Author name code: stebbins
ADS astronomy entries on 2022-09-14
author:"Stebbins, Robin T." 
------------------------------------------------------------------------  

Title: Getting Ready for LISA: The Data, Support and Preparation
    Needed to Maximize US Participation in Space-Based Gravitational
    Wave Science
Authors: Holley-Bockelmann, Kelly; :; Bellovary, Jillian; Bender,
   Peter; Berti, Emanuele; Brown, Warren; Caldwell, Robert; Cornish, Neil;
   Darling, Jeremy; Digman, Matthew; Eracleous, Mike; Gultekin, Kayhan;
   Haiman, Zoltan; Holley-Bockelmann, Kelly; Key, Joey; Larson, Shane;
   Liu, Xin; McWilliams, Sean; Natarajan, Priyamvada; Shoemaker, David;
   Shoemaker, Deirdre; Smith, Krista Lynne; Soares-Santos, Marcelle;
   Robin; Stebbins
Bibcode: 2020arXiv201202650H
Altcode:
  The NASA LISA Study Team was tasked to study how NASA might support US
  scientists to participate and maximize the science return from the Laser
  Interferometer Space Antenna (LISA) mission. LISA is gravitational wave
  observatory led by ESA with NASA as a junior partner, and is scheduled
  to launch in 2034. Among our findings: LISA science productivity
  is greatly enhanced by a full-featured US science center and an open
  access data model. As other major missions have demonstrated, a science
  center acts as both a locus and an amplifier of research innovation,
  data analysis, user support, user training and user interaction. In
  its most basic function, a US Science Center could facilitate entry
  into LISA science by hosting a Data Processing Center and a portal for
  the US community to access LISA data products. However, an enhanced
  LISA Science Center could: support one of the parallel independent
  processing pipelines required for data product validation; stimulate
  the high level of research on data analysis that LISA demands; support
  users unfamiliar with a novel observatory; facilitate astrophysics
  and fundamental research; provide an interface into the subtleties
  of the instrument to validate extraordinary discoveries; train new
  users; and expand the research community through guest investigator,
  postdoc and student programs. Establishing a US LISA Science Center
  well before launch can have a beneficial impact on the participation
  of the broader astronomical community by providing training, hosting
  topical workshops, disseminating mock catalogs, software pipelines,
  and documentation. Past experience indicates that successful science
  centers are established several years before launch; this early adoption
  model may be especially relevant for a pioneering mission like LISA.

Title: Space based gravitational wave astronomy beyond LISA
Authors: Mueller, Guido; Baker, John; Barke, Simon; Bender, Peter L.;
   Berti, Emanuele; Caldwell, Robert; Conklin, John W.; Cornish, Neil;
   Ferrara, Elizabeth C.; Holley-Bockelmann, Kelly; Kamai, Brittany;
   Larson, Shane L.; Livas, Jeff; McWilliams, Sean T.; Mueller, Guido;
   Natarajan, Priyamvada; Rioux, Norman; Sankar, Shannon S.; Schnittman,
   Jeremy; Shoemaker, Deirdre; Slutsky, Jacob; Stebbins, Robin; Thorpe,
   Ira; Ziemer, John
Bibcode: 2019BAAS...51g.243M
Altcode: 2019astro2020U.243M; 2019arXiv190711305B
  This white paper surveys the science, technology and mission concepts
  for a gravitational wave mission beyond LISA. The proposed small
  scale activity is a technology development program that would support
  a range of concepts and a mission concept study to choose a specific
  mission concept for Astro2030.

Title: Building a Field: The Future of Astronomy with Gravitational
    Waves
Authors: Holley-Bockelmann, Kelly; Ziemer, John; Thorpe, Ira; Livas,
   Jeff; Conklin, John W.; Caldwell, Robert; Berti, Emanuele; McWilliams,
   Sean T.; Stebbins, Robin; Shoemaker, David; Ferrara, Elizabeth C.;
   Larson, Shane L.; Shoemaker, Deirdre; Key, Joey Shapiro; Eracleous,
   Michael; Schnittman, Jeremy; Baghi, Quentin; Kamai, Brittany; Mueller,
   Guido; Bellovary, Jillian; Rioux, Norman; Baker, John; Cutler, Curt;
   Natarajan, Priyamvada; Kelly, Bernard J.; Brandt, T. J.; Gabella,
   William; Jani, Karan
Bibcode: 2019BAAS...51g.228H
Altcode: 2019arXiv191207642H; 2019astro2020U.228H
  Harnessing the sheer discovery potential of GW Astronomy will require
  bold, deliberate, and sustained efforts to train and develop the
  requisite workforce. This basic infrastructure is needed as an enabling
  foundation for research. We outline a set of recommendations to help
  build a thriving, diverse, and inclusive new field.

Title: The Laser Interferometer Space Antenna: Unveiling the
    Millihertz Gravitational Wave Sky
Authors: Thorpe, James Ira; Ziemer, John; Thorpe, Ira; Livas, Jeff;
   Conklin, John W.; Caldwell, Robert; Berti, Emanuele; McWilliams,
   Sean T.; Stebbins, Robin; Shoemaker, David; Ferrara, Elizabeth C.;
   Larson, Shane L.; Shoemaker, Deirdre; Key, Joey Shapiro; Vallisneri,
   Michele; Eracleous, Michael; Schnittman, Jeremy; Kamai, Brittany;
   Camp, Jordan; Mueller, Guido; Bellovary, Jillian; Rioux, Norman;
   Baker, John; Bender, Peter L.; Cutler, Curt; Cornish, Neil; Hogan,
   Craig; Manthripragada, Sridhar; Ware, Brent; Natarajan, Priyamvada;
   Numata, Kenji; Sankar, Shannon R.; Kelly, Bernard J.; McKenzie, Kirk;
   Slutsky, Jacob; Spero, Robert; Hewitson, Martin; Francis, Samuel;
   DeRosa, Ryan; Yu, Anthony; Hornschemeier, Ann; Wass, Peter
Bibcode: 2019BAAS...51g..77T
Altcode: 2019arXiv190706482B; 2019astro2020U..77T
  This whitepaper summarizes the status of the ESA-led Laser
  Interferometer Space Antenna (LISA) mission and advocates for an
  increased US role within the ‘medium’ mission category. The LISA
  science case, mission concept, technical readiness, and organizational
  partnerships are summarized and broad scenarios for US participation
  are described.

Title: NASA's Preparations for ESA's L3 Gravitational Wave Mission
Authors: Stebbins, Robin
Bibcode: 2016APS..APRJ12003S
Altcode:
  The European Space Agency (ESA) selected gravitational-wave astrophysics
  as the science theme for its third large mission opportunity, known as
  `L3,' under its Cosmic Vision Programme. NASA is seeking a role as
  an international partner in L3. NASA is: (1) participating in ESA's
  early mission activities, (2) developing potential US technology
  contributions, (3) participating in ESA's LISA Pathfinder mission,
  (4) and conducting a study of how NASA might participate. This talk
  will survey the status of these activities.

Title: Mission and Instrument Design Trades for a Space-based
    Gravitational Wave Observatory to Maximize Science Return
Authors: Livas, Jeffrey; Baker, John; Stebbins, Robin; Thorpe, James;
   Larson, Shane; Sesana, Alberto
Bibcode: 2016APS..APRJ12005L
Altcode:
  A space-based gravitational wave observatory is required to access
  the rich array of astrophysical sources expected at frequencies
  between 0.0001 and 0.1 Hz. The European Space Agency (ESA) chose
  the Gravitational Universe as the science theme of its L3 launch
  opportunity. A call for mission proposals will be released soon after
  the completion of the LISA Pathfinder (LPF) mission. LPF is scheduled
  to start science operations in March 2016, and finish by the end of
  the year, so an optimized mission concept is needed now. There are
  a number of possible design choices for both the instrument and the
  mission. One of the goals for a good mission design is to maximize
  the science return while minimizing risk and keeping costs low. This
  presentation will review some of the main design choices for a LISA-like
  laser interferometry mission and the impact of these choices on cost,
  risk, and science return.

Title: NASA's Preparations for ESA's L3 Gravitational Wave Mission
Authors: Stebbins, Robin T.
Bibcode: 2016AAS...22740502S
Altcode:
  In November 2013, the European Space Agency (ESA) selected the science
  theme, the "Gravitational Universe," for its third large mission
  opportunity, known as 'L3,' under its Cosmic Vision Programme. The
  planned launch date is 2034. NASA is seeking a role as an international
  partner in L3. NASA is supporting: (1) US participation in early mission
  studies, (2) US technology development, (3) pre-decadal preparations,
  (4) ESA's LISA Pathfinder mission and (5) the ST7 Disturbance Reduction
  System project. This talk summarizes NASA's preparations for a future
  gravitational-wave mission.

Title: Progress Toward a Space-Based Gravitational Wave Observatory
Authors: Livas, Jeffrey C.; Stebbins, Robin T.
Bibcode: 2016IAUFM..29B.357L
Altcode:
  The discovery of binary pulsar PSR 1913+16 by Hulse &amp; Taylor
  in 1974 established the existence of gravitational waves, for
  which the 1983 Nobel Prize was awarded. However, the measurement
  of astrophysical parameters from gravitational waves will open an
  entirely new spectrum for discovery and understanding of the Universe,
  not simply a new window in the electromagnetic spectrum like gamma ray
  telescopes in the 1970s. Two types of ground-based detectors, Advanced
  LIGO/Virgo and Pulsar Timing Arrays, are expected to directly detect
  gravitational waves in their respective frequency bands before the
  end of the decade. However, many of the most exciting sources are in
  the band from 0.1-100 mHz, accessible only from space due to seismic
  and gravity gradient noise on Earth. The European Space Agency (ESA)
  has chosen the 'Gravitational Universe' as the science theme for its
  L3 Cosmic Visions opportunity, planned for launch in 2034. NASA is
  planning to participate as a junior partner. Here we summarize progress
  toward realizing a gravitational wave observatory in space.

Title: Status of a Space-Based Gravitational-Wave Observatory at NASA
Authors: Stebbins, Robin
Bibcode: 2015IAUGA..2257752S
Altcode:
  For over two decades, NASA has studied a flight project to build a
  gravitational-wave observatory, and partnered with the European Space
  Agency (ESA) to formulate and study such a mission. The spectacular
  science and the well-defined and well-studied Laser Interferometer
  Space Antenna (LISA) mission concept got high recommendations in
  the U.S. astrophysics decadal surveys of 2000 and 2010.In 2013, ESA
  selected the science theme, the “Gravitational Universe,” for the
  third large mission opportunity, known as L3, under its Cosmic Vision
  Programme. The planned launch date is 2034. ESA is considering a 20%
  participation by an international partner, and NASA's Astrophysics
  Division has begun negotiating a NASA role. The US research community
  has studied the design consequences of a NASA contribution, evaluated
  the science benefits and identified the technology requirements for
  hardware that could be delivered by NASA.This talk will describe the
  current state of: mission concept studies, US participation in an
  ESA-led study, technology development, other relevant activities and
  preparation for the 2020 decadal survey.

Title: The Gravitational Universe - ESA's L3 mission
Authors: Mueller, Guido; Ando, Masaki; Binetruy, Pierre; Bouyer,
   Philippe; Cacciapuoti, Luigi; Cruise, Mike; Favata, Fabio; Gehler,
   Martin; Genzel, Reinhard; Jennrich, Oliver; Kasevich, Mark; Klipstein,
   Bill; Perryman, Michael; Safa, Frederic; Schutz, Bernard; Stebbins,
   Robin; Vitale, Stefano
Bibcode: 2015APS..APR.U7001M
Altcode:
  Following the advice of ESA's Senior Survey Committee (SSC)
  the Science Programme Committee (SPC) decided in November 2013 to
  select the science theme ``The Gravitational Universe'' for their L3
  mission. The Director of Science and Robotic Exploration (D/SRE) has
  established a Gravitational Observatory Advisory Team (GOAT) to advise
  on the scientific and technological approaches for a gravitational
  wave observatory with a planned launch date in 2034. Our team is
  comprised of scientists from Europe and the US as well as scientists
  and engineers from ESA and observers from NASA and JAXA. We meet about
  every ten weeks, evaluate the technical readiness of all necessary
  technologies, study the science impact of different mission designs,
  and will advise ESA on the required future technology development. We
  will report on our progress and plans forward to a future space-based
  gravitational-wave observatory. <P />For JAXA.

Title: Architectures for a Space-based Gravitational-Wave Observatory
Authors: Stebbins, Robin
Bibcode: 2015APS..APR.U7004S
Altcode:
  The European Space Agency (ESA) selected the science theme, the
  ``Gravitational Universe,'' for the third large mission opportunity,
  known as L3, under its Cosmic Vision Programme. The planned launch date
  is 2034. ESA is considering a 20% participation by an international
  partner, and NASA's Astrophysics Division has begun negotiating a NASA
  role. We have studied the design consequences of a NASA contribution,
  evaluated the science benefits and identified the technology
  requirements for hardware that could be delivered by NASA. The
  European community proposed a strawman mission concept, called eLISA,
  having two measurement arms, derived from the well studied LISA (Laser
  Interferometer Space Antenna) concept. The US community is promoting
  a mission concept known as SGO Mid (Space-based Gravitational-wave
  Observatory Mid-sized), a three arm LISA-like concept. If NASA were to
  partner with ESA, the eLISA concept could be transformed to SGO Mid
  by the addition of a third arm, thereby augmenting science, reducing
  risk and reducing non-recurring engineering costs. The characteristics
  of the mission concepts and the relative science performance of eLISA,
  SGO Mid and LISA are described.

Title: Future Gravitational-Wave Missions
Authors: Stebbins, Robin T.; NASA Gravitational-Wave Study Team
Bibcode: 2015AAS...22533844S
Altcode:
  In November 2013, the European Space Agency (ESA) selected the science
  theme, the 'Gravitational Universe,' for its third large mission
  opportunity, known as L3, under its Cosmic Vision Programme. The
  planned launch date is 2034. ESA is considering a 20% participation by
  an international partner, and NASA's Astrophysics Division has indicated
  an interest in participating. We have studied the design consequences of
  a NASA contribution, evaluated the science benefits and identified the
  technology requirements for hardware that could be delivered by NASA.The
  European community proposed a strawman mission concept, called eLISA,
  having two measurement arms, derived from the well studied LISA (Laser
  Interferometer Space Antenna) concept. The US community is promoting
  a mission concept known as SGO Mid (Space-based Gravitational-wave
  Observatory Mid-sized), a three arm LISA-like concept. If NASA were
  to partner with ESA, the eLISA concept could be transformed to SGO
  Mid by the addition of a third arm, augmenting science, reducing risk
  and reducing non-recurring engineering costs. The characteristics of
  the mission concepts and the relative science performance of eLISA,
  SGO Mid and LISA are described. Note that all results are based on
  models, methods and assumptions used in NASA studies.

Title: Gravitational-wave Missions at NASA
Authors: Stebbins, Robin; McNamara, Paul; Jennrich, Oliver
Bibcode: 2014cosp...40E3193S
Altcode:
  In November 2013, ESA selected the science theme, the “Gravitational
  Universe,” for its third large mission opportunity, known as L3, under
  its Cosmic Visions Programme. The planned launch date is 2034. ESA is
  considering a 20% participation by an international partner, and NASA's
  Astrophysics Division has indicated an interest in participating. We
  have studied the design consequences of a NASA contribution,
  evaluated the science benefits and identified the technology
  requirements for hardware that could be delivered by NASA. The
  European community proposed a strawman mission concept, called eLISA,
  having two measurement arms, derived from the well studied LISA (Laser
  Interferometer Space Antenna) concept. The US community is promoting
  a mission concept known as SGO Mid (Space-based Gravitational-wave
  Observatory Mid-sized), a three arm LISA-like concept. If NASA were
  to partner with ESA, the eLISA concept could be transformed to SGO
  Mid by the addition of a third arm, augmenting science, reducing risk
  and reducing non-recurring engineering costs. The characteristics of
  the mission concepts and the relative science performance of eLISA,
  SGO Mid and LISA are described.

Title: eLISA: Astrophysics and cosmology in the millihertz regime
Authors: Amaro-Seoane, Pau; Aoudia, Sofiane; Babak, Stanislav;
   Binétruy, Pierre; Berti, Emanuele; Bohé, Alejandro; Caprini,
   Chiara; Colpi, Monica; Cornish, Neil J.; Danzmann, Karsten; Dufaux,
   Jean-François; Gair, Jonathan; Hinder, Ian; Jennrich, Oliver;
   Jetzer, Philippe; Klein, Antoine; Lang, Ryan N.; Lobo, Alberto;
   Littenberg, Tyson; McWilliams, Sean T.; Nelemans, Gijs; Petiteau,
   Antoine; Porter, Edward K.; Schutz, Bernard F.; Sesana, Alberto;
   Stebbins, Robin; Sumner, Tim; Vallisneri, Michele; Vitale, Stefano;
   Volonteri, Marta; Ward, Henry; Wardell, Barry
Bibcode: 2013GWN.....6....4A
Altcode: 2012arXiv1201.3621A
  This document introduces the exciting and fundamentally new science and
  astronomy that the European New Gravitational Wave Observatory (NGO)
  mission (derived from the previous LISA proposal) will deliver. The
  mission (which we will refer to by its informal name ``eLISA'')
  will survey for the first time the low-frequency gravitational wave
  band (about 0:1 mHz to 1 Hz), with sufficient sensitivity to detect
  interesting individual astrophysical sources out to z = 15. The
  measurements described here will address the basic scientific goals
  that have been captured in ESA's ``New Gravitational Wave Observatory
  Science Requirements Document''; they are presented here so that the
  wider scientific community can have access to them. The eLISA mission
  will discover and study a variety of cosmic events and systems with
  high sensitivity: coalescences of massive black holes binaries, brought
  together by galaxy mergers; mergers of earlier, less-massive black
  holes during the epoch of hierarchical galaxy and black-hole growth;
  stellar-mass black holes and compact stars in orbits just skimming the
  horizons of massive black holes in galactic nuclei of the present era;
  extremely compact white dwarf binaries in our Galaxy, a rich source of
  information about binary evolution and about future Type Ia supernovae;
  and possibly most interesting of all, the uncertain and unpredicted
  sources, for example relics of inflation and of the symmetry-breaking
  epoch directly after the Big Bang. eLISA's measurements will allow
  detailed studies of these signals with high signal-to-noise ratio,
  addressing most of the key scientific questions raised by ESA's Cosmic
  Vision programme in the areas of astrophysics and cosmology. They will
  also provide stringent tests of general relativity in the strong-field
  dynamical regime, which cannot be probed in any other way. This document
  not only describes the science but also gives an overview on the mission
  design and orbits. LISA's heritage in the eLISA design will be clear to
  those familiar with the previous proposal, as will its incorporation of
  key elements of hardware from the LISA Pathfinder mission, scheduled
  for launch by ESA in 2014. But eLISA is fundamentally a new mission,
  one that will pioneer the completely new science of low-frequency
  gravitational wave astronomy.

Title: The Gravitational Universe
Authors: eLISA Consortium; Amaro Seoane, P.; Aoudia, S.; Audley, H.;
   Auger, G.; Babak, S.; Baker, J.; Barausse, E.; Barke, S.; Bassan, M.;
   Beckmann, V.; Benacquista, M.; Bender, P. L.; Berti, E.; Binétruy, P.;
   Bogenstahl, J.; Bonvin, C.; Bortoluzzi, D.; Brause, N. C.; Brossard,
   J.; Buchman, S.; Bykov, I.; Camp, J.; Caprini, C.; Cavalleri, A.;
   Cerdonio, M.; Ciani, G.; Colpi, M.; Congedo, G.; Conklin, J.; Cornish,
   N.; Danzmann, K.; de Vine, G.; DeBra, D.; Dewi Freitag, M.; Di Fiore,
   L.; Diaz Aguilo, M.; Diepholz, I.; Dolesi, R.; Dotti, M.; Fernández
   Barranco, G.; Ferraioli, L.; Ferroni, V.; Finetti, N.; Fitzsimons,
   E.; Gair, J.; Galeazzi, F.; Garcia, A.; Gerberding, O.; Gesa, L.;
   Giardini, D.; Gibert, F.; Grimani, C.; Groot, P.; Guzman Cervantes, F.;
   Haiman, Z.; Halloin, H.; Heinzel, G.; Hewitson, M.; Hogan, C.; Holz,
   D.; Hornstrup, A.; Hoyland, D.; Hoyle, C. D.; Hueller, M.; Hughes,
   S.; Jetzer, P.; Kalogera, V.; Karnesis, N.; Kilic, M.; Killow, C.;
   Klipstein, W.; Kochkina, E.; Korsakova, N.; Krolak, A.; Larson, S.;
   Lieser, M.; Littenberg, T.; Livas, J.; Lloro, I.; Mance, D.; Madau, P.;
   Maghami, P.; Mahrdt, C.; Marsh, T.; Mateos, I.; Mayer, L.; McClelland,
   D.; McKenzie, K.; McWilliams, S.; Merkowitz, S.; Miller, C.; Mitryk,
   S.; Moerschell, J.; Mohanty, S.; Monsky, A.; Mueller, G.; Müller,
   V.; Nelemans, G.; Nicolodi, D.; Nissanke, S.; Nofrarias, M.; Numata,
   K.; Ohme, F.; Otto, M.; Perreur-Lloyd, M.; Petiteau, A.; Phinney,
   E. S.; Plagnol, E.; Pollack, S.; Porter, E.; Prat, P.; Preston, A.;
   Prince, T.; Reiche, J.; Richstone, D.; Robertson, D.; Rossi, E. M.;
   Rosswog, S.; Rubbo, L.; Ruiter, A.; Sanjuan, J.; Sathyaprakash, B. S.;
   Schlamminger, S.; Schutz, B.; Schütze, D.; Sesana, A.; Shaddock,
   D.; Shah, S.; Sheard, B.; Sopuerta, C. F.; Spector, A.; Spero, R.;
   Stanga, R.; Stebbins, R.; Stede, G.; Steier, F.; Sumner, T.; Sun,
   K. -X.; Sutton, A.; Tanaka, T.; Tanner, D.; Thorpe, I.; Tröbs, M.;
   Tinto, M.; Tu, H. -B.; Vallisneri, M.; Vetrugno, D.; Vitale, S.;
   Volonteri, M.; Wand, V.; Wang, Y.; Wanner, G.; Ward, H.; Ware, B.;
   Wass, P.; Weber, W. J.; Yu, Y.; Yunes, N.; Zweifel, P.
Bibcode: 2013arXiv1305.5720E
Altcode: 2013arXiv1305.5720C; 2013arXiv1305.5720D
  The last century has seen enormous progress in our understanding of the
  Universe. We know the life cycles of stars, the structure of galaxies,
  the remnants of the big bang, and have a general understanding of how
  the Universe evolved. We have come remarkably far using electromagnetic
  radiation as our tool for observing the Universe. However, gravity is
  the engine behind many of the processes in the Universe, and much of
  its action is dark. Opening a gravitational window on the Universe will
  let us go further than any alternative. Gravity has its own messenger:
  Gravitational waves, ripples in the fabric of spacetime. They travel
  essentially undisturbed and let us peer deep into the formation of
  the first seed black holes, exploring redshifts as large as z ~ 20,
  prior to the epoch of cosmic re-ionisation. Exquisite and unprecedented
  measurements of black hole masses and spins will make it possible to
  trace the history of black holes across all stages of galaxy evolution,
  and at the same time constrain any deviation from the Kerr metric of
  General Relativity. eLISA will be the first ever mission to study the
  entire Universe with gravitational waves. eLISA is an all-sky monitor
  and will offer a wide view of a dynamic cosmos using gravitational waves
  as new and unique messengers to unveil The Gravitational Universe. It
  provides the closest ever view of the early processes at TeV energies,
  has guaranteed sources in the form of verification binaries in the Milky
  Way, and can probe the entire Universe, from its smallest scales around
  singularities and black holes, all the way to cosmological dimensions.

Title: A Possible U.S. Contribution to eLISA, a Gravitational-Wave
    Mission Concept for ESA’s L2 Opportunity
Authors: Stebbins, Robin T.
Bibcode: 2013HEAD...1312104S
Altcode:
  Scientists from the member states of the European Space Agency
  (ESA) that proposed the New Gravitational Wave Observatory (NGO) have
  organized the eLISA Consortium to propose for ESA's next large mission
  opportunity, called L2. The Evolved Laser Interferometer Space Antenna
  (eLISA) concept is derived from the well studied LISA concept for a
  space-based, gravitational-wave mission. eLISA will use the technology
  being developed in the LISA Pathfinder mission in a two-arm version that
  achieves much of the LISA science endorsed by the Decadal Survey. If
  invited, NASA could join the project as a junior partner with a ~15%
  share. This could enable a third arm and substantially augment the
  science return. While the details of the eLISA concept to be proposed
  have not yet been finalized, the SGO Mid concept, recently studied
  in the U.S., constitutes a possible augmented concept for an ESA/NASA
  partnership. The eLISA concept and the SGO Mid concept are described
  and compared.

Title: Status of eLISA
Authors: Stebbins, Robin T.; Jennrich, O.; Consortium, eLISA
Bibcode: 2013AAS...22115305S
Altcode:
  Scientists from the member states of the European Space Agency
  (ESA) that proposed the New Gravitational Wave Observatory (NGO)
  are organizing the eLISA Consortium to propose for the next large
  mission opportunity. The Evolved Laser Interferometer Space Antenna
  (eLISA) concept is derived from the well studied LISA concept for a
  space-based, gravitational-wave mission. eLISA will use the technology
  being developed in the LISA Pathfinder mission in a two-arm version that
  achieves much of the science of LISA. eLISA will: (1) survey very many
  compact stellar-mass binaries and study the structure of the Milky Way;
  (2) discover black holes formed at early epochs that grew over cosmic
  time to generate the supermassive black holes present in most galactic
  nuclei today; (3) trace the interaction of galaxy growth and massive
  black hole growth over the entire history of galaxy formation; (4)
  explore the populations of stellar-mass compact objects in galactic
  nuclei and their dynamics; (5) observe highly relativistic coalescences
  of black hole binaries, and provide exceptionally strong tests of
  the predictions of General Relativity; and (6) probe new physics and
  cosmology with gravitational waves, and search for unforeseen sources
  of gravitational waves. The key parameters of the design concept and a
  quantitative assessment of the science performance are given. NASA and
  the U.S. research community may be able to participate, and possibly
  extend the capabilities of the mission.

Title: NASA's Gravitational-Wave Mission Concept Study
Authors: Stebbins, Robin; Jennrich, Oliver; McNamara, Paul
Bibcode: 2012cosp...39.1890S
Altcode: 2012cosp.meet.1890S
  With the conclusion of the NASA/ESA partnership on the Laser
  interferometer Space Antenna (LISA) Project, NASA initiated a study to
  explore mission concepts that will accomplish some or all of the LISA
  science objectives at lower cost. The Gravitational-Wave Mission Concept
  Study consisted of a public Request for Information (RFI), a Core Team
  of NASA engineers and scientists, a Community Science Team, a Science
  Task Force, and an open workshop. The RFI yielded were 12 mission
  concepts, 3 instrument concepts and 2 technologies. The responses
  ranged from concepts that eliminated the drag-free test mass of LISA to
  concepts that replace the test mass with an atom interferometer. The
  Core Team reviewed the noise budgets and sensitivity curves, the
  payload and spacecraft designs and requirements, orbits and trajectories
  and technical readiness and risk. The Science Task Force assessed the
  science performance by calculating the horizons, the detection rates and
  the accuracy of astrophysical parameter estimation for massive black
  hole mergers, stellar-mass compact objects inspiraling into central
  engines, and close compact binary systems. Three mission concepts have
  been studied by Team-X, JPL's concurrent design facility, to define
  a conceptual design, evaluate key performance parameters, assess risk
  and estimate cost and schedule. The Study results are summarized.

Title: Low-frequency gravitational-wave science with eLISA/NGO
Authors: Amaro-Seoane, Pau; Aoudia, Sofiane; Babak, Stanislav;
   Binétruy, Pierre; Berti, Emanuele; Bohé, Alejandro; Caprini,
   Chiara; Colpi, Monica; Cornish, Neil J.; Danzmann, Karsten; Dufaux,
   Jean-François; Gair, Jonathan; Jennrich, Oliver; Jetzer, Philippe;
   Klein, Antoine; Lang, Ryan N.; Lobo, Alberto; Littenberg, Tyson;
   McWilliams, Sean T.; Nelemans, Gijs; Petiteau, Antoine; Porter, Edward
   K.; Schutz, Bernard F.; Sesana, Alberto; Stebbins, Robin; Sumner, Tim;
   Vallisneri, Michele; Vitale, Stefano; Volonteri, Marta; Ward, Henry
Bibcode: 2012CQGra..29l4016A
Altcode: 2012arXiv1202.0839A
  We review the expected science performance of the New Gravitational-Wave
  Observatory (NGO, a.k.a. eLISA), a mission under study by the European
  Space Agency for launch in the early 2020s. eLISA will survey the
  low-frequency gravitational-wave sky (from 0.1 mHz to 1 Hz), detecting
  and characterizing a broad variety of systems and events throughout
  the Universe, including the coalescences of massive black holes brought
  together by galaxy mergers; the inspirals of stellar-mass black holes
  and compact stars into central galactic black holes; several millions
  of ultra-compact binaries, both detached and mass transferring,
  in the Galaxy; and possibly unforeseen sources such as the relic
  gravitational-wave radiation from the early Universe. eLISA’s high
  signal-to-noise measurements will provide new insight into the structure
  and history of the Universe, and they will test general relativity in
  its strong-field dynamical regime.

Title: Plans For A Next Generation Space-based Gravitational-wave
    Observatory (NGO)
Authors: Livas, Jeffrey C.; Stebbins, R. T.; Jennrich, O.; NGO Mission
   Development Team
Bibcode: 2012AAS...21914626L
Altcode:
  The European Space Agency (ESA) is currently in the process of selecting
  a mission for the Cosmic Visions Program. A space-based gravitational
  wave observatory in the low-frequency band (0.0001 - 1 Hz) of the
  gravitational wave spectrum is one of the leading contenders. This
  low frequency band has a rich spectrum of astrophysical sources, and
  the LISA concept has been the key mission to cover this science for
  over twenty years. Tight budgets have recently forced ESA to consider
  a reformulation of the LISA mission concept that will allow the Cosmic
  Visions Program to proceed on schedule either with the US as a minority
  participant, or independently of the US altogether. We report on the
  status of these reformulation efforts.

Title: Concepts For A Space-based Gravitational-wave Observatory (SGO)
Authors: Stebbins, Robin T.; Gravitational Wave Concept Definition Team
Bibcode: 2012AAS...21914624S
Altcode:
  The low-frequency band (0.0001 - 1 Hz) of the gravitational wave
  spectrum has the most interesting astrophysical sources. It is only
  accessible from space. The Laser Interferometer Space Antenna (LISA)
  concept has been the leading contender for a space-based detector in
  this band. Despite a strong recommendation from Astro2010, constrained
  budgets motivate the search for a less expensive concept, even at the
  loss of some science. We have explored the range of lower-cost mission
  concepts derived from two decades of studying the LISA concept. We
  describe LISA-like concepts that span the range of affordable and
  scientifically worthwhile missions, and summarize the analyses behind
  them.

Title: New Concepts for Space-Based Gravitational Wave Missions
Authors: Stebbins, Robin T.; Baker, J. G.; Cooley, D.; Gallagher,
   R. J.; Hughes, S. P.; Livas, J. C.; Simpson, J. E.; Thorpe, J. I.;
   Welter, G. L.
Bibcode: 2011HEAD...12.0902S
Altcode:
  The most interesting astrophysical sources in the gravitational wave
  spectrum lie in the low-frequency band (0.0001 - 1 Hz), which is only
  accessible from space. For two decades, the LISA concept has been
  the leading contender for a detector in this band. Despite a strong
  recommendation from Astro2010, there is strong motivation to find a less
  expensive concept, even at the loss of some science. We are searching
  for a lower cost mission concept by examining alternate orbits,
  less-capable measurement concepts, radically different implementations
  of the measurement concept and other cost-saving ideas. We report the
  results of our searches to date, and summarize the analyses behind them.

Title: Characterization of photoreceivers for LISA
Authors: Guzmán Cervantes, F.; Livas, J.; Silverberg, R.; Buchanan,
   E.; Stebbins, R.
Bibcode: 2011CQGra..28i4010G
Altcode: 2012arXiv1203.2862G
  LISA will use quadrant photoreceivers as front-end devices for the
  phasemeter measuring the motion of drag-free test masses in both angular
  orientation and separation. We have set up a laboratory testbed for the
  characterization of photoreceivers. Some of the limiting noise sources
  have been identified and their contribution has been either measured
  or derived from the measured data. We have built a photoreceiver with
  a 0.5 mm diameter quadrant photodiode with an equivalent input current
  noise of better than 1.8 pA Hz<SUP>-1/2</SUP> below 20 MHz and a 3 dB
  bandwidth of 34 MHz.

Title: Preliminary Investigations of an Optical Assembly Tracking
    Mechansim for LISA
Authors: Ira Thorpe, James; Stebbins, Robin
Bibcode: 2010cosp...38.3793I
Altcode: 2010cosp.meet.3793I
  After injection into their specific orbits, the position of the
  LISA spacecraft are not actively controlled. Rather the spacecraft
  are allowed to passively follow their trajectories and the roughly
  equilateral triangular constellation is preserved. Slight variations
  in the orbits cause the constellation to experience both periodic and
  secular variations, one consequence of which is a variation in the
  interior angles of the constellation on the order of one degree. This
  variation is larger than the field of view of the LISA telescope,
  requiring a mechanism for each spacecraft to maintain pointing to its
  two companions. This Optical Assembly Tracking Mechanism (OATM) will
  be used to accommodate these variations while maintaining pointing at
  the ten nanoradian level to the far spacecraft. Here we report on a
  possible design for the OATM as well as initial results from a test
  campaign of a piezo-inchworm actuator used to drive the mechanism.

Title: LISA Technology Development, Risk Reduction and Mission
    Formulation at NASA
Authors: Stebbins, Robin; Ziemer, John; Livas, Jeffrey; Ira Thorpe,
   James; Merkowitz, Stephen
Bibcode: 2010cosp...38.3757S
Altcode: 2010cosp.meet.3757S
  The Laser Interferometer Space Antenna (LISA) is a joint ESA-NASA
  project to design, build and operate a space-based gravitational wave
  detector based on a laser interferometer. LISA relies on several
  technologies that are either new to spaceflight or must perform at
  levels not previously demonstrated in a spaceflight environment. The
  ESA-led LISA Pathfinder mission is the main effort to demonstrate LISA
  technology. NASA also supports complementary ground-based technology
  development and risk reduction activities. This presentation will
  report the status of NASA work on micronewton thrusters, the telescope,
  the optical pointing subsystem and mission formulation. More details
  on some of these topics will be given in posters. Other talks and
  posters will describe NASA-supported work on the laser subsystem, the
  phasemeter, and aspects of the interferometry. Two flight-qualified
  clusters of four colloid micronewton thrusters, each capable of thrust
  levels between 5 and 30 µN with a resolution ¡0.1 µN and a thrust
  noise ¡0.1 µN/sqrtHz (0.001 to 4 Hz), have been integrated onto the
  LISA Pathfinder spacecraft. The complementary ground-based development
  focuses on lifetime demonstration. Laboratory verification of failure
  models and accelerated life tests are just getting started. LISA
  needs a 40 cm diameter, afocal telescope for beam expansion/reduction
  that maintains an optical pathlength stability of 1 pm/sqrtHz in
  an extremely stable thermal environment. A mechanical prototype of
  a silicon carbide primary-secondary structure has been fabricated
  for stability testing. Two optical assemblies must point at different
  distant spacecraft with nanoradian accuracy over 1° annual variation in
  the angle between the distant spacecraft. A candidate piezo-inchworm
  actuator is being tested in a suitable testbed. In addition to
  technology development, NASA has carried out several studies in support
  of the mission formulation. The results of systems engineering work
  on flight software, avionics and reliability will be summarized.

Title: Instrumentation and Technology for the Laser Interferometer
    Space Antenna (LISA)
Authors: Prince, Thomas Allen; Jennrich, O.; Klipstein, W.; Livas,
   J.; McNamara, P.; Merkowitz, S.; Sallusti, M.; Stebbins, R.
Bibcode: 2010AAS...21548210P
Altcode: 2010BAAS...42..575P
  This poster discusses the present status of the technology and
  instrumentation for the joint ESA/NASA gravitational wave detector,
  LISA, focusing on&amp;nbspa description of the main payload items, such
  as: (1) the interferometric measurement system, comprising the optical
  system, which includes the optical bench and the telescope, the laser
  system, and the phase measurement system; and, (2) the disturbance
  reduction system, including the gravitational reference sensor, the
  charge control system, and the micro-propulsion&amp;nbspsystem.

Title: Preliminary LISA telescope spacer design
Authors: Livas, Jeffrey; Stebbins, Robin; Arsenovic, Petar;
   Castellucci, Kevin; Generie, Joseph; Howard, Joseph; Mueller, Guido;
   Preston, Alix; Sanjuan, Josep; Williams, Luke
Bibcode: 2010cosp...38.3783L
Altcode: 2010cosp.meet.3783L
  The LISA mission observes gravitational waves by measuring the
  separations between freely floating proof masses located 5 million
  kilometers apart with an accuracy of 10 picometers. The separations are
  measured interferometrically. The telescope is an afocal Cassegrain
  style design with a magnification of 80x. The entrance pupil has
  a 40 cm diameter and will either be centered on-axis or de-centered
  off-axis to avoid obscurations. Its two main purposes are to transform
  the small diameter beam used on the optical bench to a diffraction
  limited collimated beam to efficiently transfer the metrology laser
  between spacecraft, and to receive the incoming light from the far
  spacecraft. It transmits and receives simultaneously. The basic optical
  design and requirements are well understood for a conventional telescope
  design for imaging applications, but the LISA design is complicated
  by the additional requirement that the total optical path through the
  telescope must remain stable at the picometer level over the measurement
  band during the mission to meet the measurement accuracy. This poster
  describes the requirements for the telescope and the preliminary
  work that has been done to understand the materials and mechanical
  issues associated with the design of a passive metering structure to
  support the telescope and to maintain the spacing between the primary
  and secondary mirrors in the LISA on-orbit environment. This includes
  the requirements flowdown from the science goals, thermal modeling of
  the spacecraft and telescope to determine the expected temperature
  distribution, layout options for the telescope including an on-and
  off-axis design, and plans for fabrication and testing.

Title: The LISA Pathfinder Mission
Authors: Stebbins, Robin T.; LISA Pathfinder Science Working Team
Bibcode: 2010AAS...21548214S
Altcode: 2010BAAS...42..575S
  LISA Pathfinder (formerly known as SMART-2) is a European Space Agency
  (ESA) mission designed to pave the way for the joint ESA/NASA Laser
  Interferometer Space Antenna (LISA) mission by testing in flight the
  critical technologies required for space-borne gravitational wave
  detection: it will put two test masses in a near-perfect gravitational
  free-fall and control and measure their motion with unprecedented
  accuracy. <P />LISA Pathfinder is currently in the integration and
  test phase of the development, and is due to be launched on a dedicated
  launch vehicle in late 2011, with first results on the performance of
  the system being available approximately 6 months later. <P />This
  poster will describe the mission in detail, give the current status
  of the spacecraft development, and highlight the future milestones in
  the integration and test campaign.

Title: LISA telescope spacer design investigations
Authors: Sanjuan, Josep; Mueller, Guido; Livas, Jeffrey; Preston,
   Alix; Arsenovic, Petar; Castellucci, Kevin; Generie, Joseph; Howard,
   Joseph; Stebbins, Robin
Bibcode: 2010cosp...38.3791S
Altcode: 2010cosp.meet.3791S
  The Laser Interferometer Space Antenna (LISA) is a space-based
  gravitational wave observa-tory with the goal of observing Gravitational
  Waves (GWs) from astronomical sources in a frequency range from 30
  µHz to 0.1 Hz. The detection of GWs at such low frequency requires
  measurements of distances at the pico-meter level between bodies
  separated by 5 million kilo-meters. The LISA mission consists of
  three identical spacecraft (SC) separated by 5 × 106 km forming an
  equilateral triangle. Each SC contains two optical assemblies and
  two vacuum en-closures housing one proof mass (PM) in geodesic (free
  fall) motion each. The two assemblies on one SC are each pointing
  towards an identical assembly on each of the other two SC to form
  a non-equal arm interferometer. The measurement of the GW strain is
  done by measuring the change in the length of the optical path between
  the PMs of one arm relative to the other arms caused by the pass of a
  GW. An important element of the Interferometric Measurement System (IMS)
  is the telescope which, on one hand, gathers the light coming from the
  far SC (∼100 pW) and, on the other hand, expands and collimates the
  small outgoing beam ( 1 W) and sends it to the far SC. Due to the very
  demanding sensitivity requirements care must be taken in the design and
  validation of the telescope not to degrade the IMS performance. For
  instance, the diameter of the telescope sets the the shot noise of
  the IMS and depends critically on the diameter of the primary and the
  divergence angle of the outgoing beam. As the telescope is rather fast
  telescope, the divergence angle is a critical function of the overall
  separation between the primary and secondary. Any long term changes of
  the distance of more than a a few micro-meter would be detrimental
  to the LISA mission. Similarly challenging are the requirements
  on the in-band path-length noise for the telescope which has to be
  kept below 1 pm Hz-1/2 in the LISA band. Different configurations
  (on-axis/off axis) and materials such as Silicon Carbide (SiC) and
  Carbon Fiber Reinforced Plastic (CFRP) are considered to be used in the
  telescope spacer structure. We will describe our experimental efforts
  to understand and quantify the behavior of different materials and
  also discuss a first investigation of a specific on-axis SiC telescope
  spacer for LISA. This work is supported by NASA contract 00069955.

Title: Rightsizing LISA
Authors: Stebbins, R. T.
Bibcode: 2009CQGra..26i4014S
Altcode: 2009arXiv0904.1029S
  The Laser Interferometer Space Antenna (LISA) science requirements
  and conceptual design have been fairly stable for over a decade. In
  the interest of reducing costs, the LISA Project at NASA has looked
  for simplifications of the architecture, at downsizing of subsystems
  and at descopes of the entire mission. This is a natural activity
  of the formulation phase and one that is particularly timely in
  the current NASA budgetary context. There is, and will continue to
  be, enormous pressure for cost reduction from both ESA and NASA,
  reviewers and the broader research community. Here, the rationale
  for the baseline architecture is reviewed, and recent efforts to find
  simplifications and other reductions that might lead to savings are
  reported. A few possible simplifications have been found in the LISA
  baseline architecture. In the interest of exploring cost sensitivity,
  one moderate and one aggressive descope have been evaluated; the cost
  savings are modest and the loss of science is not.

Title: LISA Pathfinder
Authors: Stebbins, Robin T.; McNamara, P. W.
Bibcode: 2009AAS...21344906S
Altcode: 2009BAAS...41Q.341S
  LISA Pathfinder, formerly known as SMART-2, is the second of the
  European Space Agency's Small Missions for Advanced Research and
  Technology. The mission will pave the way for the joint ESA/NASA Laser
  Interferometer Space Antenna (LISA), by testing the core assumption
  of gravitational wave detection - and to a larger extent, General
  Relativity - that free particles follow geodesics. <P />In order to meet
  the goals of the mission, and to prepare the way for LISA, several new
  technologies must be demonstrated in a space environment. These include:
  inertial sensors, high-precision laser metrology, drag-free control and
  micro-Newton proportional thrusters. <P />LISA Pathfinder will carry
  two payloads: the LISA Technology Package (LTP), provided by European
  Member States and ESA, and the Disturbance Reduction System (DRS)
  provided by NASA. The DRS has passed its pre-ship acceptance review
  and has been delivered to ESA, while the LTP has passed its Critical
  Design Review, with flight hardware currently being manufactured and
  tested. <P />The spacecraft development is also proceeding well; the
  flight structures of both the science module and propulsion module
  are undergoing environmental testing, while subsystem flight hardware
  is being delivered to the spacecraft testbeds. <P />LISA Pathfinder
  will be launched on a dedicated launch vehicle in late 2010. After
  15 apogee raising manoeuvres, the sciencecraft will enter its final
  orbit around the first Sun-Earth Lagrange point. First science results
  are expected approximately three months after launch. <P />Here we
  will give an overview of the mission including the technologies being
  demonstrated. We will also report on the status of the flight hardware
  testing, and on the status of the ground system.

Title: Recent progress at NASA in LISA formulation and technology
    development
Authors: Stebbins, R. T.
Bibcode: 2008CQGra..25k4050S
Altcode:
  Over the last year, the NASA half of the joint LISA project has
  focused its efforts on responding to a major review, and advancing
  the formulation and technology development of the mission. The
  NAS/NRC Beyond Einstein program assessment review will be described,
  including the outcome. The basis of the LISA science requirements
  has changed from detection determined by integrated signal-to-noise
  ratio to observation determined by uncertainty in the estimation of
  astrophysical source parameters. The NASA team has further defined the
  spacecraft bus design, participated in many design trade studies and
  advanced the requirements flow down and the associated current best
  estimates of performance. Recent progress in technology development
  is also summarized.

Title: Astrophysics At z 10 With Gravitational Waves
Authors: Stebbins, Robin T.
Bibcode: 2008HEAD...10.0602S
Altcode:
  What astrophysics can be done at redshifts beyond 5 using gravitational
  waves? Historically, gravitational wave antennas have been characterized
  by their detection capability. This is measured in terms of signal-noise
  ratio, and implies a rate of false positives and false negatives. But
  to do useful astrophysics, one would like to measure - or more
  properly, estimate - astrophysical parameters of the gravitational wave
  sources. In the interest of strengthening the connection between science
  objectives and a specific instrument performance, the LISA community
  has reformulated the LISA science requirements around the anticipated
  uncertainty in astrophysical parameter estimation. The rationale for
  this characterization of LISA and a summary of the astrophysics that
  LISA can do will be given.

Title: LISA Technology Development at GSFC
Authors: Thorpe, James Ira; Livas, Jeffrey; Stebbins, Robin
Bibcode: 2008cosp...37.3184T
Altcode: 2008cosp.meet.3184T
  The prime focus of LISA technology development efforts at NASA/GSFC
  has been in LISA interferometry, specifically in the area of laser
  frequency noise mitigation. Laser frequency noise is addressed through
  a combination of stabilization and common-mode rejection. Current
  plans call for two stages of stabilization, pre-stabilization to
  a local frequency reference and further stabilization using the
  constellation as a frequency reference. In order for these techniques
  to be used simultaneously, the pre-stabilization step must provide an
  adjustable frequency offset. Here we report on a modification to the
  standard modulation/demodulation technique used to stabilize to optical
  cavities that generates a frequency-tunable reference from a fixedlength
  cavity. This technique requires no modifications to the cavity itself
  and only minor modifications to the components. The measured noise
  performance and dynamic range of the laboratory prototype meet the
  LISA requirements.

Title: Science requirements for LISA
Authors: Stebbins, Robin
Bibcode: 2008cosp...37.3029S
Altcode: 2008cosp.meet.3029S
  Historically, gravitational wave antennas have been characterized by
  their detection capability. This is measured in terms of signal-to-noise
  ratio, and implies a rate of false positives and false negatives. But
  to do useful astrophysics, one would like to measure - or more
  properly, estimate - astrophysical parameters of the gravitational wave
  sources. In the interest of strengthening the connection between science
  objectives and a specific instrument performance, the LISA community
  has reformulated the LISA science requirements around the anticipated
  uncertainty in astrophysical parameter estimation. The rationale for
  this characterization of LISA and a summary of the astrophysics and
  fundamental physics that LISA can do will be given. LISA will be able
  to make precision measurements of sources out to z∼10.

Title: The LISA Pathfinder Mission
Authors: Stebbins, Robin T.; LISA Pathfinder Science Team
Bibcode: 2007AAS...21114009S
Altcode: 2007BAAS...39..990S
  LISA Pathfinder is an ESA mission designed to pave the way for the
  joint ESA/NASA Laser Interferometer Space Antenna (LISA) mission by
  testing in flight the critical technologies required for space-borne
  gravitational wave detection. It will put two test masses in a
  near-perfect gravitational free-fall and measure their motion with
  unprecedented accuracy. <P />LISA Pathfinder will carry two technology
  payloads, the European provided LISA Technology Package (LTP), and
  the NASA provided Disturbance Reduction System (DRS), also known as
  the ST-7 mission of the New Millennium Program. The LTP comprises
  two inertial sensors, high precision laser metrology, drag-free
  control and an ultra-precise micro-Newton propulsion system. The DRS
  consists of a drag-free control system and a micro-Newton propulsion
  system. The DRS will use the LTP inertial sensors, each of which has a
  proof mass, reference housing with electrodes for capacitive sensing
  and actuation and discharging systems. <P />LISA Pathfinder is due
  to be launched in the first half of 2010, with first results on the
  performance of the system being available approx 6 months later. <P
  />This poster summarizes the mission concept and reports the progress
  in the last year, and the current status as the mission nears final
  integration. Many spacecraft subsystems have been delivered. Detailed
  planning for the orbital test sequences and development of the data
  reduction software has advanced significantly. Ground support equipment
  and test procedures for the spacecraft and payloads is also well
  along. Details of the LISA technology to be flight tested will be given.

Title: The LISA Pathfinder Mission
Authors: Stebbins, Robin T.; LISA Pathfinder Science Team
Bibcode: 2006AAS...209.7403S
Altcode: 2006BAAS...38..990S
  LISA Pathfinder (formerly known as SMART-2) is an ESA mission designed
  to pave the way for the joint ESA/NASA Laser Interferometer Space
  Antenna (LISA) mission by testing in flight the critical technologies
  required for space-borne gravitational wave detection: it will put two
  test masses in a near-perfect gravitational free-fall and control and
  measure their motion with unprecedented accuracy. <P />LISA Pathfinder
  will carry two technology payloads, the European provided LISA
  Technology Package (LTP), and the NASA provided Disturbance Reduction
  System (DRS). The LTP comprises two inertial sensors, high precision
  laser metrology, drag-free control and an ultra-precise micro-Newton
  propulsion system. The DRS consists of a drag-free control system and
  a micro-Newton propulsion system. The DRS will use the LTP inertial
  sensors. <P />LISA Pathfinder is due to be launched in late 2009,
  with first results on the performance of the system being available
  approx 6 months later. <P />This poster gives an introduction to, and
  status of, the mission, followed by more details on the technologies
  to be tested in a space environment. It will also highlight the ways
  in which the LISA Pathfinder mission will be used for the preparation
  of LISA, e.g. ground segment development, on-orbit commissioning of
  the hardware, etc. as well as technology development.

Title: LISA Mission Architecture
Authors: Jedrich, Nicholas M.; Stebbins, R. T.; Livas, J. C.;
   Merkowitz, S. M.; Mink, R. G.
Bibcode: 2006AAS...209.7402J
Altcode: 2006BAAS...38..990J
  The Laser Interferometer Space Antenna (LISA) mission is unique
  from a mission design perspective in that three spacecraft and their
  associated operations form one distributed science instrument, unlike
  more conventional missions where an instrument(s) is a component of
  an individual spacecraft. The interferometer measurements between
  spacecraft that form the basis for the science measurements,
  i.e. strain, relies on all three of the spacecraft interacting as
  designed. The performance of one spacecraft in the LISA constellation
  is directly coupled to the performance of the two remaining spacecraft
  in order for the instrument to collect meaningful science data. This
  dependency on all three spacecraft to function as the instrument is the
  primary driver for unique design requirements that span all spacecraft
  subsystems and the overall mission design. A detailed discussion
  will be presented that describes the spacecraft and current mission
  architecture needed to meet the LISA science requirements.

Title: System Validation and Verification Testing for the Laser
    Interferometry Space Antenna (LISA)
Authors: Livas, Jeffrey C.; Jedrich, N.; Merkowitz, S. M.; Stebbins,
   R. T.
Bibcode: 2006AAS...209.7404L
Altcode: 2006BAAS...38..990L
  The Laser Interferometry Space Antenna (LISA) mission is a set of 3
  spacecraft that fly in a heliocentric orbit in an equilateral triangle
  formation to detect gravitational waves. Each side of the triangle
  is 5 million km long, and the formation detects passing waves by
  closely monitoring the distance between spacecraft. <P />The ideal for
  system-level testing of instruments and spacecraft is to “test as you
  fly”. Given that the inter-spacecraft distance is approximately 13
  times the distance between the earth and the moon, Ground testing for
  the LISA instrument will not be able to meet this ideal in a number
  of areas, so a combination of testing, simulation, and analysis will
  be needed instead. This paper will outline some of the areas where
  direct testing on the ground will not be possible, and discuss some
  of ideas, concepts and methods to meet that challenge. <P />The focus
  of the discussion will be on the optical and system-level aspects of
  the testing, as many of the issues associated with the proof masses
  and drag-free spacecraft are covered by the LISA Pathfinder mission.

Title: LISA Mission Tutorial
Authors: Stebbins, Robin
Bibcode: 2006AIPC..873....3S
Altcode:
  The Laser Interferometer Space Antenna (LISA) relies on concepts and
  instrumentation techniques to observe gravitational waves that are
  not widely known in astrophysics or engineering for spaceflight. This
  tutorial explains the basic scientific concepts, the mission concept,
  the top-level architecture of the flight system and the character of
  the resulting data for interested astrophysicists and engineers.

Title: Demonstration of the zero-crossing phasemeter with a LISA
    test-bed interferometer
Authors: Pollack, S. E.; Stebbins, R. T.
Bibcode: 2006CQGra..23.4189P
Altcode: 2006gr.qc.....5154P
  The laser interferometer space antenna (LISA) is being designed to
  detect and study in detail gravitational waves from sources throughout
  the Universe such as massive black hole binaries. The conceptual
  formulation of the LISA space-borne gravitational wave detector
  is now well developed. The interferometric measurements between
  the sciencecraft remain one of the most important technological and
  scientific design areas for the mission. Our work has concentrated on
  developing the interferometric technologies to create a LISA-like
  optical signal and to measure the phase of that signal using
  commercially available instruments. One of the most important goals
  of this research is to demonstrate the LISA phase timing and phase
  reconstruction for a LISA-like fringe signal, in the case of a high
  fringe rate and a low signal level. We present current results of a
  test-bed interferometer designed to produce an optical LISA-like fringe
  signal previously discussed in Jennrich O, Stebbins R T, Bender P L and
  Pollack S (<A>2001 Class. Quantum Grav. 18 4159 64</A>) and Pollack
  S E, Jennrich O, Stebbins R T and Bender P (<A>2003 Class. Quantum
  Grav. 20 S291 00</A>).

Title: A demonstration of LISA laser communication
Authors: Pollack, S. E.; Stebbins, R. T.
Bibcode: 2006CQGra..23.4201P
Altcode: 2006gr.qc.....5155P
  Over the past few years, questions have been raised concerning the
  use of laser communications links between sciencecraft to transmit
  phase information crucial to the reduction of laser frequency noise
  in the LISA science measurement. The concern is that applying medium
  frequency phase modulations to the laser carrier could compromise
  the phase stability of the LISA fringe signal. We have modified the
  table-top interferometer presented in Pollack and Stebbins (2006
  Demonstration of the zero-crossing phasemeter with a LISA test-bed
  interferometer Class. Quantum Grav.) by applying phase modulations to
  the laser beams in order to evaluate the effects of such modulations
  on the LISA science fringe signal. We have demonstrated that the phase
  resolution of the science signal is not degraded by the presence of
  medium frequency phase modulations.

Title: Low-frequency active vibration isolation for advanced LIGO
Authors: Hua, Wensheng; Adhikari, R.; DeBra, Daniel B.; Giaime, Joseph
   A.; Hammond, Giles D.; Hardham, C.; Hennessy, Mike; How, Jonathan P.;
   Lantz, Brian T.; Macinnis, M.; Mittleman, R.; Richman, S.; Robertson,
   Norna A.; Rollins, J.; Shoemaker, David H.; Stebbins, Robin T.
Bibcode: 2004SPIE.5500..194H
Altcode:
  LIGO is dedicated to the detection of gravitational waves. To achieve
  the design sensitivity of the proposed Advanced LIGO detectors, the
  seismic isolation system is required to isolate the interferometer
  mirrors from ground motion above 0.1 Hz. The dominant source of
  motion above 0.1 Hz is the microseismic peaks near 0.15 Hz. The system
  needs to isolate the payload from this motion by at least a factor of
  five in all three translational degrees of freedom. Tilt-horizontal
  coupling is the most challenging problem for seismic isolation below 1
  Hz. Tilt-horizontal coupling results from the principle of equivalence:
  inertial horizontal sensors cannot distinguish horizontal acceleration
  from tilt motion. Tilt-horizontal coupling rises dramatically at low
  frequencies, which makes low frequency isolation difficult. Several
  techniques are used to address the tilt-horizontal coupling problem. The
  isolation platform is designed to separate horizontal motions from tilt
  motions. Feedback control to displacement sensors is used to command
  the platform in all degrees of freedom. These sensors are "corrected"
  by ground seismometers, using an optimal FIR filtering technique to
  separate tilt noise from horizontal acceleration. With these techniques,
  we obtained isolation factors of 10 to 20 simultaneously in all three
  degrees of freedom at 0.15 Hz.

Title: The Laser Interferometer Space Antenna: An Overview
Authors: Stebbins, Robin
Bibcode: 2004APS..APR.L9001S
Altcode:
  The Laser Interferometer Space Antenna (LISA) is a joint ESA-NASA
  mission that will explore the Universe for gravitational wave sources
  between 0.1 mHz and 1 Hz. Anticipated sources of gravitational waves
  include: the inspiral of supermassive black holes resulting from
  galactic mergers; the inspiral of intermediate mass black holes; the
  inspiral of compact objects into supermassive black holes; thousands
  of close, compact binaries in our own Galaxy; and, possibly, density
  fluctuations in the early universe if their (much more uncertain)
  amplitude permits. LISA consists of three spacecraft orbiting the
  Sun in a triangular formation. Gravitational waves are detected by
  interferometrically monitoring the 5 million kilometer separations
  between free-falling reference masses within the spacecraft. LISA
  employs technology from Â"drag-freeÂ" control systems, spaceborne
  accelerometers, microthrusters, interferometric distance-ranging and
  precision measurements to measure strains of 10<SUP>-23</SUP> over
  very long baselines.

Title: Current error estimates for LISA spurious accelerations
Authors: Stebbins, R. T.; Bender, P. L.; Hanson, J.; Hoyle, C. D.;
   Schumaker, B. L.; Vitale, S.
Bibcode: 2004CQGra..21S.653S
Altcode:
  The performance of the LISA gravitational wave detector depends
  critically on limiting spurious accelerations of the fiducial
  masses. Consequently, the requirements on allowable acceleration levels
  must be carefully allocated based on estimates of the achievable
  limits on spurious accelerations from all disturbances. Changes in
  the allocation of requirements are being considered, and are proposed
  here. The total spurious acceleration error requirement would remain
  unchanged, but a few new error sources would be added, and the
  allocations for some specific error sources would be changed. In
  support of the recommended revisions in the requirements budget,
  estimates of plausible acceleration levels for 17 of the main error
  sources are discussed. In most cases, the formula for calculating
  the size of the effect is known, but there may be questions about
  the values of various parameters to use in the estimates. Different
  possible parameter values have been discussed, and a representative set
  is presented. Improvements in our knowledge of the various experimental
  parameters will come from planned experimental and modelling studies,
  supported by further theoretical work.

Title: LISA data reduction
Authors: Stebbins, R. T.; Bender, P. L.; Folkner, W. M.
Bibcode: 2003AdSpR..32.1259S
Altcode:
  The passage of gravitational waves changes the arm lengths between
  corners of the LISA spacecraft formation. These changes are detected
  interferometrically and recorded as phase measurements. The time
  series are reduced to reveal several signal types. First, the strong
  periodic signals from all types of galactic binaries and any strong
  chirped signals are identified by template fitting, and removed. Then
  weak, periodic signals and poorly characterized signals (e.g., generic
  bursts) are searched for. Next, weak signals with complex waveforms,
  such as from compact objects orbiting massive black holes, are sought
  with templates. Genetic algorithms, template structure or hierarchical
  searches are used to efficiently search the very large parameter
  space. Finally, backgrounds from galactic binaries, extragalactic
  binaries and the Big Bang will/may be separable by their signatures.

Title: Status of LISA phase measurement work in the US
Authors: Pollack, S. E.; Jennrich, O.; Stebbins, R. T.; Bender, P.
Bibcode: 2003CQGra..20S.193P
Altcode:
  Currently there are two implementations for LISA phase measurement being
  investigated in the United States. In this paper, we present the current
  status of one of these implementations, the so-called zero-crossing
  approach or stopwatch method. This method uses a technique of counting
  and timing to make phase measurements. Herein we present a description
  of the status of an experiment which produces an optical LISA-like
  fringe which we use to test our phase meter.

Title: Information about Intermediate Mass Black Hole Growth from
    Gravitational Waves
Authors: Bender, P. L.; Stebbins, R. T.
Bibcode: 2002AAS...201.5707B
Altcode: 2002BAAS...34R1207B
  It is likely that coalescences of roughly 10 M/sun and probably 100
  M/sun black holes (BHs) with intermediate mass black holes (IMBHs)
  occurred during the growth of the IMBHs in galactic nuclei and/or
  globular clusters. Thus it is interesting to review the types of
  associated gravitational wave (GW) signals that may be observable by
  the Laser Interferometer Space Antenna (LISA), a planned joint ESA/NASA
  mission, or by a later follow-on mission. For example, simulations
  by Abel, Bryan and Norman indicate high masses for the first stars,
  and a substantial fraction may form roughly 100 M/sun BHs. Madau and
  Rees have suggested that, if this occurs, perhaps a few tens of them
  can get to the nucleus in a Hubble time for Milky Way type galaxies. If
  some arrive while IMBHs are growing there and don't plunge in rapidly,
  they could give detectable GW signals. LISA could observe such signals
  for 100 M/sun BHs coalescing with non-rotating 10,000 M/sun or larger
  IMBHs even at z = 5, in agreement with the conclusions of Madau and
  Rees. In the future, if a high-frequency LISA follow-on mission is
  chosen, it might have 1 m diam. telescopes (instead of 0.3 m diam.),
  10 W lasers, and 500,000 km arm lengths. With our present estimate of
  the GW background due to extragalactic white dwarf binaries, such a
  mission could observe 10 M/sun BHs coalescing with nonrotating IMBHs
  at z = 5 for IMBH masses between about 1,500 and 20,000 M/sun. Similar
  events could be observed out to z = 10 for Kerr IMBHs.

Title: Seismic isolation for Advanced LIGO
Authors: Abbott, R.; Adhikari, R.; Allen, G.; Cowley, S.; Daw, E.;
   DeBra, D.; Giaime, J.; Hammond, G.; Hammond, M.; Hardham, C.; How,
   J.; Hua, W.; Johnson, W.; Lantz, B.; Mason, K.; Mittleman, R.; Nichol,
   J.; Richman, S.; Rollins, J.; Shoemaker, D.; Stapfer, G.; Stebbins, R.
Bibcode: 2002CQGra..19.1591A
Altcode:
  The baseline design concept for a seismic isolation component of the
  proposed 'Advanced LIGO' detector upgrade has been developed with
  proof-of-principle experiments and computer models. It consists of
  a two-stage in-vacuum active isolation platform that is supported by
  an external hydraulic actuation stage. Construction is underway for
  prototype testing of a full-scale preliminary design.

Title: Demonstration of the LISA phase measurement principle
Authors: Jennrich, O.; Stebbins, R. T.; Bender, P. L.; Pollack, S.
Bibcode: 2001CQGra..18.4159J
Altcode:
  We present an experiment designed to test a type of phase measurement
  system that could be used for LISA. The set-up consists of two parts:
  one is an optical signal generator to provide an optical signal
  similar to that expected for the interferometry in LISA. The other is
  a phase-meter which uses a technique of counting and timing to measure
  the phase of the signal as a function of time.

Title: Interferometric Techniques for Gravitational Wave Detection
    in Space
Authors: Stebbins, Robin T; Bender, Peter L.
Bibcode: 2000STIN...0009820S
Altcode:
  The Laser Interferometer Space Antenna (LISA) mission will detect
  gravitational waves from galactic and extragalactic sources, most
  importantly those involving supermassive black holes. The primary
  goal of this project is to investigate stability and robustness issues
  associated with LISA interferometry. We specifically propose to study
  systematic errors arising from: optical misalignments, optical surface
  errors, thermal effects and pointing tolerances. This report covers
  the first fiscal year of the grant, from January 1st to December
  31st 1999. We have employed an optical modeling tool to evaluate the
  effect of misplaced and misaligned optical components. Preliminary
  results seem to indicate that positional tolerances of one micron
  and angular tolerances of 0.6 millirad produce no significant effect
  on the achievable contrast of the interference pattern. This report
  also outlines research plans for the second fiscal year of the grant,
  from January 1st to December 31st 2000. Since the work under NAG5-6880
  has gone more rapidly than projected, our test bed interferometer is
  operational, and can be used for measurements of effects that cause
  beam motion. Hence, we will design, build and characterize a sensor
  for measuring beam motion, and then install it. We are also planning
  a differential wavefront sensor based on a quadrant photodiode as a
  first generation sensor.

Title: Active seismic isolation for enhanced LIGO detectors
Authors: Giaime, Joseph; Lantz, Brian; Debra, Daniel; How, Jonathan;
   Hardham, Corwin; Richman, Sam; Stebbins, Robin
Bibcode: 2000AIPC..523..300G
Altcode: 2000grwa.conf..300G
  The levels of seismic isolation needed for LIGO II will require a
  dramatic technological shift from the systems used in the initial
  LIGO detector. To take advantage of the improved thermal noise of a 30
  kg test mass made of high-Q material and suspended with fused silica
  fibers, one must attenuate the ground motion by more than 10 orders
  of magnitude at 10 Hz. Aggressive active isolation of ground motion to
  reduce the root-mean-squared ground displacement and the displacement
  noise in the gravitational wave band, coupled with multiple pendulum
  suspensions, can make this possible. We will describe the mechanical
  design for such a system, and discuss the issues of active control
  that confront this endeavor. .

Title: Separation of LISA Galactic and Extragalactic Signals
Authors: Bender, Peter L.; Hils, Dieter; Stebbins, Robin T.
Bibcode: 2000APS..APRH20013B
Altcode:
  Data obtained by the Laser Interferometer Space Antenna (LISA) is
  expected to include gravitational wave signals from several types of
  sources involving massive black holes at cosmological distances. In
  addition, there will be a very large number of signals from short period
  galactic binaries. For 1 year of observations, the average number of
  galactic binaries per frequency bin will be large enough at frequencies
  below 1 mHz so that most of their signals cannot be resolved. At higher
  frequencies, above roughly 3 mHz, most individual galactic signals
  can be solved for and removed from the data record. Studies have been
  started to investigate, for frequencies from roughly 1 to 10 mHz, how
  much information about the extragalactic black hole sources will be lost
  because of having to solve for the galactic sources. An axisymmetric
  but fairly realistic model is being used for the distribution of
  binaries in the galaxy. It probably will be desirable to subtract out
  some sources whose reality and signal parameters are only moderately
  certain, but whose frequency characteristics differ from the massive
  black hole signals of interest.

Title: What Information May Gravitational Waves Carry About Early
    Galaxies?
Authors: Bender, Peter L.; Hils, Dieter; Stebbins, Robin T.
Bibcode: 1999ASPC..182..539B
Altcode: 1999gady.conf..539B
  No abstract at ADS

Title: Progress on Low-Frequency Active Vibration Isolation
Authors: Richman, S. J.; Giaime, J. A.; Stebbins, R. T.; Bender,
   P. L.; Faller, J. E.
Bibcode: 1999magr.meet.1066R
Altcode:
  No abstract at ADS

Title: LISA operations and sensitivity
Authors: Stebbins, R. T.; LISA Team
Bibcode: 1998AIPC..456...17S
Altcode: 1998lain.conf...17S
  The three LISA spacecraft must monitor changes in their relative
  separation to about 10 pm. The various operating modes during the
  mission lifetime will be summarized, and the science mode will be
  described in detail. The science operations involve the optical system,
  the attitude and position control system, the on-board processing for
  signal extraction, telemetry and ground operations. The instrumental
  origins of the anticipated LISA sensitivity curve will also be
  described.

Title: Experimental demonstration of some aspects of LISA
    interferometry
Authors: Giaime, J. A.; Stebbins, R. T.; Bender, P. L.; Faller, J. E.;
   Hall, J. L.
Bibcode: 1998AIPC..456..169G
Altcode: 1998lain.conf..169G
  Plans are described to experimentally demonstrate at JILA a possible
  phase measurement technique for use in LISA interferometry. This
  demonstration will include use of a compact system for fringe generation
  and photodetection with realistic beam powers in a Mach-Zehnder
  interferometer, and development of a stable digital fringe phase
  measurement system.

Title: Possible use of a narrow-field star tracker on the New
    Millennium SSI mission
Authors: Bender, Peter L.; Stebbins, Robin T.; Folkner, William M.
Bibcode: 1998SPIE.3350..626B
Altcode:
  A separated spacecraft interferometer (SSI) demonstration mission
  with three spacecraft has been proposed for flight under the NASA New
  Millennium Technology Development Program. Both the rotation rate
  of the interferometer about the normal to the plane containing the
  three spacecraft and the orientation in the plane must be determined
  accurately in order to permit the detection of white light fringes
  from sources that have visual magnitudes as high as possible. It
  presently is planned to use signals from tracking the science object
  plus other auxiliary information to determine the interferometer
  rotation rate d(theta) /dt and the angular position (theta) . We have
  investigated a possible supplementary approach that makes use of a
  combined beacon tracker and narrow-field star tracker on one of the
  two collector spacecraft. A very small beacon mounted on the other
  collector spacecraft can be viewed with respect to a reference star
  nearly 180 degrees away to determine d(theta) /dt and (theta) for the
  interferometer. Beacon/star tracker observations over roughly an hour
  appear sufficient to determine the sweep rate for starlight fringes
  in the interferometer to adequate accuracy and to detect the fringes.

Title: Gravitational Wave Frequency Range for the LISA Mission
Authors: Folkner, W. M.; Bender, P. L.; Stebbins, R. T.
Bibcode: 1998AAS...192.1708F
Altcode: 1998BAAS...30..843F
  Studies of the Laser Interferometer Space Antenna mission are being
  pursued actively both in Europe and in the US. The present mission
  design calls for three spacecraft to be launched on a single Delta II
  launch vehicle and placed in an equilateral triangle configuration about
  20 degrees behind the Earth in orbit around the Sun. Laser heterodyne
  measurements made over the 5 million km sides of the triangle permit
  the detection and detailed study of gravitational wave signals. The
  frequency range discussed for LISA usually has been limited to 0.0001
  to 1 Hz because of reliance on passive thermal isolation to keep
  noise due to temperature fluctuations in the most sensitive part of
  the payload small. However, the possibility of actively controlling
  the temperature of the thermal shield around the payload is now being
  investigated. The expected improvement in the LISA sensitivity below
  0.0001 Hz will be discussed. This would extend the useful sensitivity
  to include possible sources with larger masses, such as the coalescence
  of massive black holes after galaxy mergers.

Title: On the Origin of Solar Oscillations
Authors: Goode, Philip R.; Strous, Louis H.; Rimmele, Thomas R.;
   Stebbins, Robin T.
Bibcode: 1998ApJ...495L..27G
Altcode: 1998astro.ph..1008G
  We have made high-resolution observations of the Sun in which we
  identify individual sunquakes and see power from these seismic events
  being pumped into the resonant modes of vibration of the Sun. A typical
  event lasts about 5 minutes. We report the physical properties of
  the events and relate them to theories of the excitation of solar
  oscillations. We also discuss the local seismic potential of these
  events.

Title: LISA Mission Concept Study, Laser Interferometer Space Antenna
    for the Detection and Observation of Gravitational Waves
Authors: Folkner, W. M.; Bender, P. L.; Stebbins, R. T.
Bibcode: 1998STIN...0055623F
Altcode:
  This document presents the results of a design feasibility study for
  LISA (Laser Interferometer Space Antenna). The goal of LISA is to
  detect and study low-frequency astrophysical gravitational radiation
  from strongly relativistic regions. Astrophysical sources potentially
  visible to LISA include extra-galactic massive black hole binaries
  at cosmological distances, binary systems composed of a compact star
  and a massive black hole, galactic neutron star-black hole binaries,
  and background radiation from the Big Bang. The LISA mission will
  comprise three spacecraft located five million kilometers apart forming
  an equilateral triangle in an Earth-trailing orbit. Fluctuations in
  separation between shielded test masses located within each spacecraft
  will be determined by optical interferometry which determines the
  phase shift of laser light transmitted between the test masses.

Title: Getting astrophysical information from LISA data
Authors: Stebbins, R. T.; Bender, P. L.; Folkner, W. M.
Bibcode: 1997CQGra..14.1499S
Altcode:
  No abstract at ADS

Title: LISA data acquisition
Authors: Stebbins, R. T.; Bender, P. L.; Folkner, W. M.; LISA
   Science Team
Bibcode: 1996CQGra..13A.285S
Altcode:
  The method for measuring changes in the lengths of the three arms
  for the LISA gravitational-wave detector is described. Accurate phase
  measurements are required on signals with Doppler shifts of about 1
  MHz for the two main arms of the interferometer, and up to 15 MHz for
  the third arm. This is accomplished by shifting the signal frequencies
  down to near 100 kHz, filtering and then timing zero crossings of the
  signals. The basic methods for correcting for the laser phase noise
  and for phase noise in the ultra-stable oscillators used to derive
  various radio frequencies are described briefly. The corrections are
  made on the spacecraft, before the data are telemetred to the ground.

Title: Sensitivity of the LISA Gravitational Wave Mission
Authors: Ward, H.; Bender, P.; Faller, J. E.; Stebbins, R. T.
Bibcode: 1996APS..MAY..E901W
Altcode:
  The sensitivity achievable by the Laser Interferometer Space Antenna
  (LISA) will be discussed (see also abstracts by Stebbins et al and by
  Bender and Hils). Below about 1 mHz, the sensitivity will be limited
  mainly by spurious accelerations of the proof mass in each spacecraft
  and by a random superposition of signals from many short period galactic
  binaries. At higher frequencies, the main limitations will come from
  shot noise in determining the difference in length of the interferometer
  arms and from fluctuations in the pointing of the laser beams. Hundreds
  to thousands of galactic binaries resolved in frequency and direction
  will be detectable throughout the galaxy. A few known sources will be
  included. One possible type of source is black hole-massive black hole
  (BH-MBH) binaries, with periapsis speeds of about half the speed of
  light, very rapidly precessing elliptical orbits, and possible fast
  orbit plane precession around Kerr MBHs. The observation of such signals
  or of those from MBH-MBH binaries would permit extremely strong tests
  of the dynamical predictions of general relativity.

Title: The LISA Gravitational Wave Mission
Authors: Stebbins, R. T.; Bender, P. L.; Faller, J. E.; Folkner,
   W. M.; Ward, H.
Bibcode: 1996APS..MAY.J1506S
Altcode:
  The Laser Interferometer Space Antenna (LISA) is a mission designed for
  detailed studies of gravitational waves with frequencies of roughly 0.1
  mHz to 1 Hz. Gravitational waves will be detected by interferometrically
  monitoring the relative distances between proof masses in different
  spacecraft, separated by 5× 10^6 km. LISA will detect strains as low
  as 10<SUP>-23</SUP> with a 1 yr observation time and a S/N ratio of
  5. The sensitivity will be sufficient to detect many gravitational
  wave sources which cannot be readily observed by any other means. The
  3-arm interferometer consists of 6 spacecraft orbiting the Sun, with
  two at each vertex of an equilateral triangle. Proof mass disturbances
  are kept small by a drag-free system and the benign environment of
  solar orbit. LISA was selected in 1994 as a Cornerstone mission in
  the proposed ESA Horizon 2000 Plus program. Technology development
  studies for LISA are being started by ESA. Investigations of possible
  US contributions to LISA currently are in progress under a NASA program
  for studies of new mission concepts in astrophysics.

Title: The Sun's Acoustic Spectrum and Normal Mode Parameters
Authors: Stebbins, R. T.; Hill, F.; Stark, P. B.; GONG Data Reduction
   Team; GONG Analysis Team
Bibcode: 1996AAS...188.5306S
Altcode: 1996BAAS...28..904S
  GONG seeks to measure the frequencies, amplitudes and line widths of
  the Sun's acoustic normal modes. The Project estimates these parameters
  for more than 250,000 acoustic modes of the Sun from every 36 day-long
  set of data. Data from the network are archived, calibrated, reduced
  to several science products and made available for distribution to
  researchers at the pace of observations. GONG also produces magnetograms
  and temporally filtered solar images for convective velocity and
  magnetic field studies. The frequency resolution of a single data set
  is 0.321 mu Hz. For m- averaged frequencies the median formal error
  is 0.044 mu Hz, and the associated median fractional frequency error
  is 1.6 x 10(-5) . Results from concatenated data sets are now becoming
  available. For a three-year data set, the fractional error is expected
  to be 3 x 10(-6) , providing the highest quality helioseismic frequency
  measurements to date. Examples of power spectra and mode parameters
  will be shown. To demonstrate the reliability of the initial GONG
  frequencies, m-averaged frequency measurements will be compared with
  other helioseismic data sets. The mean systematic variations among
  the data sets are 0.03 to 0.08 mu Hz. The differences arise from a
  combination of systematic errors, random errors, and possible changes
  in solar structure and dynamics. Error sources will be discussed.

Title: The Solar Acoustic Spectrum and Eigenmode Parameters
Authors: Hill, F.; Stark, P. B.; Stebbins, R. T.; Anderson, E. R.;
   Antia, H. M.; Brown, T. M.; Duvall, T. L., Jr.; Haber, D. A.;
   Harvey, J. W.; Hathaway, D. H.; Howe, R.; Hubbard, R. P.; Jones,
   H. P.; Kennedy, J. R.; Korzennik, S. G.; Kosovichev, A. G.; Leibacher,
   J. W.; Libbrecht, K. G.; Pintar, J. A.; Rhodes, E. J., Jr.; Schou, J.;
   Thompson, M. J.; Tomczyk, S.; Toner, C. G.; Toussaint, R.; Williams,
   W. E.
Bibcode: 1996Sci...272.1292H
Altcode:
  The Global Oscillation Network Group (GONG) project estimates
  the frequencies, amplitudes, and linewidths of more than 250,000
  acoustic resonances of the sun from data sets lasting 36 days. The
  frequency resolution of a single data set is 0.321 microhertz. For
  frequencies averaged over the azimuthal order m, the median formal
  error is 0.044 microhertz, and the associated median fractional error
  is 1.6 x 10<SUP>-5</SUP>. For a 3-year data set, the fractional error
  is expected to be 3 x 10<SUP>-6</SUP>. The GONG m-averaged frequency
  measurements differ from other helioseismic data sets by 0.03 to 0.08
  microhertz. The differences arise from a combination of systematic
  errors, random errors, and possible changes in solar structure.

Title: Multiresolution-element imaging of extrasolar Earthlike planets
Authors: Bender, Peter L.; Stebbins, Robin T.
Bibcode: 1996JGR...101.9309B
Altcode:
  It has been suggested recently that imaging of extrasolar Earthlike
  planets should be considered as a possible future goal of the NASA
  space program. As an aid to discussing what would be required in order
  to undertake imaging, a partial design is described for a separated
  spacecraft interferometer which could achieve images in the visible
  with 10 resolution elements across the planet. Between 15 and 25 large
  collector telescopes or clusters of telescopes spread out over roughly
  a 200-km baseline in solar orbit at 1 AU from the Sun or possibly in
  high Earth orbit are required. A very preliminary approach to the use of
  multispectral remote sensing techniques is discussed also. Finally, the
  generalization of this approach to larger numbers of resolution elements
  across the planet is considered. Clearly, imaging is possible only
  if the truly staggering problem of avoiding the 10<SUP>10</SUP> times
  stronger scattered light from the nearby star can be overcome. However,
  even if this can be done, the amount and precision of the required
  hardware for even poor-quality images appears to present an obstacle
  to such a program which would be extremely difficult to overcome.

Title: Active/Passive Vibration Isolation at 1 HZ and Above Part II:
    Main Stages
Authors: Richman, S. J.; Newell, D. B.; Stebbins, R. T.; Bender,
   P. L.; Faller, J. E.
Bibcode: 1996magr.meet.1426R
Altcode:
  No abstract at ADS

Title: Thermal Stability Analysis for a Heliocentric Gravitational
    Radiation Detection Mission
Authors: Folkner, W. M.; McElroy, P.; Miyake, R.; Bender, P. L.;
   Stebbins, R. T.; Supper, W.
Bibcode: 1996magr.meet.1655F
Altcode:
  No abstract at ADS

Title: Active/Passive Vibration Isolation at 1Hz and Above Part I:
    Single Stage, Six Degrees of Freedom
Authors: Newell, D. B.; Richman, S. J.; Stebbins, R. T.; Nelson,
   P. G.; Mason, J. E.; Bender, P. L.; Faller, J. E.
Bibcode: 1996magr.meet.1421N
Altcode:
  No abstract at ADS

Title: The LISA Gravitational Wave Mission
Authors: Stebbins, R. T.; Bender, P. L.; Faller, J. E.; Hils, D.;
   Folkner, W. M.
Bibcode: 1995AAS...187.7105S
Altcode: 1995BAAS...27R1384S
  The Laser Interferometer Space Antenna (LISA) is a mission designed
  for detailed studies of gravitational waves with frequencies of roughly
  0.0001 to 1 Hz. It is a Cornerstone mission in the proposed ESA Horizon
  2000 Plus program. Investigations of possible US contributions to LISA
  currently are in progress under the NASA program for studies of new
  mission concepts in astrophysics. LISA is a formation of 6 spacecraft
  in the shape of an equilateral triangle 5 million km on a side, with
  2 spacecraft at each vertex. The formation is in orbit around the
  Sun, following about 20(deg) behind the Earth. Orbital parameters
  are chosen so that the distances between the spacecraft stay nearly
  constant for years. Each spacecraft is made drag-free by keeping
  it centered on a carefully shielded test mass at its center. Laser
  distance measurements are made between the test masses using roughly
  0.5 W per beam and about 40 cm diameter telescopes. Laser phase noise
  can be determined by observing the apparent changes in the 5 million
  km arm lengths, since the real variations in the arm lengths at the
  frequencies of interest are very small. The desired gravitational
  wave signals are obtained from the corrected differences in the arm
  lengths. For 1 yr of observations and a S/N of 5, the LISA sensitivity
  reaches its maximum of 10(-23) at frequencies of 0.001 to 0.03 Hz. This
  sensitivity is sufficient to detect sources such as a 5 to 10M_sun
  black hole orbiting around and coalescing with a roughly 10(6M_sun)
  black hole at z=1. Scenarios in which such events would be observed
  appear to be quite plausible if 0.01% or more of the stars in the
  cusps around supermassive black holes in galactic nuclei are black
  holes. Coalescences of two supermassive black holes after galactic or
  pregalactic mergers also may be observed. For short period galactic
  binaries, hundreds to thousands of individual sources will be resolved
  and their distribution in the galaxy determined.

Title: Dark Lanes in Granulation and the Excitation of Solar
    Oscillations
Authors: Rimmele, T. R.; Goode, P. R.; Strous, L. H.; Stebbins, R. T.
Bibcode: 1995ESASP.376b.329R
Altcode: 1995help.confP.329R; 1995soho....2..329R
  No abstract at ADS

Title: 15-m laser-stabilized imaging interferometer
Authors: Stebbins, Robin T.; Bender, Peter L.; Chen, Che Jen; Page,
   Norman A.; Meier, D.; Dupree, A. K.
Bibcode: 1995SPIE.2477...31S
Altcode:
  The LAser-Stabilized Imaging Interferometer (LASII) concept is being
  developed as an astronomical telescope for the next generation of
  optical resolution beyond Hubble Space Telescope (HST). The essential
  ingredients are: a rigid and stable structure to minimize mechanical
  and thermal distortion, active control of the optical geometry by
  a laser metrology system, a self-deploying structure fitting into a
  single launch vehicle, and ultraviolet operation. We have modified
  earlier design concepts to fit the scale of an intermediate sized
  NASA mission. Our present design calls for 24 0.5 m apertures in a
  Mills Cross configuration, supported on four trusses. A fifth truss
  perpendicular to the primary surface would support the secondary mirror
  and the laser metrology control points. Either separate interferometers
  or two guide telescopes would track guide stars. This instrument would
  have about 6 times the resolution of HST in the visible and the same
  collecting area. The resolution would reach 2.5 mas at 150 nm. The
  primary trusses would fold along the secondary truss for launch, and
  automatically deploy on orbit. Possible orbits are sun-synchronous at
  900 km altitude, high earth orbit or solar orbit. Infrared capability
  could be included, if desired.

Title: Dark Lanes in Granulation and the Excitation of Solar
    Oscillations
Authors: Rimmele, Thomas R.; Goode, Philip R.; Harold, Elliotte;
   Stebbins, Robin T.
Bibcode: 1995ApJ...444L.119R
Altcode:
  We made simultaneous, high-resolution observations of the Sun's
  granulation and solar acoustic events in the photosphere. We find that
  the acoustic events, which are a local by-product of the excitation
  of solar oscillations (Goode, Gough, &amp; Kosovichev 1992), occur
  preferentially in the dark, intergranular lanes. At the site of
  a typical acoustic event the local granulation becomes darker over
  several minutes leading up to the event with a further, abrupt darkening
  immediately preceding the peak of the event. Further, the stronger
  the acoustic event the darker the granulation. Thus, the excitation of
  solar oscillations seems more closely associated with the rapid cooling
  occurring in the upper convection layer, rather than the overshooting of
  turbulent convection itself. We find no substantial role for so-called
  'exploding' granules in the excitation of solar oscillations.

Title: Photospheric Wave Behavior
Authors: Stebbins, R. T.; Rimmele, T. R.; Goode, P. R.
Bibcode: 1995ASPC...76..354S
Altcode: 1995gong.conf..354S
  No abstract at ADS

Title: The Global Oscillation Network Group Site Survey - Part One
Authors: Hill, Frank; Fischer, George; Grier, Jennifer; Leibacher,
   John W.; Jones, Harrison B.; Jones, Patricia P.; Kupke, Renate;
   Stebbins, Robin T.
Bibcode: 1994SoPh..152..321H
Altcode:
  The Global Oscillation Network Group (GONG) Project is planning to place
  a set of instruments around the world to observe solar oscillations as
  continuously as possible for at last three years. The Project has now
  chosen the sites that will comprise the network. This paper describes
  the methods of data collection and analysis that were used to make
  this decision.

Title: The Global Oscillation Network Group Site Survey - Part Two
Authors: Hill, Frank; Fischer, George; Forgach, Suzanne; Grier,
   Jennifer; Leibacher, John W.; Jones, Harrison P.; Jones, Patricia
   B.; Kupke, Renate; Stebbins, Robin T.; Clay, Donald W.; Ingram,
   Robert E. L.; Libbrecht, Kenneth G.; Zirin, Harold; Ulrichi, Roger
   K.; Websteri, Lawrence; Hieda, Lester S.; Labonte, Barry J.; Lu,
   Wayne M. T.; Sousa, Edwin M.; Garcia, Charles J.; Yasukawa, Eric
   A.; Kennewell, John A.; Cole, David G.; Zhen, Huang; Su-Min, Xiao;
   Bhatnagar, Arvind; Ambastha, Aashok; Al-Khashlan, Abdulrahman Sa'ad;
   Abdul-Samad, Muhammad-Saleh; Benkhaldoun, Zouhair; Kadiri, Samir;
   Sánchez, Francisco; Pallé, Pere L.; Duhalde, Oscar; Solis, Hernan;
   Saá, Oscar; González, Ricardo
Bibcode: 1994SoPh..152..351H
Altcode:
  The Global Oscillation Network Group (GONG) Project will place a
  network of instruments around the world to observe solar oscillations as
  continuously as possible for three years. The Project has now chosen the
  six network sites based on analysis of survey data from fifteen sites
  around the world. The chosen sites are: Big Bear Solar Observatory,
  California; Mauna Loa Solar Observatory, Hawaii; Learmonth Solar
  Observatory, Australia; Udaipur Solar Observatory, India; Observatorio
  del Teide, Tenerife; and Cerro Tololo Interamerican Observatory, Chile.

Title: Observation of Impulsive Acoustic Events and the Excitation
    of Solar Oscillations
Authors: Restaino, Sergio R.; Stebbins, Robin T.; Goode, Philip R.
Bibcode: 1993ApJ...408L..57R
Altcode:
  The 5 minute solar oscillation has been exploited in numerous seismic
  studies in which internal properties of the sun have been inferred. It
  is generally regarded that these modes are excited by turbulent
  convection in the sun's outermost layers. We observe the oscillatory
  wakes caused by impulsive events, related to those described in 1909
  by Lamb. These correspond to the events modeled by Goode et al. (1992)
  which they associate with excitation of the global 5-min oscillations.

Title: Observation of impulsive acoustic events and the excitation
    of solar oscillations
Authors: Restaino, Sergio R.; Stebbins, Robin T.; Goode, Philip R.
Bibcode: 1992njit.rept.....R
Altcode:
  The five-minute solar oscillation has been exploited in numerous seismic
  studies in which internal properties of the Sun have been inferred. It
  is generally regarded that these modes are excited by turbulent
  convection in the Sun's outermost layers. The oscillatory wakes caused
  by impulsive events were observed, matching those described by Lamb
  (1909). These correspond to the events modeled by Goode, et al., which
  they associate with excitation of the global five-minute oscillations.

Title: Movies of Velocity and Acoustic Flux in the Solar Photosphere
Authors: Stebbins, R. T.; Restaino, S. R.; Goode, P. R.
Bibcode: 1992AAS...180.0605S
Altcode: 1992BAAS...24..737S
  CCD images of FeI 5434 Angstroms line profiles have previously
  been collected and analyzed for the average characteristics of wave
  propagation in the photosphere. The previous analysis determined the
  velocity at nine depths in the spectral line and 100 horizontal spatial
  points spanning 70 arc sec. Time series of these velocity frames,
  lasting 37 minutes, have been Fourier transformed and filtered to
  pass the five minute modes of the Sun. Through the Hilbert transform
  and the analytic signal, the instantaneous velocity amplitude and
  phase were computed at every point in the three dimensional space
  of altitude, horizontal slit position and time. These data have been
  further processed to create color-contour maps of vertical acoustic
  propagation at each time sample. Velocity amplitude, velocity phase,
  kinetic energy density and acoustic flux are all mapped. Time series of
  these maps have been assembled into a movie which shows the evolution of
  vertical acoustic propagation. This movie is a complete visualization
  of sound waves in the photosphere, based on observation. The amplitude
  and kinetic energy density behaves as one might expect in the presence
  of the solar p-modes. However, the phase and acoustic flux have
  characteristic spatial and temporal scales which are very different
  from the amplitude. For example, upward and downward flux may occur
  in the same amplitude structure at different times, or at the same
  time. These results are consistent with the localized model of p-mode
  excitation advanced by Goode, Gough and Kosovichev.

Title: Gravitational radiation observations on the moon
Authors: Stebbins, R. T.; Armstrong, J. W.; Bender, P. L.; Drever,
   R. W. P.; Hellings, R. W.; Saulson, P. R.
Bibcode: 1990AIPC..207..637S
Altcode: 1990am...proc..637S
  A Laser-Interferometer Gravitational-Wave Observatory (LIGO) is
  planned for operation in the United States, with two antennas
  separated by several thousand kilometers. Each antenna would
  incorporate laser interferometers with 4 km arm lengths, operating
  in vacuum. The frequency range covered initially would be from a few
  tens of Hz to a few kHz, with possible extension to lower frequencies
  later. Similar systems are likely to be constructed in Europe, and
  there is a possibility of at least one system in Asia or Australia. It
  will be possible to determine the direction to a gravitational wave
  source by measuring the difference in the arrival times at the various
  antennas for burst signals or the phase difference for short duration
  nearly periodic signals. The addition of an antenna on the Moon,
  operating in support of the Earth-based antennas, would improve the
  angular resolution for burst signals by about a factor 50 in the plane
  containing the source, the Moon, and the Earth. This would be of major
  importance in studies of gravitational wave sources. There is also
  a possibility of somewhat lower noise at frequencies near 1 Hz for a
  lunar gravitational wave antenna, because of lower gravity gradient
  noise and microseismic noise on the Moon. However, for frequencies
  near 0.1 Hz and below, a 107 km laser gravitational wave antenna in
  solar orbit would be much more sensitive.

Title: A lunar gravitational wave antenna using a laser interferometer
Authors: Stebbins, R. T.; Bender, P. L.
Bibcode: 1990AIPC..202..188S
Altcode: 1990palb.work..188S
  A moon-based laser interferometer for detecting gravitational radiation
  could detect signals in the band 10-1 to 104 Hz. A preliminary
  evaluation of the noise budget for an optimistic antenna design is
  reported here and compared to that for other planned gravitational wave
  interferometers. Over most of the frequency range, the sensitivity is
  controlled by the thermal noise in the test mass suspensions. From
  roughly 3 to a few hundred Hertz, it is about the same as the
  sensitivity expected in terrestrial antennas of the same construction,
  which will have been operating for at least a decade. Below 0.3 Hz,
  a proposed space-based interferometer, designed for operation down to
  10-5 Hz, would have better sensitivity. As pointed out by others, the
  most important role of a lunar antenna would be the improved angular
  resolution made possible by the long baseline to terrestrial antennas.

Title: An Algorithm for Removing Pattern Noise in Reticons
Authors: Stebbins, R. T.; Restaino, S. R.
Bibcode: 1990BAAS...22R.887S
Altcode:
  No abstract at ADS

Title: Optical interferometer in space.
Authors: Bender, Peter L.; Faller, J. E.; Hall, J. L.; Hils, D.;
   Stebbins, R. T.; Vincent, Mark A.
Bibcode: 1989NASCP3046...80B
Altcode: 1989rges.rept...80B
  The present design concepts for a Laser Gravitational-Wave Observatory
  in Space are described. Laser heterodyne distance measurements are made
  between test masses located in three spacecraft separated by roughly
  10<SUP>6</SUP>km. The science objectives are: to measure discrete
  sinusoidal gravitational wave signals from individual sources with
  periods of 1 second to 1 day; to measure the stochastic background due
  to unresolved binaries; and to search for gravitational wave pulses
  with periods longer than 1 second from possible exotic sources such
  as gravitational collapse of very massive objects.

Title: Disturbance Reduction Techniques for a Laser Gravitational
    Wave Observatory in Space
Authors: Bender, P. L.; Faller, J. E.; Hils, D.; Stebbins, R. T.
Bibcode: 1989grg..conf..566B
Altcode:
  No abstract at ADS

Title: a 1-TO-10-HZ Prototype Isolation System for Gravitational
    Wave Interferometers and Thermal Noise Measurements
Authors: Stebbins, R. T.; Bender, P. L.; Faller, J. E.; Newell, D. B.;
   Speake, C. C.
Bibcode: 1989grg..conf..585S
Altcode:
  No abstract at ADS

Title: Wave Behavior in the Solar Photosphere - a Comparison of
    Theory and Observation
Authors: Marmolino, Ciro; Stebbins, Robin T.
Bibcode: 1989SoPh..124...23M
Altcode:
  We report detailed comparisons between theoretical and empirical
  eigenfunctions of velocity and intensity for the 5-min modes in the
  photosphere. The comparison process is accomplished by obtaining
  synthetic profiles of the FeI λ5434 Å line in the presence
  of waveforms given by dynamical calculations and then applying
  a common procedure of reduction both to the observed and to the
  synthetic data. For the velocity waveforms, our results show a general
  agreement between theory and observations together with some systematic
  differences; in particular the theory systematically underestimates the
  observations in the low photosphere. These systematic differences are
  stressed by the intensity results since both the computed amplitudes
  and phases appear to be wrong in the deeper layers.

Title: An antenna for laser gravitational-wave observations in space
Authors: Faller, J. E.; Bender, P. L.; Hall, J. L.; Hils, D.; Stebbins,
   R. T.; Vincent, M. A.
Bibcode: 1989AdSpR...9i.107F
Altcode: 1989AdSpR...9..107F
  Progress during the past two years on a proposed Laser
  Gravitational-Wave Observatory in Space (LAGOS) is discussed. Calculated
  performance for a 10<SUP>6</SUP> km sized antenna over the frequency
  range of 10<SUP>-5</SUP> to 1 Hz is given. The sensitivity from
  10<SUP>-3</SUP> to 10<SUP>-1</SUP> Hz is expected to be 1 ×
  10<SUP>-21</SUP>/Hz<SUP>0.5</SUP>. Noise sources such as accelerations
  of the drag-free test masses by random molecular impacts and by
  fluctuations in the net thermal radiation pressure will limit the
  sensitivity at lower frequencies. The scientific objectives are the
  observation of CW gravitational waves from large numbers of binary
  systems and the detection of pulses which may have been emitted during
  the period of galaxy formation.

Title: The 5-minute oscillation in the solar photosphere - Theoretical
    behaviour versus observations
Authors: Marmolino, C.; Stebbins, R. T.
Bibcode: 1989MmSAI..60...71M
Altcode:
  Calculations are used to explore how theoretical waveforms for the
  five-minute solar oscillation reproduce the observed behavior of
  the solar Fe I 5434 A line. Comparison of theoretical and empirical
  velocity eigenfunctions shows some systematic differences in a framework
  of general agreement. The theory systematically underestimates the
  observations in both amplitude and phase shift in the low photosphere;
  the differences between the various theoretical treatments is much
  smaller than the difference between theory and observation. The
  intensity agreement is poor, with the theoretical treatments again
  differing much less with each other than with observation. These results
  are evidence for systematic problems with the assumptions involved in
  the calculation of the waveforms pertaining to the deeper layers of
  the photosphere.

Title: Preliminary Optical Design for a Laser Gravitational Wave
    Antenna in Space
Authors: Bender, P. L.; Faller, J. E.; Hall, J. L.; Hills, D.;
   Stebbins, R.
Bibcode: 1988soae.conf...12B
Altcode:
  No abstract at ADS

Title: Waves in the Solar Photosphere
Authors: Stebbins, Robin; Goode, Philip R.
Bibcode: 1987SoPh..110..237S
Altcode:
  Time-sequences of line profile data have been subjected to a unique
  analysis which produces an amplitude and phase of the velocity and
  intensity at several line depths for each time sample and spatial
  point on the Sun. The data have been filtered to pass only the
  frequencies and spatial wavenumbers of the 5-min band. Yet, a secondary
  oscillation emerges, the phase of which propagates downward. Empirical
  eigenfunctions for velocity and intensity are given, and the kinetic
  energy flux is computed.

Title: Proposed studies of a 30-meter imaging interferometer concept
Authors: Stebbins, R. T.; Bender, P. L.; Faller, J. E.
Bibcode: 1987ESASP.273...85S
Altcode: 1987ois..work...85S
  An imaging interferometer in space based on the use of 15 m sections of
  graphite-epoxy truss structure to form the basic mechanical support
  system is suggested. One simple design is a Y-shaped array of 3
  coplanar arms, each 15 m long and 1.5 m in diameter, together with a
  perpendicualr mast of similar length. Roughly 15 observing telescopes
  of 0.5 m diameter would be used, with laser interferometers controlling
  the optical pathlengths. The total mass of the imaging interferometer
  is 3000 kg. With this design, the entire interferometer can be carried
  to orbit with a single STS launch and then deployed. The interferometer
  could be operated either in a fully illuminated Sun-synchronous orbit
  at 1400 km altitude or loosely attached to the Space Station.

Title: A Simple Irradiance Monitor for Testing Solar Global
    Oscillation Network Sites
Authors: Fischer, G.; Hill, F.; Jones, W.; Leibacher, J.; McCurnin,
   W.; Stebbins, R.; Wagner, J.
Bibcode: 1986SoPh..103...33F
Altcode:
  We describe a simple irradiance monitor intended for use in assessing
  the suitability of candidate sites for a worldwide network of small
  solar telescopes. The network will observe the Sun as continuously
  as possible in order to provide high quality solar oscillation data
  with low diurnal sidelobe contamination and high temporal frequency
  resolution.

Title: Observation of Solar Brightness Oscillations at the South Pole
Authors: Stebbins, R. T.; Ronan, R.; Arrambide, M.
Bibcode: 1985AnJUS..20..219S
Altcode:
  No abstract at ADS

Title: A preliminary report on brightness oscillation observations
    made at South Pole during the 1982-83 Austral Summer
Authors: Stebbins, R.
Bibcode: 1984MmSAI..55..229S
Altcode:
  No abstract at ADS

Title: Observations of Solar Oscillations at the South Pole
Authors: Stebbins, R. T.; Mann, R.
Bibcode: 1984AnJUS..18..268S
Altcode:
  No abstract at ADS

Title: The measurement of long-period oscillations at Sacramento
    Peak Observatory and South Pole
Authors: Stebbins, R.; Wilson, C.
Bibcode: 1983SoPh...82...43S
Altcode: 1983IAUCo..66...43S
  A program to measure long-period brightness oscillations at the solar
  limb has been pursued at Sacramento Peak Observatory for several
  years. Past improvements in observing technique and data analysis are
  reviewed. The encouraging results aid in the verification of the reality
  and the origin of oscillatory signals. However, the main stumbling block
  to this and other observational programs is the length of observing
  sequences imposed by the day/night cycle. The South Pole has received
  considerable attention as a site where extended observations might be
  possible. Currently, the Sacramento Peak program is developing a South
  Pole telescope designed for the observing technique and data analysis
  proven in Sunspot. A review of pertinent South Pole site parameters
  is given here for other workers who may be considering South Pole
  observations. Observing sequences longer than 150 hr are possible,
  though rare. Data sets of this duration are very attractive for solar
  oscillation studies.

Title: Observation of five-minute-period gravity waves in the solar
    photosphere
Authors: Stebbins, R. T.; Goode, Philip R.; Hill, Henry A.
Bibcode: 1983SoPh...82..163S
Altcode: 1983IAUCo..66..163S
  Vertically propagating traveling waves have been observed in the
  solar photosphere. These waves have a period of 278 ± 41 seconds
  and a vertical phase velocity of about 2 km s<SUP>-1</SUP>. It is
  noted that these waves also have approximately the same period as the
  well-studied five-minute-period acoustic mode, which is evanescent in
  the photosphere. The only consistent interpretation of the traveling
  waves implies that they are gravity waves. About half the time the
  gravity waves are outgoing, while the remainder of the time they
  are ingoing.

Title: Observations of Solar Oscillations at the South Pole
Authors: Stebbins, R. T.; Mann, R.
Bibcode: 1983AnJUS..18..268S
Altcode:
  No abstract at ADS

Title: Observation of nonacoustic, 5 minute period, vertical traveling
    waves in the photosphere of the sun
Authors: Hill, H. A.; Goode, P. R.; Stebbins, R. T.
Bibcode: 1982ApJ...256L..17H
Altcode:
  Nonacoustic, radially propagating traveling waves have been observed in
  the solar photosphere. These traveling waves have a period of 278 + or -
  41 s. The vertical wavelength (approximately 500 km) and phase velocity
  (approximately 2 km/s) of the waves are among their properties deduced
  from the data. It is also observed that the waves have outgoing phase
  part of the time and ingoing phase the remainder of the time. The
  traveling waves are interpreted to be gravity waves. Their role in
  the heating of the chromosphere is discussed.

Title: Observation of Photospheric Gravity Waves
Authors: Stebbins, R. T.; Goode, P. R.; Hill, H. A.
Bibcode: 1981BAAS...13..858S
Altcode:
  No abstract at ADS

Title: Vacuum Solar Telescope Alignment System
Authors: Dunn, R.; Spence, G.; Stebbins, R.; Hill, H.
Bibcode: 1981siwn.conf..613D
Altcode:
  No abstract at ADS

Title: A Antarctic Telescope
Authors: Stebbins, R.
Bibcode: 1981siwn.conf..390S
Altcode:
  No abstract at ADS

Title: Extended Observations of Solar Oscillations
Authors: Stebbins, R. T.; Mann, R.
Bibcode: 1981AnJUS..16..223S
Altcode:
  No abstract at ADS

Title: Observational tests of pulsation theory in the solar envelope
Authors: Stebbins, R. T.; Hill, H. A.; Zanoni, R.; Davis, R. E.
Bibcode: 1980LNP...125..381S
Altcode: 1980nnsp.work..381S
  An improved observing technique has been used to look for long period
  oscillations in the brightness of the extreme solar limb. This technique
  provides a means for analyzing power spectra to secure a signature
  characteristic of the signal's origin. Results show significant
  improvement in the discrimination between solar oscillations, other
  signals, and noise. Long period intensity oscillations can be seen at
  the extreme solar limb.

Title: Observations of long period oscillations in the solar limb
    darkening function
Authors: Stebbins, R. T.
Bibcode: 1980LNP...125..191S
Altcode: 1980nnsp.work..191S
  The FFTD (finite Fourier transform definition) method was extended by
  simultaneous application of multiple edge definitions in a study of
  long period solar oscillations. Results are presented as evidence of
  the reality of long period brightness oscillations in the solar limb
  darkening function.

Title: Analysis of Pulsation Theory Tests in the Solar Envelope
Authors: Stebbins, R. T.
Bibcode: 1979BAAS...11..398S
Altcode:
  No abstract at ADS

Title: Empirical tests of solar pulsation theory.
Authors: Stebbins, R. T.
Bibcode: 1978BAAS...10..730S
Altcode:
  No abstract at ADS

Title: Long-period oscillations of the apparent solar diameter:
    observations.
Authors: Brown, T. M.; Stebbins, R. T.; Hill, H. A.
Bibcode: 1978ApJ...223..324B
Altcode:
  New observations of the time-varying component of the apparent solar
  diameter are reported. Power spectra derived from these observations
  reveal narrow-band oscillations at frequencies consistent with the
  normal mode frequencies of a standard solar model. The amplitudes of
  these oscillations are discussed and related to the observations of
  other investigators. A detailed analysis of the experiment and its
  associated sources of error is presented and used to show that there
  is a very small likelihood that the power spectrum peaks are due to
  nonsolar causes.

Title: Observations of Long Period Solar Oscillations.
Authors: Stebbins, R.
Bibcode: 1977BAAS....9R.568S
Altcode:
  No abstract at ADS

Title: Observed Oscillations of the Apparent Solar Diameter
Authors: Brown, T. M.; Stebbins, R. T.; Hill, H. A.
Bibcode: 1976ssp..conf....1B
Altcode:
  No abstract at ADS

Title: Recent solar oblateness observations: data, interpretation,
    and significance for earlier work.
Authors: Hill, H. A.; Stebbins, R. T.
Bibcode: 1975NYASA.262..472H
Altcode:
  The paper compiles the evidence necessary for the interpretation
  of an observed solar oblateness. Emphasis is on time-varying excess
  brightness, intrinsic visual oblateness, and normal oscillation modes of
  the sun. Solar edge definition is discussed, with particular attention
  paid to the finite Fourier transform definition. The possible role of
  solar oblateness in gravitation theory is considered.

Title: The finite Fourier transform definition of an edge on the
    solar disk.
Authors: Hill, H. A.; Stebbins, R. T.; Oleson, J. R.
Bibcode: 1975ApJ...200..484H
Altcode:
  A technique for locating the edge of the sun is proposed. The technique
  uses a finite Fourier transform of the observed limb-darkening function
  to achieve reduced sensitivity to atmospheric and instrumental
  effects and heightened sensitivity to the shape of the intrinsic
  limb-darkening function. A theory is developed that predicts these
  sensitivities. In order to facilitate wider application, general
  relations are calculated. A testing program which complements the theory
  is also reported. The location of the edge is shown to be influenced
  only by solar phenomena down to the milli-arcsecond range.

Title: The intrinsic visual oblateness of the sun.
Authors: Hill, H. A.; Stebbins, R. T.
Bibcode: 1975ApJ...200..471H
Altcode:
  Solar oblateness observations are reported which yield a value of 18.4
  plus or minus 12.5 milli-arcsec for the difference between equatorial
  and polar diameters. These observations were conducted when the
  time-varying excess equatorial brightness was markedly reduced, greatly
  simplifying the interpretation of the apparent solar oblateness. The
  experimental scheme for defining the 'edge' of the sun and monitoring
  the shape of the extreme limb-darkening function is summarized along
  with a description of the instrumentation. Sources of systematic error
  are exhaustively surveyed to extract the intrinsic visual oblateness
  of the sun. The result further strengthens the conclusion of Hill et
  al. (1974) that the grave consequence of the Dicke-Goldenberg (1967)
  work for Einstein's general theory of relativity is removed. This
  result excludes an oblateness as large as that required by the rapidly
  rotating interior models used to explain the low neutrino flux.

Title: INVITED PAPER - Recent Progress in Solar Oblateness Studies
Authors: Hill, H. A.; Stebbins, R. T.; Brown, T. M.
Bibcode: 1975BAAS....7R.478H
Altcode:
  No abstract at ADS

Title: Solar Oblateness, Excess Brightness, and Relativity.
Authors: Hill, H. A.; Clayton, P. D.; Patz, D. L.; Healy, A. W.;
   Stebbins, R. T.; Oleson, J. R.; Zanoni, C. A.
Bibcode: 1975PhRvL..34Q.296H
Altcode:
  No abstract at ADS

Title: An observational investigation of the solar oblateness
Authors: Stebbins, Robin Tucker Tuck
Bibcode: 1975PhDT.......304S
Altcode:
  No abstract at ADS

Title: Errata: "Solar oblateness, excess brightness, and relativity"
    [Phys. Rev. Lett., Vol. 33, p. 1497 - 1500 (1974)].
Authors: Hill, H. A.; Clayton, P. D.; Patz, D. L.; Healy, A. W.;
   Stebbins, R. T.; Oleson, J. R.; Zanoni, C. A.
Bibcode: 1975PhRvL..34..296H
Altcode:
  No abstract at ADS

Title: An Observational Investigation of the Solar Oblateness.
Authors: Stebbins, R. T.
Bibcode: 1975PhDT.........8S
Altcode:
  In recent years, the sun's figure has come under close scrutiny
  because it may reflect certain properties of the solar interior,
  and because an aspherical solar mass would alter the interpretation
  of a basic test of gravitation theories. A flurry of activity in this
  area has been triggered by the 1967 report of an equatorial diameter
  significantly larger than the polar diameter. A measurement of the
  solar oblateness using different experimental techniques which finds
  no comparable oblateness is reported. Further, the evidence indicates
  an explanation for the disagreement between previous results. A number
  of other interesting facets of the sun are also revealed.

Title: Solar Oblateness, Excess Brightness, and Relativity
Authors: Hill, H. A.; Clayton, P. D.; Patz, D. L.; Healy, A. W.;
   Stebbins, R. T.; Oleson, J. R.; Zanoni, C. A.
Bibcode: 1974PhRvL..33.1497H
Altcode:
  New observations show a small difference between the sun's polar and
  equatorial limb darkening functions. This excess equatorial brightness
  varies in time and can be of sufficient magnitude to account for
  the solar oblateness inferred by Dicke and Goldenberg from their
  measurements. This removes the serious consequence of their work for
  Einstein's general theory of relativity. The problems of a solar-edge
  definition and the derivation of a solar mass quadrupole moment are
  discussed.

Title: Upper Limit on the Gravitational Flux Reaching the Earth from
    the Crab Pulsar
Authors: Levine, Judah; Stebbins, Robin
Bibcode: 1972PhRvD...6.1465L
Altcode:
  A 30-m laser interferometer has been used in a search for gravitational
  radiation from the Crab pulsar. The minimum detectable signal would be
  produced by an incident gravitational flux of 10<SUP>9</SUP> ergs/sec
  cm<SUP>2</SUP> and we find no effect at this level.

