogeneity of the Orion Nebula
Authors: Münch, Guido
Bibcode: 1968iih..conf..507M
Altcode:
  No abstract at ADS

Title: Interstellar Absorption Lines
Authors: Münch, Guido
Bibcode: 1968nim..book..365M
Altcode:
  No abstract at ADS

Title: The physical state of the interstellar gas in the Messier
    31 nucleus
Authors: Munch, G.
Bibcode: 1968IAUS...29...71M
Altcode:
  No abstract at ADS

Title: Infrared Coronal Lines. II. Observation of [SI x] λ 1.43 μ
    and [Mg VIII] λ 3.03&amp;mu
Authors: Münch, G.; Neugebauer, G.; McCammon, D.
Bibcode: 1967ApJ...149..681M
Altcode:
  The wavdengths and intensities of the coronal lines of the ions Si +
  and Mg8+, resulting from the airborne observation of the November 12,
  1966, total solar eclipse, are given

Title: Spectrophotometry of Uranus from 3300 to 11000 Angstroms
Authors: Younkin, R. L.; Munch, G.
Bibcode: 1967AJ.....72R.328Y
Altcode:
  No abstract at ADS

Title: Observation of the coronal lines of [Si X] and [Mg VIII]
    at the 12 November 1966 Solar eclipse
Authors: Munch, G.; Neugebauer, G.; McCammon, D.
Bibcode: 1967AJ.....72S.313M
Altcode:
  No abstract at ADS

Title: Infrared Spectra of Low-Temperature Stars
Authors: McCammon, D.; Munch, G.; Neugebauer, G.
Bibcode: 1967ApJ...147..575M
Altcode:
  Spectra of stars of types M, N(R), and S, as well as of NML objects
  in Cygnus and Taurus, are presented in the regions 5-1.8 and x1 9-2 5
  . In M stars the absorption due to stellar H2O is apparent from the
  wings of the bands at xl .4, xt .9, and x2.7 Stars of N and S types
  show weaker H2O absorption. The Av = 2 and Av = 3 vibration-rotation
  band sequences of CO appear well marked in all stars, being somewhat
  weaker in the M types than in other stars. The late N stars Y CVn and
  U Hyd show a sharp discontinuity or band head at xl .76 not present
  in other stars. The entire spectra of Y CVn and U Hyd shortward of
  this discontinuity appears veiled, the Av = 3 CO band sequence being
  conspicuously weak. The spectra of the NML objects in Cygnus and
  Taurus have spectral characteristics resembling the carbon more than
  the M stars.

Title: The Weakness of Helium Lines in Globular Cluster and Halo
    B Stars
Authors: Greenstein, Jesse L.; Münch, Guido
Bibcode: 1966ApJ...146..618G
Altcode:
  No abstract at ADS

Title: Absorption Lines from Intermediate-Latitude Interstellar
    Complexes
Authors: Münch, Guido
Bibcode: 1966PASP...78..305M
Altcode:
  No abstract at ADS

Title: Infrared Lines of the Solar Corona. I. Prediction
Authors: Münch, Guido
Bibcode: 1966ApJ...145..237M
Altcode:
  The existence of coronal lines in the instrumental infrared, due to the
  ions Mg7+, Al8+, and 5i8+ and Si +, is predicted and their intensities
  are estimated. The possibility of detecting these lines with practicable
  infrared spectrometers and photoconductive detectors is analyzed, taking
  into consideration attenuation by atmospheric gases. The powers radiated
  in the [Mg viiij, [Si ix], and [Si x] lines are found to be large
  enough to make their detection feasible with instruments of modest size.

Title: Caltech-JPL Lunar and Planetary Conference
Authors: Brown, Harrison; Stanley, Gordon J.; Muhleman, Duane O.;
   Münch, Guido
Bibcode: 1966lupl.conf.....B
Altcode:
  No abstract at ADS

Title: High-Resolution Observations of Interstellar Sodium D Lines
    with an Interferometer.
Authors: Vaughan, Arthur H., Jr.; Münch, Guido
Bibcode: 1966AJ.....71..184V
Altcode:
  Interstellar sodium D line profiles in some 20 early-type stars were
  scanned at a resolving limit of about 18 mA with a single-etalon
  Fabry- Perot interferometer. The coude' spectrum scanner of the
  100-in. telescope was tised as a premonochromator, a monitor channel at
  nearby ~`avelengths provided seeing compensation, and pulse Counting
  techniques were employed. The method achieves an efficiency gain of
  a factor 10 compared to conventional spectroscopy for the study of
  the D lines. The faintest star of this survey (HD 217101, `B4~=6.2)
  gave a signal-to-dark ratio of 3. In at least one-half of the stars
  observed the number of Na I components resolved interferometrically
  exceeded the number of Ca II components previously reported by
  W. S. Adams (Astrophys. J. 109, 335, 1949). In most cases the use of
  higher resolution is responsible, but it is also of interest that a
  few components were found in Na I which are weak or missing in Ca II,
  in contrast to previous studies (Routly and Spitzer, Astrophys. J. 115,
  227, 1952) where the inverse has usually been true. A comparison of our
  data for a Cygni with results obtained by a different interferometric
  technique by L. M. Hobbs (Astrophys. J. 142, 160, 1965) indicates
  some discrepancies which as yet are unexplained. This work is partly
  supported by the National Aeronautics and Space Administration under
  Grant NsG-426.

Title: Predicted Coronal Lines in the Instrumental Infrared.
Authors: Münch, Guido
Bibcode: 1966AJ.....71..173M
Altcode:
  The ions Mg7+, Al5+, 5j9+, with 2s22p ground state configurations and
  ionization potentials IP of 266, 330, and 401 eV, produce coronal
  lines at wavelengths near 3.032, 2.047, and 1.431 p. The ion Si~+
  with 2s22p2 ground state and IP=351 eV produces lines at 2.587 and
  3.859 p. An estimate of the strength of these coronal lines has been
  made on the basis of assumed abundances and approximate theories of
  ionization and excitation. It has been found that the lines of Mg7+,
  Si5+, and 5j9+ should be as strong as the iron coronal lines in the
  photographic region. In consideration of the detectivity of infrared
  detectors (PbS), estimates have been made of the signal to noise ratios
  that may be reached with optics of practical size during a total solar
  eclipse. The effects of atmospheric absorption have been taken into
  account to the extent justified by the uncertainties affecting the
  predicted wavelengths of the lines. The probability that the lines
  will be observable from ground notwithstanding atmospheric absorption
  and that they can be detected appear fairly high.

Title: Visible and Near-Infrared Spectrophotometry of Saturn's Rings.
Authors: Younkin, Robert L.; Münch, Guido
Bibcode: 1966AJ.....71R.188Y
Altcode:
  Measurements of the narrow-band spectral energy distribution of the
  rings of Saturn have been made at the Mount Wilson Observatory using
  the 60-in. reflector and the Fastie- Ebert spectrometer. Spectral scans
  from 0.51 to 1.1 IL were made of a segment of the rings at the western
  end of the semimajor aXls. The energy distribution was determined at 54
  points in this wavelength region. The color sensitivity of the system
  was determined from scans of a Lyr and the a Lyr energy distribution
  of Oke. The relative reflectance of the rings was calculated by use of
  the solar intensity values of Labs and Neckel, converted to solar flux
  by the ratios of Minnaert. The reflectance of the rings is very nearly
  constant from 0.78 to 1.05 IL Shortward of this region it falls slowly
  to 0.60 IL' then more rapidly to a value at 0.51 IL some 0m.45 below
  the maximum. There is a slight decrease in reflectance (0~~03~0m.0S)
  from 1.05 to 1.08 IL This is marginally outside of the experimental
  error. Owen has recently reported a drop in the reflectance of the
  rings from 1.04 to 1.09 IL' whid~ he identified as due to water
  ice. This drop was determined on the basis of a drop in the ratio
  of the intensity of the rings to the intensity of Saturn in this
  region. Separate measurements at Mount Wilson of the reflectance of
  Saturn show a continuous strong absorption from 0.97 to 1.04 IL This
  unfortuitous coincidence yields a large drop in the ratio beyond 1.04
  IL which will completely mask any possible ice absorption which by
  the results above will be only a few percent at most.

Title: Structure and Kinematics of the Orion Nebula
Authors: Munch, G.
Bibcode: 1966IAUTB..12..463M
Altcode:
  No abstract at ADS

Title: The Spectra of Two Extremely Red Objects.
Authors: Münch, Guido; Scargle, Jeffrey D.
Bibcode: 1965ApJ...142..401M
Altcode:
  No abstract at ADS

Title: Galactic Structure and Interstellar Absorption Lines
Authors: Münch, Guido
Bibcode: 1965gast.book..203M
Altcode: 1965S&SS....5..203M; 1965gast.conf..203M
  No abstract at ADS

Title: On the interpretation of strong CO<SUB>2</SUB> absorption
    bands in the spectrum of Mars / G. Munch and G. Neugebauer
Authors: Munch, Guido; Neugebauer, Gerry
Bibcode: 1965LowOB...6..181M
Altcode:
  No abstract at ADS

Title: Wavelength Dependence of the Band Structures of Jupiter and
    of Saturn.
Authors: Younkin, Robert L.; Münch, Guido
Bibcode: 1964AJ.....69..565Y
Altcode:
  Photoelectric measurements of the band structures of Jupiter and of
  Saturn were made during September 1963 by moving a small slot along
  the central meridian of the planetary image. The Mt. Wilson Ebert
  spectrometer was used on the 60-in. reflector as a monochromator
  to select wavelengths from X3200 A to 10400A. Curves obtained for
  Saturn show: (1) radiance of both equatorial zone and north tropical
  zone relative to B-ring exhibit broad maxima in X5800 - X7500 range,
  falling sharply to an ultraviolet minimum near X3800 A; (2) radiance
  of equatorial zone relative north tropical zone is slightly greater
  than unity beyond X6000 A, but falls to 0.58 in the ultraviolet. This
  ratio ~ecomes large in str9ng CH4 bands: 1.6 at X7270 A and 3.7 at
  X8912A with a fairly sharp discontinuity at the north equatorial
  belt. Consistent with these observations is an atmospheric model in
  which cloud particles over the entire planet possess similar selective
  absorption which increases with decreasing wavelength below X5200A,
  but a lower effective cloud level in the temperate and polar regions'
  than the equatorial zone. Thus at short wavelengths where Rayleigh
  scattering dominates particle scattering, the temperate and polar
  regions are brighter than the equatorial zone; and, conversely, at long
  wavelengths and particularly in the CH4 bands, where particle scattering
  dominates. For Jupiter, the north tropical zone was the brightest region
  of the planet throughout the range of wavelengths. Its radiance relative
  to the south tropical zone is anomalous in CH4 absorption, increasing
  in the X8900 A band, and decreasing in the X7270 A band. Contrast
  between tropical zones and adjacent equatorial belts increases with
  decreasing wavelength below X5500 A. In strong CH4 absorption bands the
  limb darkening with latitude greatly increases. The south equatorial
  belt becomes the brightest region of the' planet. In the X8900 A band
  both polar regions become bright at the limb.

Title: Radial Velocities of Distant OB Stars.
Authors: Münch, Guido; Münch, Luis
Bibcode: 1964ApJ...140..162M
Altcode:
  The results of radial-velocity measurements for twenty-seven faint
  OB stars at galactic longitudes between 1" - 18 and 1" = 66 are
  presented. On the basis of spectroscopic absolute magnitudes in the
  Yerkes system and UB V photometry, the rotational velocities of the
  stars around the galactic center have been derived. In comparison with
  the rotational curve indicated by the interstellar neutral hydrogen, the
  stellar motions suggest rotational velocities lower by about 25 km/sec
  at distances from the center around half that of the Sun. The general
  shape of the rotation-curve provided by the new stellar observations
  remains thus the same as it was found in our previous study.

Title: An Interstellar Cloud with a High Concentration of CN
    Molecules.
Authors: Münch, Guido
Bibcode: 1964ApJ...140..107M
Altcode:
  A group of stars embedded in an emission nebula near the cluster
  NGC 7822 has been discovered to have a unique interstellar spectrum,
  characterized by exceedingly strong CN lines. Evidence is presented
  favoring the hypothesis that the CN molecules arise in the immediate
  neighborhood of the H ii region boundary. It is further suggested that
  the CN molecules are formed in the solid particles of the H 1 region
  when flashed by the UV radiation in the advancing ionization front.

Title: An Analysis of the Spectrum of Mars.
Authors: Kaplan, Lewis D.; Münch, Guido; Spinrad, Hyron
Bibcode: 1964ApJ...139....1K
Altcode:
  On a high-dispersion spectrogram of Mars taken at Mount Wilson
  rotational lines of 1120 near X 8300 and CO2 near x 8700 have been
  detected. Recent laboratory measurements of line strengths by D Rank
  have been used to determine the amounts of H2O and CO2 in the atmosphere
  of Mars: t4 + 7 precipitable water and 55 + 20 m atm CO2. From the
  absence of O2 in the Martian spectra, we set an upper limit of 70
  cm atm for the O2 content. By suitably combining the CO2 amount with
  observations by Kuiper and Sinton of the strongly saturated bands in
  the 2-j# region, a surface pressure of 25 + 15 mb has been derived. The
  implications of the results on the composition of the Martian atmosphere
  are discussed.

Title: Molecular Absorptions and Color Distributions over Jupiter's
    Disk.
Authors: Münch, Guido; Younkin, Robert L.
Bibcode: 1964AJ.....69R.553M
Altcode:
  Absorptions of NH3 and CH4 and energy curves of Jupiter have
  been obtained with a photoelectric scanning spec- trometer at the
  60-in. Mt. Wilson reflector. Spectrum scans at various parts of the
  disk and surface scans at fixed wavelength have been obtained with
  resolving powers around 10 A in the range 0.55-1.1 p. The behavior of
  individual lines or bands has also been studied photographically in
  Coude' spectra. Up to date the following results have been obtained:
  (a) The quadrupole H2 lines of the (3,0) vibrational band do not show
  detectable variation in strength with longitude or latitude. (b)
  The zones have a bluer spectrum and show more limb darkening than
  the belts. (c) The absorption at the very strong band X8892 A (CH4)
  increases markedly with latitude and appears stronger in zones than in
  belts. At the polar caps bright cusps are observed. (d) Absorption in
  the weak NH3 X6450 A and CH4 X6190 A bands is slightly weaker in belts
  than in zones, and at fixed latitude decreases in strength both towards
  the morning and evening limbs. This effect is well marked also in the
  lines of the NH3 X7900 band. From (a) it is inferred that, above the
  layers showing visual structure, there is sufficient gas to produce
  completely saturated H2 lines, the strength of which, then cannot
  provide information about the relative abundance of H2 with respect
  to other constituents. Result (b) suggests that, above the zones,
  Rayleigh scattering plays a larger role in the diffuse reflection
  of solar light than above the belts. The red color of the zones,
  relative to the sun, still indicates the presence of selectively
  scattering solid particles, which need not differ in chemical or
  physical composition from the particles forming the cloud belts. The
  higher effective layer for reflection in the belts is also indicated
  by (a). The polar brightening reveals the existence of an extremely
  high cloud cap, or possibly frozen CH4. Previous results of Hess agree
  qualitatively with (d). The intensity variation in longitude of the
  lines can be understood in terms of the pressure dependence of the
  absorption coefficient in lines arising by diffuse reflection.

Title: H<SUB>2</SUB>O and CO<SUB>2</SUB> Absorption in the
    Photographic Infrared Spectrum of Mars
Authors: Münch, G.; Kaplan, L. D.; Spinrad, H.
Bibcode: 1963PASP...75..416M
Altcode:
  No abstract at ADS

Title: Nebular absorption of He 3889 A.
Authors: Munch, G.; Wilson, O. C.
Bibcode: 1963AJ.....68..287M
Altcode:
  No abstract at ADS

Title: Letter to the Editor: the Detection of Water Vapor on Mars.
Authors: Spinrad, Hyron; Münch, Guido; Kaplan, Lewis D.
Bibcode: 1963ApJ...137.1319S
Altcode:
  No abstract at ADS

Title: On the Spectrum of Saturn
Authors: Munch, G.; Spinrad, H.
Bibcode: 1963LIACo..11..541M
Altcode:
  No abstract at ADS

Title: Nebular Absorption of He I λ3889.
Authors: Münch, G.; Wilson, O. C.
Bibcode: 1963AJ.....68Q.287M
Altcode:
  The presence of an absorption line arising from the 2~5 metastable
  level of neutral helium in the spectra of the stars imbedded in the
  Orion Nebula was noticed long ago by 0. C. Wilson. Lately it has been
  shown by G. Mu~nch and 0. C. Wilson (Z. Astrophys. 56, 127, 1962)
  how the strength of this nebular absorption line may be related to
  the surface brightness of a homogeneous emission nebula. The lack
  of agreement between the surface brightness thus computed for the
  Orion Nebula with the observed value, has been interpreted in terms
  of density inhomogeneities in the nebula, independently postulated
  by Osterbrock on other grounds. Because this interpretation has been
  criticized by K. Wurm (Z. Astrophys. 52,149, 1961), new observational
  evidence related to the line in question is being obtained. In this
  communicatioi~, besides new data for the Orion stars, the results
  of the search for the absorption line in other emission nebulae are
  presented. So far the line has been detected in a number of stars in
  the complex M8- M20, in BD +6601675, exciting NGC 6822, in BD +6002522
  exciting NGC 7635, and in HD 64315, exciting star of NGC 2467. The stars
  imbedded in 20 other H II regions do not have detectable He I nebular
  absorption. Although a complete discussion of the data requires surface
  brightness determinations (corrected for interstellar and internebular
  extinction) not available yet, it is shown how the recent observations
  fully support the interpretation advanced earlier by Wilson and Mu~nch.

Title: The Intensity of Forbidden Emission Lines.
Authors: Münch, Guido
Bibcode: 1962ApJ...136..823M
Altcode:
  A general formula for the intensity of a forbidden emission line in a
  two-level atom is derived, taking into consideration induced emissions,
  saturation effects, and departures from a Boltxmann distribution. The
  kinetic temperature is supposedly given, but not necessarily is it taken
  as constant It is shown how this general formula embodies expressions
  used in the past separately for the optical, infrared, and radio regions
  of the spectrum As an example of application of the formulae derived,
  the emission rate in the fine-structure transition of the ground state
  of C+ is re-evaluated under the conditions prevailing in interstellar
  H I regions As an illustration of a line arising in a medium with
  variable temperature, the intensity in the normal direction and flux
  of the line arising between the lowest two fine-structure levels of
  the ground state of oxygen is computed, under conditions appropriate
  to the earth's upper atmosphere. It is found that the outward energy
  flux in this line compares with the energy input provided by solar
  X-rays at the time of low solar activity.

Title: Interstellar Gas Near the Sun.
Authors: Münch, G.; Unsöld, A.
Bibcode: 1962ApJ...135..711M
Altcode:
  Observations of interstellar Ca ii lines in the spectrum of the nearby
  star a Oph and other stars in the same area of the sky are reported
  From the radial velocities and intensities of the interstellar lines
  it is shown that the cloud in front of a Oph has linear dimensions of
  the order of 1 pc and a total number density of order unity

Title: Recent Spectroscopic Investigations of Jupiter and Saturn.
Authors: Spinrad, Hyron; Münch, Guido; Trafton, Laurence M.
Bibcode: 1962AJ.....67Q.587S
Altcode:
  This report deals with high-dispersion spectroscopic studies currently
  in progress at the Mt. Wilson and Palomar Observatories. On spectra
  taken with the slit along Jupiter's equator we have found that the
  inclinations of the Jovian ammonia and methane absorption lines are less
  than would be expected if these gases rotate with the planet (Spinrad,
  Astrophys. J., to be published, 1962). The result is interpreted to mean
  a slow rotation for the NH3 and CH4 molecules. In the case of Saturn,
  the CH4 lines are inclined so that the methane appears to be rotating
  about 10% faster than the cloud layer producing the scattered Fraunhofer
  spectrum (Munch and Spinrad, 11th Liege Symposium, Physics of Planets,
  1962). The Jovian NH3 lines vary in strength with time, probably on a
  time scale longer than a few days. From the half-widths of the Jovian
  NH3 and CH4 absorption lines we have determined crude upper limits for
  the total pressure in this portion of Jupiter's atmosphere. Three weak,
  sharp new absorption lines not associated with the methane or ammonia
  bands were found in the Jovian spectrum; one of these is the 5(1)
  line of H2 in the (4,0) band. No reasonable coincidences have been
  established for the other two unidentified features. On Saturn we have
  found both the 5(1) and 5(0) lines of molecular hydrogen in the (4,0)
  band. The total amount of H2 visible is comparable to the amount above
  the Jovian "reflecting layer"; a rotational temperature for the H2
  has been determined. We cannot identify any of the red NH3 lines in
  the Saturn spectrum with certainty. The ammonia content of Saturn's
  atmosphere in 1962 must be considerably below the usually quoted value
  of 200 cm-atm.

Title: Structural Problems of Galaxies in the Light of LYMAN-α
Authors: Münch, Guido
Bibcode: 1962saa..conf..219M
Altcode:
  No abstract at ADS

Title: On the Structure of the Orion Nebula. A Reply to K. WURM. With
    2 Figures in the Text
Authors: Münch, G.; Wilson, O. C.
Bibcode: 1962ZA.....56..127M
Altcode:
  No abstract at ADS

Title: Motions of the Interstellar Gas in the Central Regions
    of Galaxies
Authors: Münch, Guido
Bibcode: 1962IAUS...15..119M
Altcode:
  No abstract at ADS

Title: Interstellar Matter at Large Distances from the Galactic Plane.
Authors: Münch, Guido; Zirin, Harold
Bibcode: 1961ApJ...133...11M
Altcode:
  The interstellar gas at large distances z from the galactic plane
  is studied by the absorption lines it produces on the spectrum of
  distant stars off the Milky Way. From the statistics of multiple lines
  in various ranges of z, it is shown that some gas clouds probably
  exist at z = 1 kpc. The number of clouds observed in 0 5 &lt;z &lt;
  1 kpc has been found to be larger than would be expected from the
  known distribution of their velocity components in the galactic
  plane. The apparent asymmetry in the distribution of high-velocity
  clouds is explained as the result of decreased chances of collisions
  in the z-direction and also in terms of an intrinsic anisotropy in the
  mechanism accelerating the clouds. The typical time required for the
  clouds to reach their actual probable height from z = 0 is evaluated
  to be 40 X 106 years From the line intensities and by assuming cosmic
  abundance of the elements, a relation between the linear dimensions and
  the densities of the clouds is established. Irrespective of whether
  the clouds are H I or H ii regions, it is found that their continued
  existence for 40 X 106 years requires the operation of a process
  preventing them from expanding. The physical conditions prevailing
  in a galactic halo or corona exerting pressure on the clouds are
  next analyzed. It is shown how the observations rule out a halo with
  an electron temperature T, around 10 K. A corona with T = 106 K, as
  postulated by Spitzer, on the other hand, is found admissible, provided
  that the high-velocity clouds at high z are H ii regions. The large
  energy input by conduction from the corona may be balanced by radiative
  losses only at about T - 10 K. Next the ionization e uilibrium in the
  clouds is briefly discussed, and it is suggested that the anomalous
  abundance ratio Na Ca observed in interstellar space is the result of
  using an unrealistic mean stellar radiation field in the photoionization
  computations. In this context, the results of a calculation of the
  ionization equilibrium of aluminum is presented It is shown that the Al
  I line at X 3964 should have a strength about one-twentieth that of Ca
  I X 4226. In a final section the possible mechanisms by means of which
  interstellar clouds may be accelerated are discussed. It is shown how
  the operation of the Oort-Spitzer process requires a ratio between the
  total amounts of ionized and neutral interstellar matter much larger
  than is observed. The relevance of magnetic fields in accelerating
  small masses of ionized field4ree material is thereby emphasized.

Title: The Linear Dimensions of HII Regions.
Authors: Münch, Guido
Bibcode: 1960AJ.....65..495M
Altcode:
  The ionization equilibrium of interstellar hydrogen near hot stars has
  been studied and has taken into consideration the finite probability
  for recombination in the ground state. Simultaneous solutions of the
  transfer equation for radiation beyond the head of the Lyman series
  and Saha's relation have been found, paying attention to the spherical
  geometry. For a value ~=0.4 for the probability of scattering of an UV
  quantum, it is found that the radius of the sphere of ionized hydrogen
  increases by a factor of 1.6 with respect to that obtained neglecting
  the diffuse radiation field (Stromgren's radius). These results are
  in disagreement with those derived by Pottash and Jefferies (1959,
  Ann. dAstrophys. 22, 297) owing to an erroneous boundary condition
  adopted by these authors. In considering the case of a thin spherical
  shell around the hot star, Pottash and Jefferies impose as boundary
  condition at the inner boundary the vanishing of the diffuse radiation
  field. The correct boundary condition is the vanishing of the flux of
  diffuse radiation throughout the inner volume enclosed by the shell
  (Milne's "planetary nebula" condition). The numerical integrations
  and procedures followed by Pottash and Jefferies for the spherical
  case have not been published in sufficient detail to be compared with
  our results. It is suspected that their work for this case is also
  vitiated by the use of a boundary condition with no physical meaning.

Title: On the Rotation of the Inner Parts of the Galactic System.
Authors: Münch, Guido; Münch, Luis
Bibcode: 1960ApJ...131..253M
Altcode:
  Results of radial-velocity measurements for 18 distant OB stars in
  galactic longitudes between 345 and 35 are presented. On the basis
  of published spectroscopic distance moduli, the results have been
  interpreted in terms of rotational velocities around the galactic center
  and compared with those of the interstellar neutral hydrogen. The
  stellar motions seem to suggest for the rotational velocity of the
  galactic system, at a distance of 6 kpc from the center, a value 10
  km/sec higher than that indicated by the 21-cm line. At a distance
  of 4 kpc from the center, the stellar motions provide rotational
  velocities around 25 km/sec lower than the 21-cm line profiles do. This
  discrepancy is shown to be unlikely to arise from systematic errors
  in the spectroscopic distance moduli or in the radial velocities. The
  motion of the stars considered indicates a value for Oort's constant
  A somewhat larger than the classical value A = 20 km/sec. The BO.S
  Ia star HD 173438 has been found to be a single-line spectroscopic
  binary with a 250- day period, a semiamplitude of 50 km/sec, and an
  eccentricity of 0.54.

Title: On the interpretation of the spiral structure in the galactic
    system
Authors: Münch, G.
Bibcode: 1960AnAp...23..403M
Altcode:
  No abstract at ADS

Title: Motions of the Gas near the Nucleus of M31.
Authors: Münch, Guido
Bibcode: 1960AJ.....65R..55M
Altcode:
  Some results of the observation of [0113 emission in the neighborhood
  of the nucleus of the Andromeda Nebula are presented. With the prime
  focus spectrograph of the Hale reflector at a dispersion of 66 A/mm,
  the [0113 doublet at ~3726-28 has been resolved and detected out to
  a distance of 50" from the nucleus, with the slit at various position
  angles. While the individual components of the doublet appear narrow,
  they show sudden large variations in velocity superposed on the
  rotational pattern of the system as a whole. Because of the underlying
  absorption spectrum, the true value of the velocities can not yet be
  found accurately, but, on the whole, the motion of the gas seems to have
  a well-defined outward motion, amounting to 50 km/sec at a distance
  of 200 pc from the nucleus. The noncircular nature of the motion
  is most clearly observed with the slit along the minor axis, where
  all rotational effects should vanish. There are reasons to interpret
  these observations in terms of motions taking place predominantly in
  directions confined to the symmetry plane of the system.

Title: The Theory of Model Stellar Atmospheres
Authors: Münch, Guido
Bibcode: 1960stat.book....1M
Altcode: 1960S&SS....6....1M; 1960stat.conf....1M
  No abstract at ADS

Title: Letter to the Editor Expending Motions of Interstellar Gas
    in the Nuclear Region of Messier 31.
Authors: Münch, Guido
Bibcode: 1960ApJ...131..250M
Altcode:
  No abstract at ADS

Title: A New O-Type Subdwarf.
Authors: Münch, Guido; Slettebak, Arne
Bibcode: 1959ApJ...129..852M
Altcode:
  No abstract at ADS

Title: On the Distance of the Cassiopeia Radio Source.
Authors: Münch, Guido; Münch, Luis
Bibcode: 1959ApJ...129..854M
Altcode:
  No abstract at ADS

Title: The Mass-Luminosity Ratio in Stellar Systems
Authors: Münch, Guido
Bibcode: 1959PASP...71..101M
Altcode:
  No abstract at ADS

Title: 4. High Temperature Subdwarfs with Anomalous Compositions
Authors: Munch, G.
Bibcode: 1959LIACo...9...53M
Altcode: 1959MSRSL...3...53M
  No abstract at ADS

Title: Internal Motions in the Orion Nebula
Authors: Münch, G.
Bibcode: 1958RvMP...30.1035M
Altcode: 1958IAUS....8.1035M
  No abstract at ADS

Title: Kinematics of the Filaments in the Crab Nebula
Authors: Münch, G.
Bibcode: 1958RvMP...30.1042M
Altcode: 1958IAUS....8.1042M
  No abstract at ADS

Title: Study of the Hydrogen and Helium II Lines in a High-Temperature
    Subdwarf.
Authors: Münch, Guido
Bibcode: 1958ApJ...127..642M
Altcode:
  The problem of line formation in a scheme of pure absorption is
  considered For the case of a source function depending linearly on
  mean optical depth, r, and a ratio, , of line to continuous absorption
  coefficients independent of r, an approximate expression for the
  line depth is derived similar in form to the Minnaert- interpolation
  formula It is shown that this formula, for a given equivalent width,
  underestimates the frequency-independent part of77 by a factor equal
  to the central depth of the line, both for lines broadened by linear
  Stark effect and for Doppler-broadened lines A procedure defining the
  mean level of formation of the various parts of the contour of a line
  with `7depending arbitrarily on r is developed. The representative
  depths for the formation of a line as a whole, when it is broadened by
  linear Stark effect, are also evaluated. The use of the theoretical
  developments is illustrated by an analysis of the lines He ii x 4686
  and H + He ii X 4340 observed in the spectrum of the 0-type subdwarf
  HZ 44. Preliminary values of the electron pressure, p (r = 23),
  the effective temperature, T , and the helium number abundance, Y,
  are derived from the observed strength of X 4686, its ratio to 4340,
  and the ionization equilibrium between the ions N Ir and N iii,
  assuming = Constant. On the basis of the model log p, = 4.0, T, =
  34000 K, and V = 0 28 thus obtained, the line intensities are again
  calculated, allowing for the r-dependence of 77. The parameters p, and
  T, of the zero approximation model atmosphere are found not to change
  significantly on this account; but the value of V is reduced to V = 0.23
  A surface gravity g = 10' 7 cm/sec2 and a visual absolute magnitude M,
  = +37 if the mass were 1 0 and M = +12 if = 10 0, are estimated.

