non-redundant masking on JWST TFI

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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)
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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
WFSC) 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)
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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,...
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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
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WR 104 Discovery ImagesNRM on Keck model
fittingHI RES FROM GROUND
Apr 1998
Jun 1998
Sep 1998
Tuthill et al, Nature 1999
50 mas (75 AU)
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HIGH ANGULAR RESOLUTION IS DIFFICULT FROM SPACE

• Roll subtraction

3 Mjup 12 separation
Kalas et al. Science 2008
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NRM cf. Conventional AO (ground)
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Signal is not the problemThrow away light but
get the science!
Rayleigh Criterion ?? 1.22 ?/D
Michelson Criterion ?? 0.5 ?/D
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JWST TFI NRM
Taurus proto-planets
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(No Transcript)
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Fourier Components
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Fourier Components
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FGS-TFI g7s6 mask50mm OD mask, 39mm OD pupil,
SS
part
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Closure Phase
Stable JWST closure amplitudes yield true
imaging, not just model-fitting
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Closure Phase

• 9 hole mask
• 36 baselines
• 84 closure triangles
• (28 independent)

?????? ??? ???????????????????????? ?????? ???
???????????????????????? ?????? ???
???????????????????????? measured phase
intrinsic instrumental
Signal extraction cf PSF suppression
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TFI G7S6 mask50mm OD mask TFI-PM pupil mapping,
titanium
part
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Predicted JWST FGS-TFI survey
Semi-major axis (AU))
part
DETECTION PROBABILITIES Companion mass lt10 MJ
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
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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
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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
starplanet for the testbed
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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)
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Undergrad NRM data space-like
Parmentier Sivaramakrishnan
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Palomar IFU NRM data
Sivaramakrishnan Zimmerman Tuthill Lloyd Ireland
Oppenheimer Soummer Simon
Calibrator Target
First IFU NRM data P1640 JH IFU on Palomar
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More study
ISSUES for JWST FGS-TFI NRM Dither for CRs bad
pixels) Bright stars possible (M gt 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
part
g7s6sc
QUESTIONS How good can the contrast really
get,??? Develop credible science for Wyoming 2011
Simulated PSF