DOCSLIB.ORG

Astronomy Astrophysics

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Astronomy Astrophysics A&A 448, 787–800 (2006) Astronomy DOI: 10.1051/0004-6361:20053516 & c ESO 2006 Astrophysics Performance study of ground-based infrared Bracewell interferometers Application to the detection of exozodiacal dust disks with GENIE O. Absil1,,R.denHartog2, P. Gondoin2,P.Fabry2,R.Wilhelm3, P. Gitton3, and F. Puech3 1 Institut d’Astrophysique et de Géophysique, Université de Liège, 17 Allée du Six Août, 4000 Sart-Tilman, Belgium e-mail: [email protected] 2 Science Payloads and Advanced Concepts Office, ESA/ESTEC, postbus 299, 2200 AG Noordwijk, The Netherlands 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany Received 25 May 2005 / Accepted 2 November 2005 ABSTRACT Nulling interferometry, a powerful technique for high-resolution imaging of the close neighbourhood of bright astrophysical objets, is currently considered for future space missions such as Darwin or the Terrestrial Planet Finder Interferometer (TPF-I), both aiming at Earth-like planet detection and characterization. Ground-based nulling interferometers are being studied for both technology demonstration and scientific prepa- ration of the Darwin/TPF-I missions through a systematic survey of circumstellar dust disks around nearby stars. In this paper, we investigate the influence of atmospheric turbulence on the performance of ground-based nulling instruments, and deduce the major design guidelines for such instruments. End-to-end numerical simulations allow us to estimate the performance of the main subsystems and thereby the actual sen- sitivity of the nuller to faint exozodiacal disks. Particular attention is also given to the important question of stellar leakage calibration. This study is illustrated in the context of GENIE, the Ground-based European Nulling Interferometer Experiment, to be installed at the VLTI and working in the L band. We estimate that this instrument will detect exozodiacal clouds as faint as about 50 times the Solar zodiacal cloud, thereby placing strong constraints on the acceptable targets for Darwin/TPF-I. Key words. instrumentation: high angular resolution – instrumentation: interferometers – techniques: interferometric – circumstellar matter – planetary systems 1. Introduction The principle of nulling interferometry, first proposed by Bracewell (1978) and generalized by several authors (Angel The existence of extraterrestrial life in the Universe is a long- 1989; Léger et al. 1996; Angel & Woolf 1997; Karlsson & standing question of humankind. Future space missions such Mennesson 2000; Absil et al. 2003c), is to combine the light as Darwin (Fridlund 2000) or the Terrestrial Planet Finder collected by two or more telescopes in a co-axial mode, ad- Interferometer (Beichman et al. 1999; Lawson & Dooley 2005) justing their respective phases in order to produce a totally de- are currently being studied respectively by ESA and NASA structive interference on the optical axis. The interferometer to search for evidence of life on Earth-like exoplanets by is characterized by its transmission map Tλ(θ, φ), displayed in means of nulling interferometry (Bracewell 1978). These am- Fig. 1 for a two-telescope interferometer, in one arm of which bitious missions are particularly innovative from the technol- a phase shift of π radians has been introduced (Bracewell in- ogy point of view and demand several techniques to be first terferometer). Assuming that the field-of-view is limited by the tested on ground. Both ESA and NASA have therefore initiated diffraction pattern of a single telescope, its expression results studies for ground-based infrared nulling interferometers (or from the fringe pattern produced by the interference between “nullers”), to be installed respectively at the VLTI (Glindemann the beams, i.e., for a two-telescope interferometer: et al. 2004) or Keck Interferometer (Colavita et al. 2004). A cryogenic nulling beam-combiner is also under development πθ /λ 2 θ 2J1( D ) 2 B Tλ(θ, φ) = sin π cos φ , (1) for the LBT in the context of the NASA Origins Program πθD/λ λ (Herbst & Hinz 2004). where θ and φ are respectively the radial and polar angular co- O.A. acknowledges the financial support of the Belgian National ordinates with respect to the optical axis, B the interferometer Fund for Scientific Research (FNRS). baseline, D the telescope diameter and λ the wavelength. In the Article published by EDP Sciences and available at http://www.edpsciences.org/aa or http://dx.doi.org/10.1051/0004-6361:20053516 788 O. Absil et al.: Performance study of ground-based infrared Bracewell interferometers sequence stars up to 25 pc (Stankov et al. 2005), with median distances to these four stellar types of respectively 20, 20, 19 and 15 pc. Ideally, the survey should detect exozodiacal clouds about 20 times as dense as the Solar zodiacal cloud (“20-zodi” clouds hereafter). Based on the model of Kelsall et al. (1998), such clouds are typically 104 times fainter than the star in the L band (centered around 3.8 µm) or 103 times fainter in the N band (centered around 10.5 µm). The M band will not be considered in this study, because is too much affected by wa- ter vapor to be useful for nulling interferometry (Young et al. 1994). Besides this survey aspect, ground-based nullers have var- ious interesting scientific applications. Any target requiring both high dynamic range and high angular resolution will ben- efit from their capabilities, including the detection and char- Fig. 1. Monochromatic transmission map for a 47 m Bracewell in- acterization of debris disks around Vega-type stars, proto- terferometer formed of two 8-m telescopes. The interferometric planetary disks around Young Stellar Objects, high-contrast field-of-view, limited by the use of single-mode waveguides (see binaries, bounded brown dwarfs and hot extrasolar giant plan- Ω=λ2/ Sect. 3.3), is given by S with S the telescope surface. Its ets. Extragalactic studies may also benefit from ground-based diameter is respectively of 137 mas and 378 mas at the centers of the nulling through the characterization of dust tori around nearby L and N bands. The transmission map acts as a “photon sieve”: it AGNs. Ground-based nullers are extremely powerful at angular shows the parts of the field that are transmitted (white stripes) and those that are blocked (dark stripes, including the central dark fringe) diameter measurements as well: thanks to their very high sta- by the interference process. The whole transmitted flux is integrated bility, they could, for instance, detect pulsations in unresolved on a single pixel. stars that still produce a non negligible stellar leakage in the nulled data. In this paper, we estimate the performance of ground-based following study, we assume that recombination and detection infrared nulling interferometers for the detection of exozodia- are both done in the pupil plane, so that no image is formed: cal dust around typical Darwin/TPF-I targets. The structure of the flux is integrated on the field-of-view and detected on a sin- the paper follows the path of the light, beginning with the as- gle pixel. Performing the detection in an image plane would not trophysical sources and ending up after detection with the data significantly change the conclusions of this study. analysis procedures. In Sect. 2, we present the different con- Besides pure technology demonstration, ground-based tributors to the detected signals in ground-based nulling inter- nullers have an important scientific goal in the context of the ferometry. Section 3 then focuses on a particularly important Darwin/TPF-I missions, through the detection of faint circum- contributor (instrumental leakage), which strongly depends on stellar dust disks (“exozodiacal dust disks”) around nearby the turbulent processes taking place in the Earth’s atmosphere. main sequence stars. Such dust clouds may present a severe We will show that this stochastic contributor needs to be com- limitation to Earth-like planet detection with Darwin/TPF-I pensated in real time at the hardware level in order to reach the if they are more than 20 times as dense as the Solar zodia- required sensitivity. This has important consequences for the cal cloud (Absil 2001). A systematic survey of nearby main- design of a ground-based nulling interferometer, as discussed sequence stars is thus mandatory to select convenient targets in Sect. 4, where real-time control loops are addressed. After for these future space missions. Photometric surveys with in- passing though the instrument and being recorded by the de- frared space telescopes such as IRAS, ISO and Spitzer have tector, the signal still needs to be carefully analyzed in order to detected cold dust around nearby stars at a level of ∼100 times extract the useful exozodiacal contribution from the raw data. our Kuiper Belt, but did not allow the characterization of warm Section 5 describes the associated post-processing techniques. dust emission at a better level than about 500 times the Solar In all these sections, we will take a Sun-like G2V star at 20 pc zodiacal cloud (Beichman et al. 2005). Attempts to spatially re- as a typical target for illustrative purposes. Finally, these con- solve faint exozodiacal clouds with single dish telescopes in the cepts are applied in Sect. 6, where we derive the expected sensi- mid-infrared (Kuchner et al. 1998) and near infrared (Kuchner tivity of a specific instrument to the dust emission for different & Brown 2000) have not yielded better detection limits. Even types of targets in the Darwin star catalogue. the MIRI instrument onboard the future James Webb Space Telescope, equipped with coronagraphic devices at 10.6 µm and other longer wavelengths, does not have a good enough 2. Signals and noises in ground-based nulling angular resolution (∼330 mas) to detect warm dust within the interferometry habitable zone of Darwin/TPF candidate targets. 2.1. Exozodiacal dust disk Nulling interferometry, combining high dynamic range and high angular resolution, is particularly appropriate to carry out The Solar zodiacal cloud, a sparse disk of 10–100 µmdiame- this systematic survey of the Darwin/TPF-I candidate targets.
Load more

Recommended publications
  • Michael Garcia Hubble Space Telescope Users Committee (STUC)
    Hubble Space Telescope Users Committee (STUC) April 16, 2015 Michael Garcia HST Program Scientist [email protected] 1 Hubble Sees Supernova Split into Four Images by Cosmic Lens 2 NASA’s Hubble Observations suggest Underground Ocean on Jupiter’s Largest Moon Ganymede file:///Users/ file:///Users/ mrgarci2/Desktop/mrgarci2/Desktop/ hs-2015-09-a-hs-2015-09-a- web.jpg web.jpg 3 NASA’s Hubble detects Distortion of Circumstellar Disk by a Planet 4 The Exoplanet Travel Bureau 5 TESS Transiting Exoplanet Survey Satellite CURRENT STATUS: • Downselected April 2013. • Major partners: - PI and science lead: MIT - Project management: NASA GSFC - Instrument: Lincoln Laboratory - Spacecraft: Orbital Science Corp • Agency launch readiness date NLT June 2018 (working launch date August 2017). • High-Earth elliptical orbit (17 x 58.7 Earth radii). Standard Explorer (EX) Mission PI: G. Ricker (MIT) • Development progressing on plan. Mission: All-Sky photometric exoplanet - Systems Requirement Review (SRR) mapping mission. successfully completed on February Science goal: Search for transiting 12-13, 2014. exoplanets around the nearby, bright stars. Instruments: Four wide field of view (24x24 - Preliminary Design Review (PDR) degrees) CCD cameras with overlapping successfully completed Sept 9-12, 2014. field of view operating in the Visible-IR - Confirmation Review, for approval to enter spectrum (0.6-1 micron). implementation phase, successfully Operations: 3-year science mission after completed October 31, 2014. launch. - Mission CDR on track for August 2015 6 JWST Hardware Progress JWST remains on track for an October 2018 launch within its replan budget guidelines 7 WFIRST / AFTA Widefield Infrared Survey Telescope with Astrophysics Focused Telescope Assets Coronagraph Technology Milestones Widefield Detector Technology Milestones 1 Shaped Pupil mask fabricated with reflectivity of 7/21/14 1 Produce, test, and analyze 2 candidate 7/31/14 -4 10 and 20 µm pixel size.
    [Show full text]
  • Report by the ESA–ESO Working Group on Extra-Solar Planets
    Report by the ESA–ESO Working Group on Extra-Solar Planets 4 March 2005 Summary Various techniques are being used to search for extra-solar planetary signatures, including accurate measurement of radial velocity and positional (astrometric) dis- placements, gravitational microlensing, and photometric transits. Planned space experiments promise a considerable increase in the detections and statistical know- ledge arising especially from transit and astrometric measurements over the years 2005–15, with some hundreds of terrestrial-type planets expected from transit mea- surements, and many thousands of Jupiter-mass planets expected from astrometric measurements. Beyond 2015, very ambitious space (Darwin/TPF) and ground (OWL) experiments are targeting direct detection of nearby Earth-mass planets in the habitable zone and the measurement of their spectral characteristics. Beyond these, ‘Life Finder’ (aiming to produce confirmatory evidence of the presence of life) and ‘Earth Imager’ (some massive interferometric array providing resolved images of a distant Earth) arXiv:astro-ph/0506163v1 8 Jun 2005 appear as distant visions. This report, to ESA and ESO, summarises the direction of exo-planet research that can be expected over the next 10 years or so, identifies the roles of the major facilities of the two organisations in the field, and concludes with some recommendations which may assist development of the field. The report has been compiled by the Working Group members and experts (page iii) over the period June–December 2004. Introduction & Background Following an agreement to cooperate on science planning issues, the executives of the European Southern Observatory (ESO) and the European Space Agency (ESA) Science Programme and representatives of their science advisory structures have met to share information and to identify potential synergies within their future projects.
    [Show full text]
  • Stsci Newsletter: 2011 Volume 028 Issue 02
    National Aeronautics and Space Administration Interacting Galaxies UGC 1810 and UGC 1813 Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA) 2011 VOL 28 ISSUE 02 NEWSLETTER Space Telescope Science Institute We received a total of 1,007 proposals, after accounting for duplications Hubble Cycle 19 and withdrawals. Review process Proposal Selection Members of the international astronomical community review Hubble propos- als. Grouped in panels organized by science category, each panel has one or more “mirror” panels to enable transfer of proposals in order to avoid conflicts. In Cycle 19, the panels were divided into the categories of Planets, Stars, Stellar Rachel Somerville, [email protected], Claus Leitherer, [email protected], & Brett Populations and Interstellar Medium (ISM), Galaxies, Active Galactic Nuclei and Blacker, [email protected] the Inter-Galactic Medium (AGN/IGM), and Cosmology, for a total of 14 panels. One of these panels reviewed Regular Guest Observer, Archival, Theory, and Chronology SNAP proposals. The panel chairs also serve as members of the Time Allocation Committee hen the Cycle 19 Call for Proposals was released in December 2010, (TAC), which reviews Large and Archival Legacy proposals. In addition, there Hubble had already seen a full cycle of operation with the newly are three at-large TAC members, whose broad expertise allows them to review installed and repaired instruments calibrated and characterized. W proposals as needed, and to advise panels if the panelists feel they do not have The Advanced Camera for Surveys (ACS), Cosmic Origins Spectrograph (COS), the expertise to review a certain proposal. Fine Guidance Sensor (FGS), Space Telescope Imaging Spectrograph (STIS), and The process of selecting the panelists begins with the selection of the TAC Chair, Wide Field Camera 3 (WFC3) were all close to nominal operation and were avail- about six months prior to the proposal deadline.
    [Show full text]
  • An Implementation Concept for the ASPIRE Mission
    An Implementation Concept for the ASPIRE Mission. W. D. Deininger* ([email protected]), W. Purcell,* P. Atcheson,*G. Mills,* S. A Sandford,** R. P. Hanel,** M. McKelvey,** and R. McMurray** *Ball Aerospace & Technologies Corp. (BATC) P. O. Box 1062 Boulder, CO, USA 80306-1062 **NASA Ames Research Center Moffett Field, CA, USA 94035 Abstract—The Astrobiology Space Infrared Explorer complex and tied to the cyclic process whereby these (ASPIRE) is a Probe-class mission concept developed as elements are ejected into the diffuse interstellar medium part of NASA’s Astrophysics Strategic Mission Concept (ISM) by dying stars, gathered into dense clouds and studies. 1 2 ASPIRE uses infrared spectroscopy to explore formed into the next generation of stars and planetary the identity, abundance, and distribution of molecules, systems (Figure 1). Each stage in this cycle entails chemical particularly those of astrobiological importance throughout alteration of gas- and solid-state species by a diverse set of the Universe. ASPIRE’s observational program is focused astrophysical processes: hocks, stellar winds, radiation on investigating the evolution of ices and organics in all processing by photons and particles, gas-phase neutral and phases of the lifecycle of carbon in the universe, from ion chemistry, accretion, and grain surface reactions. These stellar birth through stellar death while also addressing the processes create new species, destroy old ones, cause role of silicates and gas-phase materials in interstellar isotopic enrichments, shuffle elements between chemical organic chemistry. ASPIRE achieves these goals using a compounds, and drive the universe to greater molecular Spitzer-derived, cryogenically-cooled, 1-m-class telescope complexity.
    [Show full text]
  • Astronomers Mull Merger of Missions
    NEWS IN FOCUS project along these lines — was indefinitely postponed in 2007, but the agency has contin- ued to put US$6 million a year into developing technology for exoplanet searches. Now planet NASA/JPL-CALTECH hunters think that joining forces with COPAG will be the winning strategy. Jim Kasting, a plan- etary scientist at Pennsylvania State University in University Park who is chair of the exoplanet group, says the two communities would both like to see a 4–8-metre telescope in space that would cost in excess of $5 billion. “Our interests are basically aligned,” he says. Such a mission would compete for top billing in the next decadal survey of astronomy by the US National Academy of Sciences, due in 2020. The big question, which follow-up meetings will consider, is whether the same technology can do both kinds of science. A cosmic-origins mission would need to collect as much ultraviolet and visible light as possible to image intergalactic gas, star formation and Exoplanet hunters want something to replace the postponed Terrestrial Planet Finder. Sun-like stars in nearby galaxies. A planet-hunt- ing probe would need a coronagraph to block SPACE SCIENCE direct light from host stars, and would have to be sensitive to the visible and near-infrared wavelengths that Earth-like planets primar- ily emit. The infrared 6.5-metre James Webb Astronomers mull Space Telescope (JWST), scheduled for launch in 2014, will be able to see larger planets but will not be sensitive to Earth-sized ones. The key to making the joint concept work will be develop- merger of missions ing a reflective coating for the telescope’s mirror that works from the ultraviolet to the infrared ranges and does not distort the incoming light Cosmic-origins scientists convene with exoplanet hunters.
    [Show full text]
  • Cosmic Origins Program Analysis Group
    Cosmic Origins Program Analysis Group Ken Sembach (STScI) 2014 COPAG Execuve CommiEee Daniela Julianne Dennis James Sally CalzeH Dalcanton Ebbets Green Heap Lynn David James Paul Ken Hillenbrand Leisawitz Lowenthal Scowen Sembach2 2014 COPAG Ex-Officio Members Susan Neff Mario Perez Michael Garcia GSFC COR Program Office NASA HQ NASA HQ COPAG members recently compleCng service: Jonathan Gardner Paul Goldsmith Charles Lillie Christopher MarCn 3 Cosmic Origins Quesons • How did we get here? – How and when did galaxies form? – How do stars form, evolve, and eventually die? – How are maer and the chemical elements distributed throughout the universe? 4 COPAG Tasks • Solicit and coordinate community input into the development and execuCon of NASA’s Cosmic Origins (COR) Program • Analyze this input in support of the planning and prioriCzaon of future exploraon within the COR program • Specific types of tasks include – ArCculang and prioriCzing key science drivers for COR research – Evaluang capabiliCes of potenCal missions for achieving COR science goals – Providing input and analysis on related acCviCes (e.g., ground-based observing, theory invesCgaons, laboratory astrophysics, suborbital invesCgaons, data archiving, etc) needed to achieve COR science goals – IdenCfying focus areas for technologies needed to advance COR science • All input is provided to the NASA Astrophysics SubcommiEee 5 2014 Science Analysis Groups (SAGs) and Science Interest Groups (SIGs) • SAG #6: Cosmic Origins Science Enabled by the WFIRST-AFTA Coronagraph • SAG #7: Science
    [Show full text]
  • Interferometric Space Missions for Exoplanet Science: Legacy of Darwin/TPF
    Interferometric Space Missions for Exoplanet Science: Legacy of Darwin/TPF D. Defrere` 1, O. Absil1, and C. Beichman2 1 Space sciences, Technologies & Astrophysics Research (STAR) Institute, University of Liege, Liege, Belgium. 2 NASA Exoplanet Science Institute, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, Califor- nia, USA. Abstract DARWIN/TPF is a project of an infrared space-based interferometer designed to directly detect and charac- terize terrestrial exoplanets around nearby stars. Unlike spectro-photometric instruments observing planetary transits, an interferometer does not rely on any particular geometric constraints and could characterize exoplanets with any orbital configuration around nearby stars. The idea to use an infrared nulling interferometer to characterize exoplanets dates back to Bracewell(1978), and was extensively studied in the 1990s and 2000s by both ESA and NASA. The project focuses on the mid-infrared regime (5-20 mm), which provides access to key features of exoplanets, such as their size, their temperature, the presence of an atmosphere, their climate structure, as well as the presence of impor- tant atmospheric molecules such as H2O, CO2,O3, NH3, and CH4. This wavelength regime also provides a favorable planet/star contrast to detect the thermal emission of temperate (∼ 300 K) exoplanets (107 vs 1010 in the visible). In this chapter, we first review the scientific rationale of a mid-infrared nulling interferometer and present how it would provide an essential context for interpreting detections of possible biosignatures. Then, we present the main techno- logical challenges identified during the ESA and NASA studies, and how they have progressed over the last 10 years.
    [Show full text]
  • Cosmic Origins RFI Responses PASP Final
    Scientific Objectives for UV/Visible Astrophysics Investigations: A Summary of Responses by the Community (2012) Paul A. Scowen1, Mario R. Perez2, Susan G. Neff3, and Dominic J. Benford3 Abstract Following several recommendations presented by the Astrophysics Decadal Survey 2010 centered around the need to define “a future ultraviolet-optical space capability,” on 2012 May 25, NASA issued a Request for Information (RFI) seeking persuasive ultraviolet (UV) and visible wavelength astrophysics science investigations. The goal was to develop a cohesive and compelling set of science objectives that motivate and support the development of the next generation of ultraviolet/visible space astrophysics missions. Responses were due on 10 August 2012 when 34 submissions were received addressing a number of potential science drivers. A UV/visible Mission RFI Workshop was held on 2012 September 20 where each of these submissions was summarized and discussed in the context of each other. We present a scientific analysis of these submissions and presentations and the pursuant measurement capability needs, which could influence ultraviolet/visible technology development plans for the rest of this decade. We also describe the process and requirements leading to the inception of this community RFI, subsequent workshop and the expected evolution of these ideas and concepts for the remainder of this decade. Keywords: Conference Summary; Astronomical Instrumentation; Galaxies; Stars; Extrasolar Planets I. Introduction It has been recognized that at mid- and near-ultraviolet wavelengths (90 < λ < 300 nm), it is possible to detect and measure important astrophysical processes, which can shed light into the physical conditions of many environments of interest. For example, in the local interstellar medium (LISM) all but two (CaII H and K lines) of the key diagnostic of resonance lines are in the ultraviolet (Redfield 2006), which is depicted in Figure 1.
    [Show full text]
  • Sessions Calendar
    Associated Societies GSA has a long tradition of collaborating with a wide range of partners in pursuit of our mutual goals to advance the geosciences, enhance the professional growth of society members, and promote the geosciences in the service of humanity. GSA works with other organizations on many programs and services. AASP - The American Association American Geophysical American Institute American Quaternary American Rock Association for the Palynological Society of Petroleum Union (AGU) of Professional Association Mechanics Association Sciences of Limnology and Geologists (AAPG) Geologists (AIPG) (AMQUA) (ARMA) Oceanography (ASLO) American Water Asociación Geológica Association for Association of Association of Earth Association of Association of Geoscientists Resources Association Argentina (AGA) Women Geoscientists American State Science Editors Environmental & Engineering for International (AWRA) (AWG) Geologists (AASG) (AESE) Geologists (AEG) Development (AGID) Blueprint Earth (BE) The Clay Minerals Colorado Scientifi c Council on Undergraduate Cushman Foundation Environmental & European Association Society (CMS) Society (CSS) Research Geosciences (CF) Engineering Geophysical of Geoscientists & Division (CUR) Society (EEGS) Engineers (EAGE) European Geosciences Geochemical Society Geologica Belgica Geological Association Geological Society of Geological Society of Geological Society of Union (EGU) (GS) (GB) of Canada (GAC) Africa (GSAF) Australia (GSAus) China (GSC) Geological Society of Geological Society of Geologische Geoscience
    [Show full text]
  • Cosmic Origins Program Analysis Group
    Cosmic Origins Program Analysis Group Astrophysics Subcommi8ee Mee;ng March 26-27, 2014 Kenneth Sembach 1 2014 COPAG Execuve Commi8ee • Current Members – Daniela CalzeJ University of Massachuse8s – Amherst – Julianne Dalcanton University of Washington – Dennis Ebbets Ball Aerospace – Michael Garcia (ex-officio) NASA Headquarters – James Green University of Colorado – Boulder – Sally Heap Goddard Space Flight Center – Lynne Hillenbrand California Ins;tute of Technology – David Leisawitz Goddard Space Flight Center – James Lowenthal Smith College – Susan Neff (ex-officio) GSFC COR Program Office – Mario Perez (ex-officio, Ex. Secretary) NASA Headquarters – Paul Scowen Arizona State University – Ken Sembach (Chair) Space Telescope Science Ins;tute Members in red are new to the Execu;ve Commi8ee since the November 2013 Astrophysics Subcommi8ee telecon 2 Recent Ac;vi;es • Recruitment of new Execu;ve Commi8ee members • Establishment of 3 new Science Analysis Groups, as approved at the November 2013 ApS telecon – SAG #6: Cosmic Origins Science Enabled by the WFIRST-AFTA Coronagraph • COPAG Lead: James Green – SAG #7: Science Enabled by Operaons Overlap of the Hubble Space Telescope and the James Webb Space Telescope • COPAG Lead: Dennis Ebbets – SAG #8: Science Enabled by the WFIRST-AFTA Data Archive • COPAG Lead: Sally Heap (See backup slides for more details) 3 Recent Ac;vi;es • Establishment of 1 new Science Interest Group, as approved at the November 2013 ApS telecon – SIG #1: Far-Infrared Cosmic Origins Science and Technology Development • Lead:
    [Show full text]
  • Not Yet Imagined: a Study of Hubble Space Telescope Operations
    NOT YET IMAGINED A STUDY OF HUBBLE SPACE TELESCOPE OPERATIONS CHRISTOPHER GAINOR NOT YET IMAGINED NOT YET IMAGINED A STUDY OF HUBBLE SPACE TELESCOPE OPERATIONS CHRISTOPHER GAINOR National Aeronautics and Space Administration Office of Communications NASA History Division Washington, DC 20546 NASA SP-2020-4237 Library of Congress Cataloging-in-Publication Data Names: Gainor, Christopher, author. | United States. NASA History Program Office, publisher. Title: Not Yet Imagined : A study of Hubble Space Telescope Operations / Christopher Gainor. Description: Washington, DC: National Aeronautics and Space Administration, Office of Communications, NASA History Division, [2020] | Series: NASA history series ; sp-2020-4237 | Includes bibliographical references and index. | Summary: “Dr. Christopher Gainor’s Not Yet Imagined documents the history of NASA’s Hubble Space Telescope (HST) from launch in 1990 through 2020. This is considered a follow-on book to Robert W. Smith’s The Space Telescope: A Study of NASA, Science, Technology, and Politics, which recorded the development history of HST. Dr. Gainor’s book will be suitable for a general audience, while also being scholarly. Highly visible interactions among the general public, astronomers, engineers, govern- ment officials, and members of Congress about HST’s servicing missions by Space Shuttle crews is a central theme of this history book. Beyond the glare of public attention, the evolution of HST becoming a model of supranational cooperation amongst scientists is a second central theme. Third, the decision-making behind the changes in Hubble’s instrument packages on servicing missions is chronicled, along with HST’s contributions to our knowledge about our solar system, our galaxy, and our universe.
    [Show full text]
  • Astrophysics
    National Aeronautics and Space Administration Astrophysics Astronomy and Astrophysics Paul Hertz Advisory Committee Director, Astrophysics Division Telecon Meeting Science Mission Directorate February 25, 2016 @PHertzNASA What’s New? • LISA Pathfinder launched on December 3, 2015 • NASA’s FY16 budget appropriation signed on December 18, 2015 • NASA’s FY17 budget requested submitted on February 9, 2016 • Hitomi (neé ASTRO-H) launched on February 17, 2016 • WFIRST began formulation on February 17, 2016 • ROSES-16 released on February 19, 2016 2 LISA Pathfinder ST-7/Disturbance Reduction System (DRS) Launched December 3, 2015 Dec 3 Launch Dec 11 On way to L1 Jan 22 Arrive at L1 Feb 3 Uncage test masses Feb 15 Test mass 1 “Elwood” release Feb 16 Test mass 2 “Jake” release Mar 1 Begin LTP operations (90 days) Jun 20 Begin DRS operations (90 days) Sep 20 ESA mission extension review http://sci.esa.int/lisa-pathfinder/ https://lisapathfinder.org/ 3 Hitomi (ASTRO-H) Soft X-ray Spectrometer (SXS) • ASTRO-H successfully launched on Feb 17, 2016 from Tanegashima Space Center on a H-IIA launch vehicle. • The word Hitomi translates into "eye" or "pupil" hence the spacecraft has become the aperture with which to see the secrets of the universe. o Feb 25 SXS first light o Feb 28 Deployment of extensible optical bench o Apr 1 Release of Cycle 1 GO call-for-proposals in ROSES (target) https://heasarc.gsfc.nasa.gov/docs/astroh/ 4 WFIRST Wide-Field Infrared Survey Telescope CURRENT STATUS: • Completed Mission Concept Review (MCR) held in December 2015 • Formulation Science Investigation Teams selected in December 2015 • Industry RFI released July 2015; RFP for industry studies released in January 2016; Proposals received from industry in February 2016 to support Wide-field Instrument Concept Study.
    [Show full text]