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non-redundant masking on JWST TFI

non-redundant masking on JWST TFI. Anand Sivaramakrishnan STScI. JWST TFI Science Team (NRM lead) Stony Brook Physics & Astronomy JAM team lead (JWST Aperture masking, GPI, P1640). JAM Team JWST Aperture Masking team. Anand Sivaramakrishnan (Lead) Peter Tuthill, Mike Ireland (U Sydney)

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non-redundant masking on JWST TFI

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

  2. JAM TeamJWST Aperture Masking team 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 Racine 1999 Fitzgerald & Graham 2006 10ms 2um Fitzgerald & Graham 2006 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,...

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

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

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

  7. NRM cf. Conventional AO (ground)

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

  9. JWST TFI NRM Taurus proto-planets

  10. FGS-TFI g7s6 mask50mm OD mask, 39mm OD pupil, SS part Simulated PSF PSF’s power spectrum g7s6sc Blocking off 11 of 18 PM segments leads to otherwise inaccessible science with JWST

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

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

  13. 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

  14. 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)

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

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

  17. 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 More study part g7s6sc QUESTIONS: How good can the contrast really get,??? Develop credible science for Wyoming 2011 Simulated PSF

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