1. non-redundant masking on JWST TFI Anand Sivaramakrishnan STScI 1 JWST TFI Science Team (NRM lead) Stony Brook Physics & Astronomy JAM team lead (JWST Aperture masking, GPI, P1640)

2. JAM Team JWST Aperture Masking team 2 Anand Sivaramakrishnan (Lead) Peter Tuthill, Mike Ireland (U Sydney) James Lloyd (Cornell) Frantz Martinache (Subaru) Rene Doyon (TFI) David Lafreniere (TFI) Remi Soummer (JWST WFS&C) Chas Beichman (NIRCam) Barry McKernan, Saavik Ford (AGNs, QSOs GBHCs) Marshall Perrin (STScI - IFU on GPI) Laurent Pueyo (NRM on GPI, Sagan Felolw) Michael McElwain (IFU on Keck, NSF Fellow) Sasha Hinkley (IFU, Palomar Hale, Sagan Fellow)

3. High contrast is difficult from the ground 3 Racine et al. PASP 1999 Sivaramakrishnan et al ApJL 2002, Perrin et al. ApJ 2003, Aime & Soummer ApJ 2004, Fitzgerald & Graham 2006, Soummer et al. 2007,... Racine 1999 Fitzgerald & Graham 2006 10ms 2um Fitzgerald & Graham 2006

4. Optimal data analysis 4 Bayesian approach to combining all data Marois et al. 2008 Science “ADI” Lafreniere et al 2007 refined methods - LOCI Fitzgerald & Graham 2006 10ms 2um

5. WR 104 Discovery Images NRM on Keck – model fitting HI RES FROM GROUND Apr 1998Jun 1998Sep 1998 50 mas (75 AU) Tuthill et al, Nature 1999 5

6. HIGH ANGULAR RESOLUTION IS DIFFICULT FROM SPACE 6 3 Mjup 12” separationKalas et al. Science 2008 Roll subtraction

7. NRM cf. Conventional AO (ground) 7

8. Signal is not the problem Throw away light but get the science! Rayleigh Criterion  = 1.22 /D Michelson Criterion  = 0.5 /D 8

9. JWST TFI NRM 9 Taurus proto- planets Taurus proto- planets

10. 10

11. Fourier Components

13. PSF’s power spectrum FGS-TFI g7s6 mask 50mm OD mask, 39mm OD pupil, SS Simulated PSF g7s6sc part 13 Blocking off 11 of 18 PM segments leads to otherwise inaccessible science with JWST

14. Closure Phase 14 Stable JWST closure amplitudes yield true imaging, not just model-fitting

15. Closure Phase                   measured phase = intrinsic + instrumental 9 hole mask 36 baselines 84 closure triangles (28 independent) Signal extraction cf PSF suppression 15

16. TFI G7S6 mask 50mm OD mask TFI-PM pupil mapping, titanium part

17. Predicted JWST FGS-TFI survey part 17 DETECTION PROBABILITIES Companion mass <=10 M J 1 hour exposure 10 mag contrast floor 4.4 micron JWST coronagraph & ExAOC survey simulations: Beichman, Krist, Trauger, Greene, Oppenheimer, Sivaramakrishnan, Doyon, Bocaletti, Barman, Rieke PASP 2010 0.3 0.7 0.5 0.2 0.1 0.4 0.5 0 0.6 0.1 0.8 0.7 0.6 0.5 Log 10 (M/M J ) Semi-major axis (AU))

18. Predicted JWST FGS-TFI survey results 18 JWST coronagraph & ExAOC survey simulations: Beichman, Krist, Trauger, Greene, Oppenheimer, Sivaramakrishnan, Doyon, Bocaletti, Barman, Rieke PASP 2010

19. Undergrad NRM at Stony Brook Parmentier & Sivaramakrishnan Inexpensive CCD camera, lens, laser-cut SS mask SB NRM Testbed Mark II – mirror instead of lens 2010 NSF REU Alexandra Greenbaum to make a ‘star+planet’ for the testbed

20. Undergrad NRM data – space-like Parmentier & Sivaramakrishnan FT of ‘interferogram’: absolute value and phase GOAL: Develop estimates of contrast of faint point source companions that JWST can achieve in IR to see protoplanets in Taurus, and other places planets are being formed. Stable images, data reduction algorithm development, help plan JWST science & observing proposals Future extragalactic space-based observations of disks and dusty tori around massive black holes at centers of external galaxies – JWST (& ATLAST)

21. Undergrad NRM data – space-like Parmentier & Sivaramakrishnan

22. Palomar IFU NRM data Sivaramakrishnan Zimmerman Tuthill Lloyd Ireland Oppenheimer Soummer Simon Calibrator Target First IFU NRM data P1640 J+H IFU on Palomar

23. More study Simulated PSF g7s6sc part ISSUES for JWST FGS-TFI NRM Dither for CRs & bad pixels) Bright stars possible (M >= 2 ) Good target acquisition cures calibration troubles Intrapixel sensitivity, persistence, flat field accuracy studies under waySsimulated L2 CR library (Robberto), full data reduction pipeline Robust to PM actuator freezing Mask is also a wavefront sensor Robust backup for coarse phasing 23 QUESTIONS: How good can the contrast really get,??? Develop credible science for Wyoming 2011