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) 1

JAM Team

JWST 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) 2

High contrast is difficult from the ground

Racine 1999 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,...

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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 4

Apr 1998

WR 104 Discovery Images

NRM on Keck – model fitting HI RES FROM GROUND Jun 1998 Sep 1998

50 mas (75 AU)

Tuthill et al, Nature 1999 5

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

NRM cf. Conventional AO (ground)

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Signal is not the problem Throw away light but get the science!

 Rayleigh = Criterion

1.22

 /D Michelson Criterion  =

0.5

 /D 8

Taurus proto planets

JWST TFI NRM

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

Closure Phase

Stable JWST closure amplitudes yield true imaging, not just model-fitting

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

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

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)

Undergrad NRM data – space-like Parmentier & Sivaramakrishnan

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

g7s6sc

Bright stars possible (M >= 2 ) Good target acquisition cures calibration troubles Robust to PM actuator freezing Mask is also a wavefront sensor Robust backup for coarse phasing QUESTIONS: How good can the contrast really get,???

Develop credible science for Wyoming 2011

Simulated PSF 23