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High Contrast Imaging from Space and the WFIRST Coronagraph Instrument

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High Contrast Imaging from Space and the WFIRST Coronagraph Instrument High Contrast Imaging from Space and the WFIRST Coronagraph Instrument N. Jeremy Kasdin Eugene Higgins Prof. of Mechanical & Aerospace Eng. Princeton University 20 May 2018 1 Acknowledgments I am indebted to my direct imaging and WFIRST colleagues for their help and contributions to this talk: Vanessa Bailey, Bruce Macintosh, Maggie Turnbull, Peg Frerking, Feng Zhao, Ilya Poberezhkiy, Rick Demers, Eric Cady, A J Riggs, BijanNemati, Bertrand Menneson, John Trauger, John Krist, Fang Shi, and the entire CGI team. Neil Zimmerman, Tyler Groff, Missy Vess, and the team at Goddard Space Flight Center. Laurent Pueyo, Remi Soummer, and Chris Stark at STScI. Gary Ruane (Caltech), Dmitry Savransky(Cornell), Aki Roberge (GSFC), Leslie Rogers (Chicago), Courtney Dressing (Berkeley). Sara Seager, Andrew Grey, Andrew Romero-Wolf, Doug Lisman, Stuart Shaklan, and the StarshadeRendezvous team. My students and postdocs: Christian Delcroix, Jessica Gersh-Range, Anthony Harness, Leonel Palacios Moreno, Mia Hu, Leonid Pogorelyuki, He Sun. 2 3 CGI in Context Giant Planet Imaging Photometry Narrow-band Spectroscopy of Self-luminous & RV Planets New Planet Discovery ExozodiacalDisk Imaging Visible light characterization of Debris Disks 6 WFIRST after WIETR • The Coronagraph Instrument is a technology demonstration only • Requirements established using standard engineering practice • Reduction in modes and science center role • If successful, ”Participating Science Program” following tech demo • Design to support possible starshade (pending Decadal recommendation) Notional CGI Program • 3 months of technology demonstration observing in first 1.5 years of WFIRST mission • If meet success criteria, 1 year Participating Science Program • If successful, follow-on 2.5 year science program 7 Realizing a Coronagraph Mission Science/Technology Objectives Instrument Design Reference Capability Mission Coronagraph Image Design Processing Wavefront Control Operations & & Optical System Measurement Observatory Jitter and Drift WFIRST as a Pathfinder L2.5 Planet-Star Flux Ratio [ppb] Mission Simulation Full SystemsPlanet Photon Shot Noise [ppb] Req. 7.0 L1 Requirement L1 Telescope Req. 0.23 CBE 6.0 L2.5 SNR L2 Science Requirement Diameter [m] CBE 0.21 L3 / L4 Engr Requirement Value 2.36 Value 10 1s Noise Eq. Control Loop Zodi Photon L2.5 Zodi L2.5 Star Shot Noise [ppb] Flux Ratio [ppb] Cont Stability Observatory Interface & Yield EngineeringBrightness [mag] &Backg round w/Post Proc. [ppb] Req. 0.12 Req. 0.70 Value Solar Req. 0.49 Value 5 CBE 0.11 CBE 0.60 CBE 0.43 Post Processing L2.5 Filter Bands Gain Center Photometry Random Noise Systematic Noise Value 2 [nm] 770 L3 Cont Stability Noise [ppb] w/2 hr Chop [ppb] Error BudgetingWidth 18% Req. 0.50 Science/Technology Req. 0.98 With Pixel-by-Pixel L2.5 Resolving CBE 0.41 CBE 0.87 Power Subtraction Value 50 Stellar Leakage L2.5 Planet Int. Shot Noise [ppb] L3 Raw Contrast Time [hrs] Req. 0.14 [ppb] Value 240 CBE 0.10 Req. 3 CGI Internal Drift Suppressed Obs Suppressed Obs Unsuppressed Suppressed Obs CBE 2.1 [ppb] Focus Drift [ppb] WFE Drift [ppb] Drift/Jitter [ppb] LOS Jitter [ppb] Objectives Req. 0.8 Req. 0.20 Req. 0.20 Req. 0.40 Req. 0.30 ppb/count Detector/Elec CBE 0.75 CBE 0.02 CBE 0.02 CBE 0.35 CBE 0.25 Conversion Noise [ppb] Coherent Dominated by DM drifts Req. 0.0047 Req. 0.41 Contrast [ppb] CBE 0.0031 CBE 0.32 Req. 2 Suppressed Obs Suppressed Obs Suppressed Obs CBE 1.5 Focus Drift [nm] WFE Drift [nm] LOS Jitter [mas] Req. 0.07 Req. 0.07 Req. 0.50 L3 Planet Sig. L4 Dark Current CBE 0.02 CBE 0.02 CBE 0.45 Throughput [e/pix/s] HOWFS Control Req. 1.2% Req. 2.5*10-4 using DMs CBE 1.4% CBE 2.2*10-4 Coronagraph Calibration Errors L4 CIC Noise Raw Contrast w/o Design Contrast Focus Control WFE Control Pointing L4 QE [e/pix/fr] Control [ppb] [ppb] using using Control using -2 Value 75% Req. 1.5*10 Req. N/A Req. 1.2 LOWFS+FCM LOWFS+DMs LOWFS+FSM -2 CBE 1.0*10 CBE 1000 CBE 1 Telescope Coronagraph Obs Focus Drift Obs WFE Drift Obs Uncorrected Obs LOS Jitter L4 Pixel/PSF L4 Read Noise Surface Error Fab/Align Errors Instrument[nm] [nm] Disturbances [mas] Design Reference [e/pix/fr] Value 9 Req. 77 nm Req. 10 nm Req. 2 nm Req. 12 mas Req. 1.5*10-6 WFE jitter, beamwalk, CBE 77 nm CBE 0.2 nm CBE 0.05 nm pupil shear CBE 5 mas CBE 1*10-6 Due to thCapabilityermal drift Due to thermal drift Due to RWAs/ACS Mission High Contrast Coronagraph Image Processing Stable Space Elements at Unprecedented Telescope & Coronagraph Contrast LevelsImage Observatory Design First Use of Processing Deformable Mirrors in Space Wavefront Control Operations & & Optical System Measurement Observatory Autonomous Jitter and Precision Ultra-low noise Wavefront photon counting Drift Sensing & Control Visible Detectors CGI Will . Demonstrate in space critical coronagraph technology and state of the art wavefront control. Advance the state of the art in direct imaging and spectra toward future missions. Characterize the in-flight interactions between coronagraph and observatory. Prototype systems engineering for space coronagraph. Validate end-to-end data analysis for space coronagraph. Potentially perform important science in spectral retrieval, direct imaging of RV planets, blind searches, and zodi and debris disk characterization. Results will inform requirements (particularly stability) and design of future missions such as HabEx and LUVOIR. 10 Realizing a Coronagraph Mission L2.5 Planet-Star Flux Ratio [ppb] Planet Photon Shot Noise [ppb] Req. 7.0 L1 Requirement Req. 0.23 CBE 6.0 L1 Telescope L2 Science Requirement FullDia meSystemster [m] L2.5 SNR CBE 0.21 L3 / L4 Engr Requirement Value 2.36 Value 10 1s Noise Eq. Control Loop Zodi Photon L2.5 Zodi L2.5 Star Shot Noise [ppb] Flux Ratio [ppb] Cont Stability Observatory Interface Brightness [mag] Background w/Post Proc. [ppb] Req. 0.12 Req. 0.70 Value Solar Req. 0.49 Value 5 CBE 0.11 CBE 0.60 CBE 0.43 Post Processing EngineeringL2.5 Filter Bands & Gain Center Photometry Random Noise Systematic Noise Value 2 [nm] 770 L3 Cont Stability Noise [ppb] w/2 hr Chop [ppb] Width 18% Req. 0.50 Science/Technology Req. 0.98 With Pixel-by-Pixel L2.5 Resolving CBE 0.41 CBE 0.87 Power Subtraction ErrorVa lue Budgeting50 Stellar Leakage L2.5 Planet Int. Shot Noise [ppb] L3 Raw Contrast Time [hrs] Req. 0.14 [ppb] Value 240 CBE 0.10 Req. 3 CGI Internal Drift Suppressed Obs Suppressed Obs Unsuppressed Suppressed Obs CBE 2.1 [ppb] Focus Drift [ppb] WFE Drift [ppb] Drift/Jitter [ppb] LOS Jitter [ppb] Objectives Req. 0.8 Req. 0.20 Req. 0.20 Req. 0.40 Req. 0.30 ppb/count Detector/Elec CBE 0.75 CBE 0.02 CBE 0.02 CBE 0.35 CBE 0.25 Conversion Noise [ppb] Coherent Dominated by DM drifts Req. 0.0047 Req. 0.41 Contrast [ppb] CBE 0.0031 CBE 0.32 Req. 2 Suppressed Obs Suppressed Obs Suppressed Obs CBE 1.5 Focus Drift [nm] WFE Drift [nm] LOS Jitter [mas] Req. 0.07 Req. 0.07 Req. 0.50 L3 Planet Sig. L4 Dark Current CBE 0.02 CBE 0.02 CBE 0.45 Throughput [e/pix/s] HOWFS Control Req. 1.2% Req. 2.5*10-4 using DMs CBE 1.4% CBE 2.2*10-4 Coronagraph Calibration Errors L4 CIC Noise Raw Contrast w/o Design Contrast Focus Control WFE Control Pointing L4 QE [e/pix/fr] Control [ppb] [ppb] using using Control using -2 Value 75% Req. 1.5*10 Req. N/A Req. 1.2 LOWFS+FCM LOWFS+DMs LOWFS+FSM -2 CBE 1.0*10 CBE 1000 CBE 1 Telescope Coronagraph Obs Focus Drift Obs WFE Drift Obs Uncorrected Obs LOS Jitter L4 Pixel/PSF L4 Read Noise Surface Error Fab/Align Errors Instrument[nm] [nm] Disturbances [mas] Design Reference [e/pix/fr] Value 9 Req. 77 nm Req. 10 nm Req. 2 nm Req. 12 mas Req. 1.5*10-6 WFE jitter, beamwalk, CBE 77 nm CBE 0.2 nm CBE 0.05 nm pupil shear CBE 5 mas CBE 1*10-6 Due to thCapabilityermal drift Due to thermal drift Due to RWAs/ACS Mission Coronagraph Image Design Processing Wavefront Control Operations & & Optical System Measurement Observatory Jitter and Drift CGI Technology Objectives Demonstrate Coronagraphy with Active Wavefront Control in space Advance Engineering & Readiness of Coronagraph Elements Development and Demonstration of Advanced Coronagraph Algorithms Integrated Observatory Performance Characterization Demonstration of Advanced High-Contrast Data Processing In short, WFIRST will validate our models and assumptions for the entire system, including data processing, in a space environment. 12 WFIRST Instrument Capability CGI Level 2 Requirements • High-Contrast Direct Imaging • High-Contrast Imaging Spectroscopy • Extended Source Imaging with Large FOV • Polarization Measurements of Disks • Exoplanet Astrometric Accuracy • Wavefront Sensing and Control Telemetry • Telescope Polarization • Measure Pointing Jitter • Measure Slow Wavefront Aberrations 15 Example Level 2 Requirements 1) High-Contrast Direct Imaging WFIRST CGI shall be able to measure the brightness of an astrophysical point source to an SNR of 10 or greater within 10 hours of integration time on the target in CGI Filter Band 1 for an object with a source-to-star flux ratio as faint as 1e-7 at separations from 0.16 arcsec to 0.21 arcsec, 5e-8 at separations from 0.21 arcsec to 0.4 arcsec, and 1e-7 at separations from 0.4 arcsec to 0.45 arcsec. 2) High-Contrast Imaging Spectroscopy WFIRST CGI shall be able to measure spectra of an astrophysical point source with R = 50 or greater spectral resolution with a wavelength accuracy of 5 nm or smaller (TBR) to an SNR of 10 within 100 hours of integration time on the target in CGI Filter Band 3 for an object with a source-to-star flux ratio as faint as 1e-7 at separations from 0.21 arcsec to 0.27 arscec, 5e-8 at separations from 0.27 arcsec to 0.53 arcsec, and 1e-7 at separations from 0.53 arcsec to 0.60 arcsec.
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