non-redundant masking on JWST TFI

Anand SivaramakrishnanSTScI

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JWST TFI Science Team (NRM lead)

Stony Brook Physics & Astronomy

JAM team lead (JWST Aperture masking, GPI, P1640)

JAM TeamJWST Aperture Masking team

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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)

High contrast is difficult from the ground

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Racine et al. PASP 1999Sivaramakrishnan 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 2umFitzgerald & Graham 2006

Optimal data analysis

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Bayesian approach to combining all data

Marois et al. 2008 Science “ADI”Lafreniere et al 2007 refined methods

- LOCI

Fitzgerald & Graham 2006 10ms 2um

WR 104 Discovery ImagesNRM on Keck – model fitting

HI RES FROM GROUND

Apr 1998 Jun 1998 Sep 1998

50 mas (75 AU)Tuthill et al, Nature 1999

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HIGH ANGULAR RESOLUTION IS DIFFICULT FROM SPACE

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3 Mjup 12” separation Kalas et al. Science 2008

Roll subtraction

NRM cf. Conventional AO (ground)

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Signal is not the problemThrow away light but get the science!

RayleighCriterion

= 1.22 /D

MichelsonCriterion = 0.5 /D

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JWST TFI NRM

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Taurusproto-planets

Taurusproto-planets

PSF’s power spectrum

FGS-TFI g7s6 mask50mm OD mask, 39mm OD pupil, SS

Simulated PSF

g7s6sc

part

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Blocking off 11 of 18 PM segments leads to otherwise inaccessible science with JWST

Closure Phase

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

Predicted JWST FGS-TFI survey results

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

Undergrad NRM at Stony BrookParmentier & 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-likeParmentier & 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-likeParmentier & Sivaramakrishnan

Palomar IFU NRM dataSivaramakrishnan Zimmerman Tuthill Lloyd Ireland Oppenheimer Soummer Simon

Calibrator Target

First IFU NRM dataP1640 J+H IFU on Palomar

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 troublesIntrapixel 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

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QUESTIONS:

How good can the contrast really get,???

Develop credible science for Wyoming 2011