220 likes | 321 Views
FMOS on COSMOS. Tomo GOTO (ifa/Subaru, JSPS fellow). J=20.1 H=19.8. Current status. Open for common use starting 10A. Only IRS1, low resolution mode available (200 fibers). Full 400 fibers, high-resolution will be operational from 11A. Continuum sensitivity. For 1 hour, 4pix,
E N D
FMOS on COSMOS Tomo GOTO (ifa/Subaru, JSPS fellow) T.Goto
J=20.1 H=19.8 T.Goto
Current status • Open for common use starting 10A. • Only IRS1, low resolution mode available (200 fibers). • Full 400 fibers, high-resolution will be operational from 11A. T.Goto
Continuum sensitivity For 1 hour, 4pix, S/N=5 at (ABmag) In reality, 1.05-1.7um T.Goto
Line sensitivity For 1 hour, S/N=5 at 1x10-16 erg/cm2/s Corrected for fiber loss T.Goto
Proposal deadline 9/30/10 FMOS instrument team is preparing a proposal. T.Goto
FMOS team SSP proposal draft • Galaxy/AGN , SXDS • Photoz sample 10 nights, • X-ray AGN: 10 nights • Emitter : 5 nights • Cluster: 16 nights • Subaru deep field (photoz+emitter) :8 nights • AKARI NEP (mid-IR source) : 5 nights • Redshift space distortion :50 nights • Pending :10 nights. • Total 140 nights (including weather factor). T.Goto
Why not COSMOS field? • HST morphology is irreplaceable. • Accurate photo-z is essential when continuum sensitivity is not good. • Many one line only detections expected. Need photo-z to use data. • X-ray, Spitzer, Herschel coverages are better than other large field. T.Goto
Public COSMOS data • RA (J2000) = 10:00:28.6, DEC (J2000) = +02:12:21.0 • 588 orbits of HST/ACS, ~2 million objects to IAB < 27; • Photo-z accurate to Δz < 1% (30 bands) • GALEX, CFHTui, • Subaru (Bvgri, z =26.5AB+13 Int. bands, NBs) • UKIRT YHK, KPNO J, • X-ray • XMM • Chandra ~1700 Chandra sources down to 610-16 cgs, >half with spectroscopic redshifts. 1.8 Ms,1sq.deg,@160 ksec,1761 sources (Elvis et al) • IR • Spitzer IRAC/MIPS, 3,4,5,8,24,70,160um. 24um>0.42mJy. • RADIO, VLA • Spectra • ZCOSMOS, 10,000 spectra at z<1 T.Goto Maximum science output from rich data sets (HST,photoz…)
Cosmos data in future • UltraVista Y=26.7, J=26.6,H=26.1, K=25.6 • Herschel PACS/SPIRE (100,160,250,350, 500um) • WFC3 data 0.1sq.deg T.Goto
Excellent Spitzer coverage T.Goto
N sources • X-ray sources XMM:1886, Chandra 1761 • 24um: 17713 • 70um: 1513 • 160um: 499 • VLA: 2901 • Photoz: 1<z<1.6, 39582 galaxies. • => FMOS T.Goto
FMOS 1hr sensitivity T.Goto
My proposal to the FMOS team • 1<z<1.6 with Hβ, [OIII], Hα • Hα flux>3x10-16 erg/s/cm2 (1hr exposure) • 18277 galaxies • 18277/400x2hrs, => 11 nights • could include • 24um sources • X-ray sources • LAE/LBG at high-z T.Goto
My proposal to the FMOS team Science cases at 1<z<1.6 • 100Mpc scale, includes rich cluster to field(5x106 Mpc3) • LF, MF, HαLF, SFRD • Morphology, environment, SFR • AGN/SB • X-ray/radio/IR sources • Obscured sources… • With spec-z and Hαluminosity T.Goto
FMOS teams response: “Tomo, What you are saying is absolutely right.” “COSMOS is the best field to observe.” But…. COSMOS cannot be included in the initial targets because… part of us are cosmos members. “This is a complicated political issue, Tomo” ??? T.Goto
So COSMOS won’t be in initial targets. I failed. According to Japanese tradition, I should do HARAKIRI But not so soon, T.Goto
My life is saved! • FMOS team does not want to PI COSMOS field, but they welcome someone else to do the field. • SSP must open the proposal to entire Japanese community. They will accept proposal for additional field. • “Tomo, COSMOS stands a good chance.” T.Goto
Summary • COSMOS is a good target for FMOS SSP. • It won’t be in the initial list of targets. • But it is likely, to be added to targets at later stage, if we keep pushing. • We can do a lot with 20k NIR spectra. T.Goto