ULTIMATE Subaru AYO / instrument fact sheets ULTIMATE Subaru Working Group
(3) Wavefront Sensors 4x LGS > 8x8 Shack-Hartmann for each 3 x Tip/Tilt NGS 2x2 Shack-Hartmann for each (1) Adaptive Secondary Mirror Preliminary Subaru ASM designed by Microgate with ~ 1000 actuators (4) Wide-field NIR instruments • Imager FoV~16arcmin max. • Multi-Object Slit spec. at Cs. focus • Multi-Object IFU spec. i Laser Guide Star system TOPICA 20W CW fiber laser(589nm) x 2 Generate 4 laser guide stars
. Sky coverage:  Almost entire sky! • Seeing improvement ↓ ↓
Note: Spatial resolution is comparable to WFIRST or HST/WFC3 (particularly at K-band) obabili
1)  Wide-field imager 2)  Multi-object integral field spectrograph 3)  Multi-slit spectrograph
ª In case of using MOIRCS as a spectrograph. b FoV will be limited to 6' if the instrument is installed at NsIR. c NBF, MBF, and TBF indicate narrow-band, medium-band, and tunable filters, respectively. d Total Efficiency includes atmosphere, telescope, and instrument (optics + detector). Note: There are three instrument plans, with wide-field imager being the highest priority (according to the review meeting in February), but we would like to have your comments on the priority during the workshop.
Appendix
Tele
•   In addition to the wide-field GLAO, the adaptive secondary mirror (ASM) with ~1000 actuators can provide high Strhel ratio (> 80%) with narrow-field single-conjugate AO or laser tomography AO even in the optical wavelength. → Largely improve the performance of the existing narrow-field instruments. H-band PSF obtained with LBT ASM - - ' Extreme AO with SCExAO High-Dispersion (R~160,000) Optical Spectroscopy with HDS Thermal infrared imaging/spectroscopy with IRCS/COMICS → TMT 1st gen. instruments will not offer such capabilities. (1)  Wide-field imager

Summary
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 WFC covers ~14’x14’ FoV with ~0.1” pixel scale - although exact values of these parameters are still TBD. Your input is welcome. . Tunable filter option is under discussion (recommended by reviewers). . The WFC is currently the 1st priority instrument for ULTIMATE. . We can expect sensitivity improvement by ~o.75-mag for point source.
Example filter set (from SWIMS-18). Note that this is just an example ! We plan to install many filters (BB/ MB/NB) on WFC, as shown in left. You can expect sensitivity improve- ment by 0.75-mag compared with MOIRCS (for point source; see table below). See next page for extended source. Please contact us if you need sensitivity for NBs.
These estimates are from MOIRCS ETC by changing seeing size and/or aperture sizes.
(in collaboration with AAO/Australia team)

Summary
• >10 IFUs within ~15’ FoV. Each IFU has 1.18 arcsec² with 0.15” spatial sampling. . Wavelength coverage is < 1.8um – i.e. K-band is not available with current plan. Roughly speaking – you can imaging GLAO-assisted KMOS(VLT). . . See talk by S. Ellis (AAO) for more details of Starbug+IFU system.
a This number can be increased by using a new larger spectrograph. b FoV of the wide field corrector.
Expected sensitivity for emission-lines (S/N per spaxel with 1-hr on-source integration) (3) Multi-object slit spectrograph

Summary
• Technical study for ULTIMATE MOS spectrograph is very premature – but at this moment we assume “MOSFIRE-like” instrument with specification below. Sensitivity calculation follows next page. .
Expected sensitivity for emission-lines (point source and extended source) Figure 7.26: Expected emission line flux detected at 5 σ in 5 hours integration time as a function of wavelength in NIR (1.0-2.5μm). Left and right panels show the limiting line flux for point sources and
Expected sensitivity for continuum (point source and extended source) Figure 7.27: Expected continuum flux in AB magnitude detected at 5 σ in 5 hours integration time. Left and right panels show the sensitivity for point sources and extended sources (same as Figure 7.26), respectively. Red and blue lines show the expected sensitivity for the ULTIMATE-Subaru (GLAO), and