NASA Origins Probes Concept Studies

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NASA Origins Probes Concept Studies • NASA has selected nine studies to investigate new ideas for future mission concepts within its Astronomical Search for Origins Program.

• Each of the selected studies will have eight months to further develop and refine concepts for missions addressing different aspects of Origins Program science. The Origins Program seeks to address the fundamental questions: "Where did we come from?" and "Are we alone?" NASA received 26 proposals in response to this call for mission concepts.

• The missions under study are $670-M class: larger than current “Explorer” (SMEX and MIDEX) missions, but smaller than flagship great observatories like Hubble.

• There are no “Origins Probes” or funding for such in NASA’s current budget. However if this class of mission is seen (through these studies) to fill a missing ‘gap’ in current Origins program missions, it may be pursued as a future new program.

• Some of the new missions envisioned would survey one billion stars within our own galaxy; measure the distribution of galaxies in the distant universe; study dust and gas between galaxies; study organic compounds in space and investigate their role in planetary system formation; and create an optical-ultraviolet telescope with instruments previously slated for NASA's Hubble Space Telescope. Origins Probes Solicitation Results

• Origins Probe Mission Concept Studies (2004-2005) – Fill missing science in current Origins Program • April 2004, 26 proposals received - 9 selected

PI Institution Short Title BLISS: Revealing the Nature of the Far-IR M. Bradford JPL Universe K. Johnston USNO Origins Billion Star Survey D. Leisawitz GSFC The Space Infrared Interferometric Telescope G. Melnick SAO Cosmic Inflation Probe J. Morse ASU HORUS: High ORbit Ultraviolet-visible Satellite C. Norman JHU Hubble Origins Probe S. Sandford ARC The Astrobiology SPace InfraRed Explorer K. Sembach STScI The Baryonic Structure Probe R. Thompson U of A GEOP: A Galaxy Evolution and Origins Probe Study Results Will Feed Into NASA Roadmapping Activities

• Roadmapping Team will use study results to assess whether proposed missions are sufficiently compelling for them to recommend inclusion in NASA plans

• First draft “Universe roadmap” December 2004 • AAS town hall discussion January 2005 • Second draft April 2005 • Final Draft June 2005 • Final publication October 2005 The selected proposals and their principal investigators are:

• A Background Limited Infrared-Submillimeter Spectrograph for Spica: Revealing the Nature of the Far-Infrared Universe Matt Bradford, JPL, Pasadena, Calif. – The study will enable far-infrared spectroscopy of the galaxies that make up the far-infrared background out to distances of some of the farthest galaxies known today. Its spectral surveys will chart the history of creation of elements heavier than helium and energy production through cosmic time. (Note: Spica is a Japanese mission). • Origins Billion Star Survey Kenneth Johnston, U.S. Naval Observatory, Washington – The survey will provide a complete census of giant extrasolar planets for all types of stars in our galaxy and the demographics of stars within 30,000 light-years of the Sun. Steven Pravdo of JPL is a co-investigator. • The Space Infrared Interferometric Telescope David Leisawitz, Goddard Space Flight Center, Greenbelt, Md. – This imaging and spectral Michelson interferometer operates in the mid- to far-infrared region of the spectrum. Its very high angular resolution in the far-infrared will enable revolutionary developments in the field of star and planet formation research. • Cosmic Inflation Probe Gary Melnick, Smithsonian Astrophysical Observatory, Cambridge, Mass. – The probe will measure the shape of cosmic inflation potential by conducting a space-based, near-infrared, large-area redshift survey capable of detecting galaxies that formed early in the history of the universe. • High Orbit Ultraviolet-visible Satellite Jon Morse, Arizona State University, Tempe. – This mission will conduct a step-wise, systematic investigation of star formation in the Milky Way, nearby galaxies and the high- redshift universe; the origin of the elements and cosmic structure; and the composition of and physical conditions in the extended atmospheres of extrasolar planets. • Hubble Origins Probe Colin Norman, Johns Hopkins University, Baltimore – This mission seeks to combine instruments built for the fifth Hubble servicing mission: Cosmic Origins Spectrograph and Wide Field Camera 3. This new space telescope at the forefront of modern astronomy will have a unifying focus on the period when the great majority of star and planet formation, heavy element production, black-hole growth and galaxy assembly took place. • The Astrobiology Space Infrared Explorer Mission: A Concept Mission to Understand the Role Cosmic Organics Play in the Origin of Life Scott Sandford, Ames Research Center, Moffett Field, Calif. – This is a mid- and far-infrared space observatory optimized to spectroscopically detect and identify organic compounds and related materials in space, and understand how these materials are formed, evolve and find their way to planetary surfaces. Michael Werner and Karen Willacy of JPL are co-investigators. • The Baryonic Structure Probe Kenneth Sembach, Space Telescope Science Institute, Baltimore – The probe will strengthen the foundations of observational cosmology by directly detecting, mapping and characterizing the cosmic web of matter in the early universe, its inflow into galaxies, and its enrichment with elements heavier than hydrogen and helium (the products of stellar and galactic evolution). • Galaxy Evolution and Origins Probe Rodger Thompson, University of Arizona – The probe will observe more than five million galaxies to study the mass assembly of galaxies, the global history of star formation, and the change of galaxy size and brightness over a volume of the universe large enough to determine the fluctuations of these processes. Hubble Origins Probe (HOP) P.I. Colin Norman, Johns Hopkins University [email protected] 410-516-7329

• Dedicated ~2.4 Meter Free Flyer • Core Mission flies Instruments: COS and WFC3 • Launch before 2010 • Lifetime ≥ 5years • Cost within Origins Probes line $500-700M • Synergy with Chandra, Spitzer, JWST • Basic KISS principle Simplest, lowest risk option HOP Overview

• Enhanced Mission possible with international collaboration, subject to schedule constraints. • Extends science with additional instrumentation – Very Wide Field Imaging – (Japan) – Integral Field Unit for visible spectroscopy – (ESA/Australia) • Completes Hubble Science and Important Part of Origins/SEUS Roadmap • Extends Origins/SEUS Roadmap toward Kepler, JWST, TPF-C, SUVO... era • Complements large ground-based telescope initiatives • International Collaboration The Core Science Goals

• Study the Universe from z=0→3 • Covers 80% of the history of the Universe • Is the Epoch of * Star Formation * Planet Formation * Metal Production * Galaxy Assembly • Core Science Questions: – Where are (most of) the Baryons? – How does the Intergalactic Medium collapse to form galaxies? – How does feedback from star formation influence the origin and evolution of galaxies? – When and where did galaxies assemble into their current form? – What physical processes link the formation of supermassive black holes and galactic bulges? – How do planetary systems form and what are their properties? HOP Mission Concept

• No new technology • HST class (2.4m) • LEO low earth orbit (prob. low inclination) • 48 month schedule •COS & WFC3 • Reuse HST Ground System • Operate as a Great Observatory • Aperture Size: – Consider standardly available 1.8m and 2.4m diameter unaberrated mirrors – Trade cost/schedule of heavy Smithsonian NASA mirror vs current technology light mirrors – Use Lower mass OTA – Unaberrated telescope OK for COS and WFC3 with minor modifications including COS gratings (Ball study) • Launcher: – Delta IV, Atlas 5 – Modifications of COS & WFC3 for ELV launch loads vs STS loads is under study. HOP Mission: Estimated Parameters. • Reduced mirror mass, less expensive launch vehicles → reduced cost • WFC3 requires same focal lengths and mirror spacing as HST -> Delta IV –H or equivalent • Optimize Re-use of items e.g ground system, data handling and storage. Identical interfaces. • Mass 10,000 kg, 3.3kW provided • Critical path is primary mirror fabrication Possibilities provided by an Enhanced HOP Mission

• Extend COS sensitivity into UV • Enhance WFC3 filter complement • Add Additional Imaging Instrument -Very Wide Field Imager ( Japan ) (VWFI) • Compensate for Demise of STIS - COS mods for UV spectroscopy - Visible Integral Field Spectrometer as fourth (radial) instrument (ESA?)

• Very Wide Field Imager: – Streamlined Mission A-latches and FGS pickoff mirrors could be removed – Very large expanse opened for VWFI – Very low backgrounds ~100 lower at 1 – Qualitatively different science emerges. – Large FOV (200 arcmin), broad λ coverage, stable PSF VWFI Science • The Origin of Galaxies – Focus on the Emergence of galaxies and structure in the modern universe – Stringent tests of galaxy formation models possible using wide-field multi-filter imaging – Study Galaxy clustering as a function of galaxy luminosity, color, morphology, cosmic epoch – Obtain Mass spectrum as a function of epoch using weak lensing to infer cosmic shear – Study cosmology through SN observations (Snap-lite) • The Origin of Planets – VWFI ideal complement to Kepler – Transit studies: In Galactic Bulge can inspect 2 million FGK dwarfs in a single pointing • → >1000 planetary transits per year. – Microlensing studies: Optical depth toward Bulge is 3 x 10-6. Sensitive to stars down to I ~ 25. 5-6 million stars monitored in a single pointing, 5 concurrent fields monitored • → 100 microlensing event, 10 planets. • method is sensitive to earth-like planets (gravitational) Statement from HOP Team

We are currently evaluating how we might accomplish the HOP mission within the Origins Probe funding limit of $670M. There are significant number of spacecraft and instrument components in existing inventory. In addition, there have been major advances in spacecraft and instrumentation technology in the decades since the construction of HST. Lockheed Martin Corporation and Ball Aerospace Corporation are the industrial partners assisting us in this study. These two companies have extensive HST experience and are currently involved with the SIRTF and Kepler missions. We are also exploring the possibility of international collaboration on HOP. Summary

• HOP completes SM4 science and connects to future NASA missions. • HOP will make unique contributions in key science areas – Evolution of the Intergalactic medium – Galaxy formation and mass assembly – Cosmology – Extra-solar planets (microlensing, transits) • Like HST, HOP would be a flexible Great Observatory, whose uses and returns in the hands of an ingenious community would exceed our expectations. Contact the P.I.’s for More Info! e.g. Dr. Jim Green, P.I., COS [email protected] (for more info on COS, and COS performance on HST vs. MIDEX Explorer platform vs. HOP vs. other free-flier, etc.)

Dr. Colin Norman, HOP Dr. Jon Morse, HORUS and HIFEX Dr. Ken Sembach, Baryonic Structure Probe HORUS: High-ORbit Ultraviolet-visible Satellite Hubble Replacement Origins Science Mission Exploring the Origin, Evolution, and Fate of the Universe PI: Jon Morse (Arizona State University; [email protected]; 480-965-2552); Industry Partner: Lockheed-Martin Science Goals: • Characterize star formation in the Milky Way, the Local Group, and the distant Universe. • Understand how environment influences the process of star and planet formation. • Determine survivability criteria for proto-planetary disks in massive star forming regions, similar to where the Solar Nebula likely formed. • Spectroscopically detect and characterize extrasolar planets. • Develop a classification scheme for star forming regions based on observable stellar and nebular diagnostics, and apply it to the distant Universe. • Also can characterize the nature of dark energy. HORUS: High-ORbit Ultraviolet-visible Satellite Hubble Replacement Origins Science Mission Exploring the Origin, Evolution, and Fate of the Universe

Measurements: • Image all massive star forming regions out to 2.5 kpc through continuum and emission-line filters with sufficient spatial resolution to distinguish Solar System-scale structures. • Conduct a census of all exposed proto-planetary disks in nearby massive star forming regions, and quantify their sizes, orientations, opacities, and distributions. • Observe Kepler and other transit sources spectroscopically to characterize extrasolar planet atmospheres as well as infalling cometary material in protostellar systems • Survey massive star forming regions in the LMC/SMC and nearby Universe with sufficient spatial resolution to distinguish structures and processes that have Galactic analogs. • Extend the survey to star formation in the distant universe by direct imaging and origin of the heavy elements through spectroscopic observations of Ly-α forest clouds and quasars. • Observe distant Type Ia supernovae and weak lensing to measure expansion rate of the Universe and the growth of large scale structure over time. HORUS: Hubble Replacement Origins Science Mission Exploring the Origin, Evolution, and Fate of the Universe

Performance Requirements and Implementation Summary: Primary Mirror Diameter: 2.4m (yields ~0.05˝ resolution at 5000Å) Image Scales: 0.05 arcsec/pixel (hi-res mode); and 0.1 arcsec/pixel (survey mode) Wavelength Coverage: 200 – 1000 nm (imaging); 100 – 200 nm (spectroscopy) Field of View: 14´×14´ (~200 sq-arcmin; 8k×8k FPAs; 25× HST-WFC3) Wavelength Multiplexing: Dichroic split at ~510nm for simultaneous UV-blue and red-NIR imaging; optimized UV-blue and red-NIR channels Spectroscopic Capabilities: 100 – 200 nm; COS-like design; low and medium spectral resolution over a 0.5”x5” slit Imaging Survey Capability: > 40 sq-degs/yr to surf. brightness of 10-16 ergs/cm2/s/arcsec2 Telescope Optical Design: Three mirror anastigmat; diffraction-limited in V-band Detectors: 200-1000nm: Si-CMOS or CCD; 100-300nm Si-MCP-CsI,CsTe Orbit and Mission Duration: Earth-Sun L2; 5 year core mission, 10 year goal

Cost Envelope: $670M (FY04, life-cycle costs; SIRTF-class) Discovery Efficiency: Imaging: Designed to be 100x HST-WFC3/ACS capabilities; Spectroscopic: >10x HST-STIS (restore COS-like performance) H/W Re-Use: Re-host COS and cannibalize WFC3 to achieve state-of-the-art. The Hubble Instrument Free-flying Explorer (HIFEX): [a.k.a. “HST-lite”] A Low Cost Option to Deploy the Hubble Wide Field Camera 3 (WFC3) and the Cosmic Origins Spectrograph (COS) [not an Origins Probe study]

Fixed Light COS, WFC3 & FPA Shield Instrument Module

Spacecraft Bus

Deployable Light Shield Optical and Aperture Door Telescope Assembly

The 1.8m diameter HIFEX features a modular design

HIFEX configuration is similar to HST

HIFEX Concept: Jon Morse (ASU), with GD-SpectrumAstro

HIFEX in Delta II Separate Deploy Solar Extend Open Aperture Cost Envelope: $420M, incl. 10L Fairing From Launch Arrays and High Deployable Door Vehicle Gain Antenna Light Shield LV and 25% cost reserves HIFEX fits into a Delta II-10L fairing using a deployable light shade Baryonic Structure Probe P.I. Ken Sembach, Space Telescope Science Institute 3700 San Martin Dr., Baltimore, MD 21218 410-338-5051 [email protected] Key Science Objectives: • Detect and characterize the cosmic web of matter predicted by hydrodynamical simulations of the evolution of large scale cosmic structure – Approximately half of all baryonic matter at low-redshift is predicted to be in the form of a hot (T = 10^5-10^7 K) intergalactic medium – Most of this baryonic material has yet to be detected observationally – Baryons serve as "test particles" in the dark matter distribution since baryonic material and dark matter should be strongly coupled if the hydrodynamical simulations are correct – Detecting and mapping the baryons is critical to understanding the distribution of dark matter in the universe and the forces acting upon it (i.e., dark energy) • Hydrodynamical simulations predict that the hot cosmic web should be strongly influenced by star-formation feedback during galaxy formation – Galaxy formation/evolution is driven by the inflow/outflow of gas – Feedback disperses heavy elements into the intergalactic medium – Mapping the cosmic web in the vicinity of clusters and groups of galaxies will quantify the importance of feedback on the distribution of the hot gas in the cosmic web Baryonic Structure Probe: The Study • The Study – Refine expectations of observable phenomena through theoretical and computational cosmology to estimate absorption and emission line properties of the cosmic web – Flow the science requirements down into the primary mission/instrument requirements – Develop a mission concept and instrument design capable of quantifying the web properties at redshifts z < 1.5 • Why Ultraviolet Spectroscopy? – Despite a few detections of hot intergalactic gas with HST/STIS and FUSE, little is known about its properties owing to the extreme faintness of its signals and limited sensitivity of current observatories – The best tracers of the feedback and hot cosmic web gas occur at ultraviolet wavelengths (e.g., O VI, N V, C IV, Ly-alpha, and redshifted EUV lines of O IV-V, Ne VIII) – Ultraviolet spectroscopy provides both the high sensitivity and high spectral resolution necessary to study the feedback processes and physical properties of the hot gas in both absoprtion and emission – Deep galaxy imaging can be combined with the cosmic web imaging to reveal the relationship between the cosmic web and galaxies Baryonic Structure Probe: Instrumentation

• Ultraviolet (110-300 nm) spectroscopy to characterize the cosmic web of matter – High-resolution, high-sensitivity absorption-line spectroscopic capability to quantify the physical conditions of the hot gas (e.g., temperature, density, pressure, kinematics, composition) – Baseline sensitivity goal to exceed that of HST/COS – Moderate-resolution ultra-high-sensitivity hyperspectral imaging to map the hot intergalactic gas and reveal its relationship to galaxies – Represents a completely new avenue of exploration for NASA – No current or planned observatory has this capability – Instrument capabilities under consideration will be applicable to a broad range of other exciting science investigations (e.g., extrasolar planet studies, AGN/QSO and starburst outflows, gas-phase abundances in dwarf galaxies, stellar atmospheres and winds, etc.) Science Impact of Hubble Space Telescope Servicing Options

Science Mission Directorate Evaluation Team Interim Report 13 August 2004

23 Science Mission Directorate Evaluation Team (SMDET -- formerly OSSET) z Established by the former Office of Space Science to evaluate the impact to science return of the Hubble servicing options considered by the Analyses of Alternatives (AoA) team z Members include: Dr. Jennifer Wiseman, HST Program Scientist, NASA Headquarters Dr. Rob Kennicutt, Professor and Associate Head, Dept. of Astronomy, University of Arizona Dr. David Leckrone (ex officio), HST Project Scientist, NASA GSFC Dr. Malcolm Niedner, Deputy HST Project Scientist, NASA GSFC Dr. Hans-Walter Rix, Director, Max-Planck Institut fur Astronomie Dr. Peter Stockman, JWST Mission Head, Space Telescope Science Institute

24 Options and Assumptions z Options include: – deorbit-only of Hubble -- science operations cease in 2007-2008 due to loss of gyros – servicing of Hubble, including installation of gyros, batteries, and new science instruments -- HST operates with both new and most current instruments for ~5 years beyond servicing – rehost of science instruments on alternate platform(s) -- science operations of current HST instruments cease in 2007-2008; new rehost mission launched by 2010

25 Science Team Findings (1): Servicing of HST Including Science Instrument Installation z The Cosmic Origins Spectrograph (COS) and the Wide Field Camera 3 (WFC3) were designed in 1996-1997 for 2002 launch. z WFC3 and COS are fully optimized for Hubble, with order-of-magnitude gains over prior Hubble instruments. Instruments are designed for highest scientific gain when used in complementary mode with current HST instruments, especially the Advanced Camera for Surveys (ACS). z The STIS spectrograph that recently failed on Hubble was beyond its design life and was not slated for replacement or repair on any future servicing mission. Most (70%) current Hubble science is unaffected. COS would provide future spectrographic capability with very high sensitivity at important wavelength bands. STIS robotic repair is under preliminary consideration, due to the unique 2-D capabilities of STIS. z Current camera(s) and new instruments are predicted to function well for ~5 years beyond a 2009 servicing mission, based on failure rate analysis. Some cosmic-ray damage will occur over time, but this can be accommodated. z Important science programs require synergistic use of current and new science instruments: – ACS + WFC3 science is an important precursor to JWST – Combined instrument usage will allow studies of the evolution of galaxies, stellar populations, and the intergalactic medium over billions of years – Continued operations of current and new instruments will allow better understanding of dark energy and refined estimates of the cosmological equation of state through supernova observations

26 Science Team Findings (2): Rehosting Science Instruments z New HST science instruments were designed to work best in parallel with current HST instruments, especially the Advanced Camera for Surveys (ACS). Rehosting on a new platform would result in loss of some important science relying on synergy between science instruments, since the current HST would fail (and current instruments lost) before the new mission launched. z Timing is important: A full HST-quality platform may be problematic to fund and build in this decade, but rehosting after ~2010 would lose overlap and synergy with Chandra, Spitzer, and JWST pathfinder studies; some of WFC3 capabilities would become redundant to JWST. A rehost in this time frame would likely require recompetition and new mission design and selection to ensure highest scientific return for the investment. z The COS instrument is more amenable to a rehost on a smaller platform than is WFC3: some good COS science could be achieved on a smaller platform, while WFC3 requires a 2-meter class (I.e. Hubble class) platform for justifiable science return. z Bottom line: Best science return comes from fully serviced HST, providing synergistic use of both new and current instruments. Good, though reduced, science return would result from re-hosting the new instrument(s), especially if the timeframe is soon. Recompetition/re-evaluation might be warranted for a new mission.

27 Scorecard of the Major Capabilities: Fully serviced HST (no STIS) & COS-WFC3 Observatory

* T S Examples of Lost/Reduced Science H

d e 3 c i C v r F e W s - y t l S s Capability l O o u h F C e r Visible Imaging, High Resolution

Visible Imaging, Wide Field of View

Visible Long-Slit Spectroscopy

Visible Multi-Object Spectroscopy • For Dark Energy studies, ACS is the best “search engine” for UV Imaging, High Resolution detecting distant supernovae (left); WFC3/IR then observes

UV Imaging, Wide Field of View them for critical quantitative assessment. • For understanding Galaxy Formation w/ future UDFs (right), UV Long-Slit Spectroscopy ACS+WFC3 is a more efficient toolkit than WFC3 alone. UV Spectr., Med. Res. w/ optimized thruput

UV Spectroscopy, High Spectral Res. • ACS coverage of medium

UV Multi-Object Spectroscopy redshifts (med-Z) complements WFC3’s lo- and hi-Z coverage IR Imaging, High Resolution (**) in powerful grism surveys of IR Imaging, Wide Field of View distant galaxies.

IR Multi-Object Spectroscopy

Coronagraphy • Characterization of exoplanet-building zones & direct detection w/HST * Assumes STIS remains failed requires ACS/NICMOS coronagraphy. ** Long-term viability of NICMOS operations post-servicing is TBD 28 Scorecard of the Major Capabilities: Fully Serviced HST (no STIS) & Today’s HST

d e Examples of Lost Science ic T v S r e H s S ’ • With HST’s first-ever wide- y y ll * a u T d field UV imaging, WFC3 will Capability F S o H T go to the deep “fossil record” Visible Imaging, High Resolution of star populations to probe galaxy formation. Visible Imaging, Wide Field of View

Visible Long-Slit Spectroscopy

Visible Multi-Object Spectroscopy

UV Imaging, High Resolution

UV Imaging, Wide Field of View +

UV Long-Slit Spectroscopy

UV Spectr., Med. Res. w/ optimized thruput • COS will probe the chemical UV Spectroscopy, High Spectral Res. evolution of primordial intergalactic gas (left) and UV Multi-Object Spectroscopy nascent galaxy haloes (right) w/ IR Imaging, High Resolution (*) first far-UV optimized IR Imaging, Wide Field of View spectroscopy on HST.

IR Multi-Object Spectroscopy • WFC3 will provide HST’s first Coronagraphy wide-field IR capability for detection of high-redshift objects * long-term viability of NICMOS operations post-servicing is TBD and critical trailblazing for JWST. 29 Scorecard of the Major Capabilities: Fully serviced HST/STIS & COS-WFC3 Observatory

* t T s S o h H e r Examples of Lost Science d e 3 c i C v r F • Efficient hunting of super- e W s - y S massive black holes (STIS) ll Capability u O F C Visible Imaging, High Resolution

Visible Imaging, Wide Field of View

Visible Long-Slit Spectroscopy

Visible Multi-Object Spectroscopy UV Imaging, High Resolution • ACS coverage of medium UV Imaging, Wide Field of View redshifts (med-Z) complements WFC3’s lo- and hi-Z coverage UV Long-Slit Spectroscopy in powerful grism surveys of UV Spectr., Med. Res. w/ optimized thruput distant galaxies.

UV Spectroscopy, High Spectral Res.

UV Multi-Object Spectroscopy • Spectroscopy at visible wave- IR Imaging, High Resolution (**) lengths is vital for exoplanet atmosphere studies; studies in UV IR Imaging, Wide Field of View benefit from 2D spectroscopy (STIS) IR Multi-Object Spectroscopy

Coronagraphy • Characterization of exoplanet-building zones & direct detection w/HST * Assumes STIS repair is successful requires ACS/NICMOS coronagraphy. ** long-term viability of NICMOS operations post-servicing is TBD 30 Potential overlap with more Critical Mission capable missions Timescales UV/VIS/NIR Imaging WFC3 Re-hosted UV Spectroscopy COS Re-hosted UV-VIS-NIR (WFC3, COS, ACS,[STIS]) (full array of imaging & spectroscopic capability) Hubble after Full Servicing UV-VIS-NIR (Current Instr.) Hubble pre-servicing

X-ray imaging and spectroscopy Chandra MIR & FIR Imaging, MIR Spectroscopy Spitzer

SIM Visible Precision Astrometry (Large Planet Finder) JWST NIR-MIR imaging and spectroscopy TPF-C VIS Coronagraphy/imaging/UV spectr.? JDEM? Widefield VIS/NIR Imaging

Unique Hubble Science; Spitzer, Chandra, SIM followup; Precursor to/overlap with JWST

2004 2005 2006 2007 2008 2009 2010 2011 2012 2013 2014 2015 2016 2017 2018

31 Rehosting New HST Science Instruments: A Few Issues to Consider z ~”Pros”: – Less Technological Risk? – Cost control? – New telescope, new platform, updated technology – Could recover much of Hubble SM4 science goals and more – Chance for innovation, mission/instrument updates and science enhancement z ~”Cons”: – Current HST camera(s) fail with gyros in 2007-2008, before launch of new instruments – Lose synergy of new and current instruments; lose some science return as compared to fully-serviced Hubble – Origins Probes (as one possible vehicle for rehosting) do not yet exist in budget -- (but interesting concept studies could justify the need) – Must still launch autonomous mission to HST to install deorbit module z Scheduling (for science) and cost issues will affect both servicing and rehosting options. New mission may warrant competition to ensure maximum science return for the investment (and may result in a different mission than simple rehost)