1. WFIRST SDT and Project Studies Princeton Workshop September 4, 2012 Neil Gehrels WFIRST Study Scientist

2. WFIRST Summary  WFIRST is the highest ranked large space mission in NWNH, and plans to: - complete the statistical census of Galactic planetary systems using microlensing - determine the nature of the dark energy that is driving the current accelerating expansion of the universe - survey the NIR sky for the community - conduct a guest observer program  Measurements all require wide-field NIR observatory - NIR sky surveys for BAO and weak lensing and - NIR monitoring for SNe and exoplanets  Space-qualified large format HgCdTe detectors are US developed technology and flight ready H2RG EDU FPA H4RG Mosaic Plate

3. WFIRST Dark Energy Bright H  line for BAO Kocevsk+ '11 Galaxy Shapes in IR for WL Systematics Control for SNe Atek+ '12 Kowalski+ '08

4. Figures from B. MacIntosh of the ExoPlanet Task Force WFIRST Kepler WFIRST Exoplanets

5. WFIRST provides a factor of 100 improvement in IR surveys WFIRST NIR Redshift Surveys NIR Imaging Surveys WFIRST WFIRST-SN WFIRST NIR Surveys

6. Key Conclusions of the SDT WFIRST created by NWNH EOS panel from JDEM (dark energy), MPF (exoplanet microlensing) and NIRSS (IR surveys) (JDEM Omega configuration, 1.5m telescope) Science Definition Team (SDT) formed November 2010 Co-Chairs Jim Green & Paul Schechter SDT interim report June 2011 (arXiv 1108.1374) (IDRM – off-axis telescope version of JDEM-Omega) Discussion of using NRO telescope with 2.4m mirror SDT final report August 2012 (DRM1 & DRM2 – off-axis telescopes, single instrument) WFIRST Happenings

7. The SDT Charter “The SDT is to provide science requirements, investigation approaches, key mission parameters, and any other scientific studies needed to support the definition of an optimized space mission concept satisfying the goals of the WFIRST mission as outlined by the Astro2010 Decadal Survey.” 2 nd Year - Complete detailed study of primary configuration - Create a second cheaper option that is complementary to Euclid, LSST and JWST - Augment SDT with 5 new members SDT original Charter

8. 8 Paul Schechter, MIT Co-Chair James Green, U. Colorado/CASA Co-Chair Rachel Bean, Cornell University Charles Baltay, Yale David Bennett, Univ. of Notre Dame Robert Brown, STScI Christopher Conselice, Univ. of Nottingham Megan Donahue, Michigan State Univ. Scott Gaudi, Ohio State Univ. Tod Lauer, NOAO Bob Nichol, Univ. of Portsmouth Saul Perlmutter, UC Berkeley / LBNL Bernard Rauscher, GSFC Jason Rhodes, JPL Thomas Roellig, Ames Daniel Stern, JPL Takahashi Sumi, Nagoya Univ. Angelle Tanner, Mississippi State Univ. Yun Wang, Univ. of Oklahoma Edward Wright, UCLA Neil Gehrels, GSFC Ex-Officio Wes Traub, JPL Ex-Officio Rita Sambruna, NASA HQ Ex-Officio WFIRST Science Definition Team Xiaohui Fan, U. Arizona Chris Hirata, Caltech Jason Kalirai, STScI Nikhil Padmanabhan, Yale David Weinberg, Ohio State U. New Members Jan. 2012

9. H4RG-10 Mosaic Plate with WFIRST Science Definition Team, NASA HQ, and Project Office Team February 3, 2012

10. Requirements Flowdown Substantiation that WFIRST can achieve NWNH science Traces science requirements from top level objectives

11. Over 80 Concepts Developed

12. TMA Telescope Three Mirror Anastigmatic Unobscured (unocculted) design Three powered (curved) mirrors 9 degrees of freedom from mirrors (curvature, conic constant, position for each) Allows control of 9 parameters (focal length, magnification of each mirror, astigmatism, coma, spherical aberration, field curvature) Wider field than Ritchey-Chrétien Better image quality than Schmidt

13. NIR Detectors H2RG detectors - H >> HAWAII = HgCdTe Astron. Wide Area IR Imager - 2 >> 2048 x 2048 pixels - R >> reference rows & columns to correct bias fluctuations - G >> guiding function, selectable window for guide star Space H1Rs used on HST. Space H2RGs developed for JWST Goals of WFIRST program - Larger mosaics than JWST - Silicon carbide support structure - H4RG development Sensor Chip Assembly GSFC SI Carbide mount

14. Design Reference Missions  IDRM  1.3 meter off-axis telescope  3-channel payload  5 year mission  Atlas V Launch Vehicle  DRM1  1.3 meter off-axis telescope  Single channel payload  5 year mission  Atlas V Launch Vehicle  DRM2  1.1 meter off-axis telescope  Single channel payload  3 year mission  Falcon 9 Launch Vehicle

15.  IDRM  1.3 meter off-axis telescope  3-channel payload  5 year mission  Atlas V Launch Vehicle  DRM1  1.3 meter off-axis telescope  Single channel payload  5 year mission  Atlas V Launch Vehicle  DRM2  1.1 meter off-axis telescope  Single channel payload  3 year mission  Falcon 9 Launch Vehicle Design Reference Missions

16. WFIRST DRM1 Payload Optics Block Diagram ~205K Unobstructed, Focal Telescope: 9x4 FPA; 2kx2k.18 μm SCAs; 150 Mpix; 100K; 0.6-2.4µm bandpass; 0.375 deg 2 Active Area 180 mas/pix f/15.9 0.30° x 0.14° FOV Extent Science Channel SN Resolving power 75/2pixel; GRS Dispersion D  = 160-240 arcsec 8 positions (6 filters, open, blank) GRS = Galaxy Redshift Survey FGS = Fine Guidance Sensor: Outrigger FGS used during imaging, Auxiliary FGS used during spectroscopy SN = Type1a Supernovae Filter Wheel “Outrigger FGS” SCAs (4, in pink) shown in notional positions on Focal Plane Cold Pupil Mask TM Instrument Telescope 1x2 FPA; 2kx2k, 18μm pixel size SCAs; ~8 Mpix; <120K; 0.6-2.0µ bandpass; 0.04 deg 2 Active Area 250 mas/pix; f/11.4 180 mas/pix Auxiliary FGS Prism Wheel 6 positions (3 prism assemblies, {SN, 2 GRS}, 3 open) PM and SM followed by Tertiary Mirror (TM) and fold flats that feed the science channel and an auxiliary FGS

17. DRM1 Field of view & focal plane layout WFIRST-JWST Focal plane Comparison Area is 145x larger than NIRCAM (0.375 vs. 0.00259 sq degrees Focal plane has 5x more pixels than NIRCAM short wave cameras (150 vs 33 Mpix) H2RG detectors

18. CANDELS fields on DRM1 focal plane from J. Kruk

19. DRM2 Field of view & focal plane layout WFIRST-JWST Focal plane Comparison Area is 226x larger than NIRCAM (0.585 sq vs 0.00259 degrees) Focal plane has 7x more pixels than NIRCAM short wave cameras (235 vs 33 Mpix) H4RG detectors

20. WFIRST DRM1 Observatory Layout & Ray Trace Solar array/sunshield Spacecraft FPA radiator SM PM TM F1 F2 GRS prism

21. WFIRST DRM2 Observatory Layout Sun at bottom WMAP-like progression from warm solar array (300K) to cold focal plane (100K) from bottom to top Overall dry mass 500+ kg less than DRM1 Solar array(blue) & sunshade, deployed Spacecraft Telescope Radiator Instrument FPA Solar array(blue) & sunshade Launch configuration

22. Survey Strategies from C. Hirata exoplanets SNe HL Survey WL & BAO GPS GO Program Example DRM1 Observing Plan Sun angle (deg) Time (months)

23. DRM1 Performance Exoplanets: >2000 bound exoplanets of 0.1 – 10,000 Earth mass (M Earth ) >30 free floating planets of 1 M Earth  200 terrestrial planets* (0.3 – 3 M Earth ) Accelerating Universe: WL and BAO surveys of >1400 deg 2 per year to a Hα line spectroscopy limit of 1 × 10 −16 ergs/cm 2 /sec and imaging limit of AB=26. SNe-Ia: 2 tiered survey covering 6 deg 2 and 2 deg 2 with a five day cadence over 1.8 years yielding ~100 SNe per ∆z = 0.1 bin NIR Surveys:  2000 quasars at redshift z > 7 and  35 quasars at redshift > 10 Broad-band NIR spectral energy distributions of  3 X 10 9 galaxies Map of Galaxy structure using red giant clump stars as tracers

24. WFIRST DRM1 Schedule Estimate Funded Schedule Reserve 79 month development schedule Start of Phase B FY 15 Launch Readiness Date Sept ember 2020 7 month schedule reserve

25. The WFIRST Independent Cost Estimate by Astro2010 (based on JDEM configuration) was $1.6B The Project Office cost estimates indicate that DRM1 would have a full cost less that $1.6B due to single instrument channel and reduced mass. The Independent Cost Estimate for DRM2 is $1.1B Cost Estimates

26. The SDT and Project have completed the action of developing two compelling mission concepts. DRM1: Fully responsive to the objectives of NWNH at reduced cost DRM2: Capable low-cost near-infrared survey opportunity. The limited 3 year life precludes full compliance with NWNH goals. Path forward: Study WFIRST mission utilizing NRO telescope with new SDT Develop 4kx4k IR detectors for wide-field applications Conclusions