introducing jwst’s niriss : the n ear i nfra r ed i mager & s litless s pectrograph
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JWST FGS. Introducing JWST’s NIRISS : The N ear I nfra R ed I mager & S litless S pectrograph. Alex Fullerton STScI / HIA. TIPS/JIM 2011 September 15. The Tunable Filter Imager (TFI). TFI Lessons Learned. July 20, 2011: Wave good-bye to TFI. Say hello to NIRISS. - PowerPoint PPT PresentationTRANSCRIPT
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Introducing JWST’s NIRISS:The Near InfraRed Imager & Slitless Spectrograph
TIPS/JIM2011 September 15
Alex FullertonSTScI / HIA
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TIPS/JIM2011 September 15
The Tunable Filter Imager (TFI)
TIPS / JIM Presenter Title
2004 May 20 Nelan JWST FGS SRR (April 7, 2004)
2005 March 17 Fullerton Overview of Calibration Activities for the JWST FGS-TFI
2005 May 19 Fullerton FGS Tunable Filter Imager: Updates from PDR
2006 June 15 Fullerton “Phase C” Design of the JWST/FGS Tunable Filter Imager
2008 Sept. 18 Fullerton The Tunable Filter Imager Passes its CDR[s]
2010 Sept. 16 Sivaramakrishnan The Non-Redundant Mask on JWST
2010 Nov. 18 Sivaramakrishnan Non-Redundant Tilts (NRT): A Fallback Coarse Phasing Method for JWST Using TFI
2011 March 17 Chayer JWST FGS & TFI Cryovac Risk Mitigation Tests
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TIPS/JIM2011 September 15
TFI Lessons Learned
#1: Cryogenic etalons are tricky.
July 20, 2011:
Wave good-bye to TFI.
Say hello to NIRISS.
Near InfraRed Imager & Slitless Spectrograph
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TIPS/JIM2011 September 15
Design Considerations for NIRISS
Maintain capability to address core TFI Science• “First Light”• Exoplanets
Minimize technical risk • Schedule is a (big) issue• Cost is a (big) issue
Simplify operations
Emphasis of nascent GTO Programs
“Scope” is the only adjustable parameter available to CSA Program Management.
Helps the S&OC (i.e., us) a bit.
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TIPS/JIM2011 September 15
Observing Modes
TFI NIRISSNarrow-Band Imaging
R~100; tunable 1.5 – 2.6 & 3.0 – 5.0 micronsWide-Field Slitless Spectroscopy
R~ 150; 1.0 – 2.5 microns
Coronagraphic ImagingR~100; tunable 3.0 – 5.0 microns XXXXXXXXXXXXXXXXX
Sparse-Aperture Interferometric ImagingR~100; tunable 3.0 – 5.0 microns
Sparse-Aperture Interferometric ImagingFixed medium-band filters
Single-Object Slitless SpectroscopyR~700; 0.7 – 3.0 microns
Broad-Band ImagingFixed filters; 1 – 5 microns
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TIPS/JIM2011 September 15
Optical Layout of the TFI
20482048 HgCdTe5.2 micron cut-off18 micron pixels
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TIPS/JIM2011 September 15
Optical Layout of NIRISS
20482048 HgCdTe5.2 micron cut-off18 micron pixels
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TIPS/JIM2011 September 15
Elements in the NIRISS Dual Wheel
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TIPS/JIM2011 September 15
Wide-Field Slitless Spectroscopy
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Slitless Spectroscopy with Two Orthogonal Grisms
• A spectrum for every source in the field of view.
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NIRISS is Competitive With NIRSpec
Bad
Good
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TIPS/JIM2011 September 15
Sparse-Aperture Interferometric Imaging
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Sparse-aperture interferometry with NIRISS pushes the angular resolution of JWST to its limit
goal
Beichman et al 2010
Bright planets
Faint planets
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Filter Set (3) for Use With MASKNR Optimized for constraining temperature and mass.
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TIPS/JIM2011 September 15
Single-Object Slitless Spectroscopy
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G700XD design
R 700 dispersion with grism along V2∼ Low dispersion with prism along V3, to separate orders Weak cylindrical lens on front side of prism to induce a
defocus along V3
weak cylindrical
surface
m=0
m=1
m=2
m=3
Slitless cross-dispersed 0.6-3.0 μm spectroscopy
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17
Schematic of Transit and Eclipse Science
Measure size of planet 10-2
See starlight transmittedthrough planet atmosphere 10-4
Eclipse
Planet thermalemission appearsand disappears 10-3
Learn about atmosphericcirculation from thermalphase curves
Transit
Seager & Deming (2010, ARAA, 48, 631)
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Transit Spectrum of Habitable “Ocean Planet”
NIRISS G700XD perfectly suited for such challenging programs. The water vapor features below have a depth of 50 parts per million.
0.6 μm 2.5 μm
NIRISS wavelength range
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TIPS/JIM2011 September 15
Broad-Band Imaging - Blue
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TIPS/JIM2011 September 15
Broad-Band Imaging - Red
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NIRISS Sensitivity vs NIRCam
Good
In general , NIRISS is more sensitive than NIRCam.
NIRISS with spare NIRCam filter filter
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TIPS/JIM2011 September 15
Summary
NIRISS is coming!
Capable instrumentComplements & Extends near-IR capability of JWSTStraightforward to operate*
* Grisms / aperture mask introduce complexity on the “back end”.
First Light: Lyman alpha emitters (10< z<13) ; photometric redshifts
High-resolution imaging: exoplanet imaging and characterization
Spectroscopy of transiting exoplanet atmospheres (including H2O, CO2 features…)