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ALMA -JWST Synergy:Disk Structure and Chemistry in 2013
Alycia J. WeinbergerCarnegie / DTM
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Some JWST Basics
Telescope18 Be Segments, Au coated6.5 m diameter150 K primary mirror temperatureLocated at L2
4 Science InstrumentsFine Guidance Sensor - Tunable Filter Modules
(FGS-TS)Near Infrared Camera (NIRCam)Near Infrared Spectrograph (NIRSpec)Mid Infrared Instrument (MIRI)
Launch: Scheduled for 2013
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The Successor
HST
And
Spitzer
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JWST-Spitzer Comparison
Beam Size at 8 µm: * Spitzer: 2’’• JWST: 0.25’’
(µJy)
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MIRI Background
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MIRI (http://ircamera.as.arizona.edu/MIRI)
Imaging 5-27 µm with 1.3x1.7’ FOVCoronagraphs at 10.65, 11.4, 15.5, 23 µm
0.05’’ resol; Kalas et al.2005
7.5’’ resol.Holland et al. 2003
5.8’’ resol.Stapelfeldt et al. 2003
ALMA at 450 µm can be < 0.1’’; JWST 24 µm resolution is 0.8’’
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MIRI Spectroscopy
R~100 at 5-10 µmR~3000 5-28.3 µm
(in 3 portions)
12.1 12.3 12.5H2
S(2)
flu
x [m
Jy]
Lahuis et al. 2007, ApJ in press
Note: Spitzer IRS has R~600
Track the CO:H2 ratioin disks over time
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Gas:Dust Statistically
Rettig et al. 2006
Observe disks ata range ofinclinations
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Beta Pic Gas Composition
No Debris Disks have (yet) detections of submm gas emission
(Roberge et al. 2006,Nature)
C:O = 18 × solar
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NIRCam (http://ircamera.as.arizona.edu/nircam)
Two Channels: 0.6-2.4 µm and 2.5-5 µm Nyquist sampled at 2 and 4 µm Field of View: 2.2 x 4.4 arcmin Coronagraphy
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FGS-TFI
1.2 - 2.4 µm and 2.4 - 4.8 µm2.2 x 2.2 arcmin FOVSelectable R~100Coronagraphs for 20x20’’ FOV
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FGS-TFI Contrast at 4.5µm
100
10-2
10-4
10-6
10-8
0 1 2 3 4 5Separation (arcsec)
Cont
rast
Rat
ioPlanet and Disk Imaging
Doyon et al. 2004
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Contrast Similar to HST
HR 4796: NICMOS/STISContrast ~ 10-4 at 0.5’’
Image: Color compositeat 0.5 - 2.2 µm(Debes, Weinberger & Schneider,in prep )
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Imaging in Scattered LightCoronagraphy in FGS-TF and NIRCam
Green et al.2005
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Scattering Albedo: Silicates,Ices and Organics
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NIRSpec (http://www.stsci.edu/jwst/instruments/)
0.6 - 5 µmR=100, 1000, 3000FOV 3.4 x 3.4 arcminMicroshutter arrayContrast
(open/closed)~3000
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TW Hya With HST
1.1 µm1.6 µm
Color same as star: largeish grains, as expectedInner Warp?
Roberge et al. 2005 Debes et al. in prep0.5 - 2 µm
500 AU
0.5 µm “True” Color
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Spatially Resolved Spectra
Blue color in inner-most disk: collision dominated?
Roberge et al. 2005
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My Combo Wish List
Spatially resolved gas:dust ratios anddepletion in transitional disks
Prevalence of organics on surfaces andin gas phase of disks
Ice lines;volatile gradients in disks
Disk morphologies and evidence forplanets
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More about JWST
Space Science Reviews Paper on JWSTCapabilities by Gardner et al.: http://arxiv.org/abs/astro-ph/0606175
Space Telescope Science Institute JWST Site:http://jwstsite.stsci.edu/