Subaru/XMM-Newton Deep Survey Observing galaxy mass assembly at z > 1 in the SXDF FMOS Science Workshop January 13, 2004 Kaz Sekiguchi (Subaru Telescope) ★ Redshift Desert ★ Subaru/XMM-Newton Deep Field ★ What the FOMS can do ?
Dec 26, 2015
Subaru/XMM-Newton Deep Survey
Observing galaxy mass assembly at z > 1 in the SXDF
FMOS Science WorkshopJanuary 13, 2004
Kaz Sekiguchi (Subaru Telescope)
★ Redshift Desert
★ Subaru/XMM-Newton Deep Field
★ What the FOMS can do ?
Subaru/XMM-Newton Deep Survey
Redshift Desert: 1.0 < z < 2.0~2.5
Where the familiar optical spectral features redshifted inthe near infrared region,
From Glazebrook (2004)
Subaru/XMM-Newton Deep Survey
z Age of U (Gyr) 0 13.666 1.0 5.935 1.5 4.346 2.0 3.342 2.5 2.667
Redshift Desert is an important epoch of the history of the Universe.-> Peak of the QSO epoch-> Formation of ☆’s in massive galaxies (from Sub-mm) [Test ground of the current hierarchical paradigm]
Subaru/XMM-Newton Deep Survey
From GEMINI GDDS Press Release
Subaru/XMM-Newton Deep Survey
LRIS-B (Keck-I) study by Steidel et al. (2004)
・ Optical Spectroscopy using LRIS-B (Keck-I)・ Covers 3,200 Å < λ< 6,000 Å (FWHM ≈ 1.5-2.0Å)・ Sample selection : R, G, & Un・ Magnitude limit : R = 25.5・ Integration time : 5,400 sec・ # of Objects : 792
Compare to the sample of star forming galaxies at z~3,galaxies at z~2 are significantly redder. This indicates an increase in the average stellar mass at z~2 comparedto their counterparts at z~3.
Subaru/XMM-Newton Deep Survey
Subaru/XMM-Newton Deep Survey
Subaru/XMM-Newton Deep Survey
Subaru/XMM-Newton Deep Survey
FIRES /HDFS (Franx et al. 2000, 2003)
・ Near-IR Photometry ・ Js, H, Ks ・ Sample selection : Js-Ks >2.3 (z > 2)・ Magnitude limit : Ks < 22.5・ Field size : 4.7 arcmin2
・ 14 galaxies・ Surface density : 3±0.8 galaxies arcmin-2
・ Photometric redshift : 1.92 < z < 4.26 (median z = 2.6)・ One Star –forming G & Red faint optical (median V=26.6)
Remnants of the LBG of higher redshifts ( z > 4) ???
Subaru/XMM-Newton Deep Survey
K20 (Daddi et al., 2004)
・ Optical Spectroscopy using VLT FORS1 & FORS2・ Covers 3,600 Å < λ< 8,000 Å (FWHM ≈ 13 Å)・ Sample selection : Ks-band・ Magnitude limit : Ks < 20 ・ Two fields (52 arcmin2)・ 546 objects (about 30 galaxies are z > 1.7, ~ 6%)Subset of K20/GOODS-South・ 32 arcmin2
・ 304 objects (9 galaxies with spectroscopic z > 1.7, ~ 3%)・ Surface density : 0.28±0.26/0.13 galaxies arcmin-2
z~2, the peak or low-z tail of the massive galaxy assembly?
Subaru/XMM-Newton Deep Survey
Subaru/XMM-Newton Deep Survey
Gemini Deep Deep Servey (GDDS, Glazebrook 2003 & 2004)
・ Optical Spectroscopy using GMOS with Nod & Shuffle・ Covers 5,000 Å < λ< 10,000 Å (FWHM ≈ 16 Å)・ Sample selection : K-band・ Magnitude limit : K = 20.6・ 4 fields (5’5 x 5.’5)
Two of them:SA22 (48,600 sec) : 111 objectsNDWS (90,000 sec) : 60 objects
The mass density in the most massive galaxies declinesvery slowly to z = 2. Giant galaxies formed much earlier(at z > 3).
Subaru/XMM-Newton Deep Survey
(From Glazebrook et al., 2004)
Subaru/XMM-Newton Deep Survey
(From Glazebrook et al., 2004)
Subaru/XMM-Newton Deep Survey
(From Glazebrook et al., 2004)
Subaru/XMM-Newton Deep Survey
Subaru Telescope Observatory Project
SXDS Teamhttp://www.naoj.org/science/sxds/index.html
Subaru/XMM-Newton Deep Survey
SXDS Team members :Akiyama M.1, Aoki K. 1, Doi M.2, Furusawa H. 1, Fuse T. 1, Imanishi M. 3, Ishida C. 1, Iye M. 3, Kajisawa K. 4, Karoji H. 1, Kobayashi N. 2, Kodama T. 3, Komiyama Y. 1, Kosugi G. 1, Maeda Y. 5, Miyazaki S. 3, Mizumoto Y. 3 Morokuma T2. Nakata F. 6, Noumaru J. 1, Ogasawara R. 1, Ouchi M. 2, Sasaki T. 1, Sekiguchi K. 1, Shimasaku K. 1, Simpson C. 6, Takata T. 1, Tanaka I. 3, Ueda Y. 5, Watson M. 7, Yamada T. 3, Yasuda N. 3, & Yoshida M. 8
1 Subaru Telescope, 2 University of Tokyo, 3 National Astronomical Observatory of Japan, 4 Tohoku University, 5 Institute of Space and Astronautical Science 6 University of Durham7 University of Leicester (XMM/SSC)8 Okayama Astrophysical Observatory
Subaru/XMM-Newton Deep Survey
Chandra DFS
VIRMOS Deep
SA68
LZLE
Slone Slone
Various Survey fields on the Subaru sky
SXDS Field
COSMOS
Subaru/XMM-Newton Deep Survey
1.3º
02h18m
-5º00’
SXDS Field
Subaru/XMM-Newton Deep Survey(From Benson et al. 2001)
141h
-1 M
pc
z = 3.0
B-V-0.1 0.9
-22.0-21.5-21.0-20.5-20.0-19.5-19.0
MB – 5 log h
GOODS
COSMOS
SXDS
HDF
Subaru/XMM-Newton Deep Survey
Multiwavelength: ( : Done, : On-going, Allocated)✓ ✜
✓XMM-Newton (XMM/SSC) PI: Mike Watson✓Subaru B,(V),R,i’& z’Imaging SXDS Team
ESO/VLT U Imaging Public Survey
✜Subaru FOCAS Spectroscopy SXDS Team✓AAT 2dF Spectroscopy AAT/SXDS Team
UKIRT/WFCAM (UKIDSS/UDS) PI: Omar AlmainiSIRTF (SWIRE) PI: Carol LonsdaleBLAST (BLAST Consortium) PI: Mark Devlin
✜JCMT/SCUBA (SHADES) PI: James Dunlop ✓VLA PI: Chris Simpson
✓HST ACS (I-band) as part of the High-z SNe project
CSO : 350μ Obs. SHADES+Canadian
Subaru/XMM-Newton Deep Survey
Multiwavelength: (Planned)
Chandra : X-ray high spatial resolution imaging
GALEX : UV imaging & spectroscopy
VIMOS : Multi-Object Spectroscopy
SMA : high spatial resolution mm imaging
ALMA : high spatial resolution mm imaging
SIRTF: IRAC Deep Imaging
Subaru/FMOS: Galaxy Survey of 1.0 < z < 2.0
Subaru/XMM-Newton Deep Survey
100
50 50
50 50
50 50
1.3 deg
x-ray
400 ksec of EPIC data from XMM/Newton:100 ksec on central field50 ksec on 6 flanking fields
Subaru/XMM-Newton Deep Survey
deta
iled
X-r
ay s
pectr
a~
30 s
ou
rces
cru
de X
-ray s
pectr
a~
300 s
ou
rces
X-r
ay c
olo
urs
~1000 s
ou
rces
~1000 X-ray detections
source detection and parameterisation completed
– X-ray colours, spectra, morphology
– X-ray variability 12h• 24h (between
obs)• years (SDS-4
& some overlap regions)
Subaru/XMM-Newton Deep Survey
Subaru/XMM-Newton Deep Survey
Optical Imaging by Subaru Suprime-Cam
The SXDS covers 5 Suprime-Cam pointings (1.3 deg2) to the exposure time (estimated depth) :
B : 18,000 sec, 900sec x 20 (B=28.1) ( s/n=3σ) R : 12,480 sec, 480sec x 26 (R=27.5) i’: 15,000 sec, 300sec x 50 (i’=27.3) z’: 14,560 sec, 180sec x 80 (z’=26.7)
All 5 FOV
Consistent with n(m) given in previous surveys
~0.3-0.5 mag deeper thanGTO SDF data
From Furusawa
Subaru/XMM-Newton Deep Survey
x-rayoptical
deep Suprime-Cam BRi’z’ (& V) data over entire SXDS field, plus some spectroscopy (FOCAS and AAT/2dF)plus ESO/VLT deep U (to 27 mag) over entire SXDS field and extensive moderately-deep FOCAS spectroscopy
Subaru/XMM-Newton Deep Survey
From Furusawa
Subaru/XMM-Newton Deep Survey
FOCAS/MOS: 30 masks (~1-2 hr per field , ~500 IDs)
2dF/AAT : 4 nights
Spectroscopic ID of X-ray Sources in the SXDS field
From Akiyama
Subaru/XMM-Newton Deep Survey
Spectra of XMM-Newton X-ray Sources Taken by FOCAS MOS
From Akiyama
Subaru/XMM-Newton Deep Survey
* QSO at z=4.5
10 fields (0.2-3hours) = ~3000 objectsR<21mag QSOs, R<20 mag Galaxies
AAT/ 2dF Spectroscopy
From Akiyama
Subaru/XMM-Newton Deep Survey
x-rayopticalNIR
175 arcmin2 to J=22, H=21 & K=20 from UH2.2m/SIRIUS800 arcmin2 to J=21.5, H=20.5, & K=19.5 from SAAO1.4m / SIRIUS0.7 deg2 to J=25, H=24 & K=23 from UKIRT / WFCAM (UKIDSS / UDS)
Subaru/XMM-Newton Deep Survey
SIRIUS JHKs coverage of the SXDF
From Takata et al.
Subaru/XMM-Newton Deep Survey
Telescope: 1.4m IRSF @ SAAO, SutherlandInstrument: SIRIUS(Simultaneous 3color Infrared Imager for Unbiased Survey)
1 field => 7.8’x7.8’ J,H,Ks simultaneous imaging2 hours exposure of 18 field (~790 arcmin2)Seeing was ~1.0-1.4 arcsec @Ks bandDepth: Ks(Vega)=19.3-19.5 ?(to be estimated)
~4000 object with Ks(Vega) < 19.2
From Takata et al.
Subaru/XMM-Newton Deep Survey
Red: EROViolet:VLA RadioGreen:X-ray
From Takata et al.
Subaru/XMM-Newton Deep Survey
From Takata et al.
Subaru/XMM-Newton Deep Survey
Sky Distribution of EROs (R-Ks>5.3 & i’-Ks>4.0 & Ks<19.2)
From Takata et al.
Subaru/XMM-Newton Deep Survey
WFCAM Cryostat
Subaru/XMM-Newton Deep Survey
UKIDSS UDS Science goals K=23.0 (0.4 microJy) 0.77 sq. degs
Epoch of spheroid formation
Map of the Universe at z=3
Relation between EROs, ULIRGs, & AGN
Subaru/XMM-Newton Deep Survey
x-rayopticalNIRMFIR
MIR imaging with IRAC to S3.6=7 Jy, S4.5=10 Jy, S5.8=27 Jy, S8.0=32 Jy
MIR imaging with MIPS to S24=0.4 mJy, S70=2.7 mJy,
S160=17 mJy
MIR imaging with IRAC to S3.6=7 Jy, S4.5=10 Jy, S5.8=27 Jy, S8.0=32 Jy
MIR imaging with MIPS to S24=0.4 mJy, S70=2.7 mJy,
S160=17 mJy
Subaru/XMM-Newton Deep Survey
Subaru/XMM-Newton Deep Survey
x-rayopticalNIRMFIRsubmmradio
entire field to S1.4=15 mJy with B-array VLA
entire field to S5=30 mJy with B-array VLA
GMRT240MHz & 151MHz
Subaru/XMM-Newton Deep Survey
Subaru/XMM-Newton Deep Survey
1.3º
02h18m
-5º00’
Subaru/XMM-Newton Deep Survey
・ What the FMOS can do (?)
There are ~ 10,000 galaxies with Ks < 20 in the SXDF.These galaxies can be observed with FMOS in 100 hours(assuming the average integration time of 3 hours per setting)
Then, we can expect about a few hundreds to a thousandof z > 1 galaxies sample. These include both blue & redgalaxies, EROs, sub-mm galaxies, and QSOs.
Subaru/XMM-Newton Deep Survey
・ Properties of the galaxies in the “Redshift Desert” ・ Redshift distribution・ Evolution of LF・ Evolution of LD・ Evolution ot galaxy star mass function・ Nature of old & dusty EROs・ Nature of Starburst at z ~ 2
Combined with FMOS data and some K-band MOIRCS observations at the center field ( where also the SHADES data exist) and the wealth of the Multiwavelength data available, we can explore;
Subaru/XMM-Newton Deep Survey
Subaru/XMM-Newton Deep Survey