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
Signal is not the problemThrow away light but get the science!
RayleighCriterion
= 1.22 /D
MichelsonCriterion = 0.5 /D
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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
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)
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