Subaru GLAO: Comparisons with Space Missions. I. Iwata (Subaru Telescope) 2011/08/ /05/28 small revisions 2013/06/04 include JWST/NIRISS
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1 Subaru GLAO: Comparisons with Space Missions I. Iwata (Subaru Telescope) 2011/08/ /05/28 small revisions 2013/06/04 include JWST/NIRISS
2 Space Missions in Near-Future
3 JWST 6.5m Deployable Mirror, Passive Cooling at S-E L2 Four Science Instruments: MIRI: Mid-IR (5-28μm) NIRSpec NIRCam NIRISS
4 JWST MIRI Imaging μm, FoV 1.25 x 1.88 Coronagraph R=1,000-3,000 Spectroscopy at μm
5 JWST NIRCam Two Channels, both 2.2 x 4.4 Short: μm, 32 mas (8 H2RGs) Long: μm, 64 mas (2 H2RGs) Coronagraphic High Contrast Imaging Slitless Grism Spectroscopy R~1800
6 NIRCam Filters
7 JWST NIRSpec 3.6 x 3.4 FOV Micro-Shutter Assembly: 0.2 x 0.46 Micro-Shutters Fixed Slits: 0.4 x3.8, 0.2 x3.3, 1.6 x1.6 IFU: 3 x3 FOV, 30 Slices, 0.1 (dispersion) x 3 (spatial) R = 100, 1000, x H2RG
8 JWST NIRISS (Near-IR Imager and Slitless Spectrograph) 1x H2RG 5.3μm cutoff, /pix, 2.2 x 2.2 FoV Wide-Field Slitless Spectroscopy: μm, R~150 optimized for z>10 LAEs Single-Object Slitless Spectroscopy: R~700 ( μm) using crossdisperser optimized for transiting exoplanets Aperture Masking Interferometry: μm Imaging: μm
9 WISH: Wide-field Imaging Surveyor for High-redshift Space Telescope Mission with 1.5m Diameter Aperture Wide-Field Near-Infrared Camera (0.9-5 μm) (Passively) Cooled Mission with Sun - Earth L2 Orbit Depth - deeper than images with any ground-based telescopes Width square degrees in deepest images, >1,000 deg 2 in shallower surveys
10 WISH Broad-band Filter Set y J H K L M (6) IRAC1 IRAC2 Continuous Wavelength Coverage
11 Euclid, WFIRST, and WISH Euclid WFIRST WISH Mirror 1.2m 1.3m / 2.4m? 1.5m FoV 0.5 deg 2 0.3deg deg 2 Visual Imager RIz -- NIR Imager YJH μm μm Lim. Mag. 24AB 25.9AB / 28AB Survey Area 20,000 deg 2 >11,000 deg deg 2 Primary Science Expected Operations Dark Energy DE, Exoplanet, QSO (7 years) 202x? (5 years) First Galaxies end of 2010s (5 years)
12 Imaging Sensitivity
13 Imaging: Sensitivity for Point Sources MOIRCS Subaru-GLAO WISH JWST-NIRCam TMT-IRIS
14 Imaging: Sensitivities for Extended Sources MOIRCS Subaru-GLAO WISH TMT-IRIS JWST-NIRCam
15 Imaging: Sensitivity and Field-of-View 2μm MOIRCS HAWK-I VISTA Subaru-GLAO WISH TMT/IRIS JWST/NIRCam
16 Imaging: Sensitivity and Field-of-View 2μm MOIRCS HAWK-I VISTA Subaru-GLAO TMT/IRIS WFC3/IR (F160W) JWST/NIRCam WISH
17 Number Density of z=12 Galaxies JWST Imaging Limit N=1/deg 2 WISH ELT Spectroscopy Limit Lyα emission would not help improving the detection limit with ELTs for extended sources
18 Spectroscopic Sensitivity
19 Spectroscopy: Continuum Sensitivity (Point Sources) J-band MOIRCS Subaru-GLAO JWST-NIRSpec TMT-IRIS
20 Spectroscopy: Continuum Sensitivity (Point Sources) H-band MOIRCS Subaru-GLAO JWST-NIRSpec TMT-IRIS
21 Spectroscopy: Continuum Sensitivity (Point Sources) K-band MOIRCS Subaru-GLAO TMT-IRIS JWST-NIRSpec
22 Spectroscopy: Sensitivity for Emission Lines 1 hours, ~0.25 extended source MOIRCS Subaru-GLAO JWST-NIRSpec TMT-IRIS TMT-IRIS (Point Source)
23 Spectroscopy: Sensitivity for Emission Lines 1 hours, ~0.25 extended source MOIRCS Subaru-GLAO JWST-NIRSpec TMT-IRIS TMT-IRIS (Point Source)
24 Summary Imaging: Space Missions have significant advantages Narrow-band imaging capability is more suited for ground-based telescopes Spectroscopy: Sensitivity gain can be as much as ~2x with GLAO For extended sources difference between ground-based and space telescopes becomes smaller. The most sensitive observations will be realized by TMT. Reducing Read-out Noise is important.
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