subaru/xmm-newton deep survey observing galaxy mass assembly at z > 1 in the sxdf fmos science...

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 ?


Redshift Desert: 1.0 < z < 2.0~2.5

Where the familiar optical spectral features redshifted inthe near infrared region,

From Glazebrook (2004)


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]


From GEMINI GDDS Press Release


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.


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) ???


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?


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).


(From Glazebrook et al., 2004)


Subaru Telescope Observatory Project

SXDS Teamhttp://www.naoj.org/science/sxds/index.html


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


Chandra DFS

VIRMOS Deep

SA68

LZLE

Slone Slone

Various Survey fields on the Subaru sky

SXDS Field

COSMOS


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


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


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


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


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)


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


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


From Furusawa


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


Spectra of XMM-Newton X-ray Sources Taken by FOCAS MOS

From Akiyama


* QSO at z=4.5

10 fields (0.2-3hours) = ~3000 objectsR<21mag QSOs, R<20 mag Galaxies

AAT/ 2dF Spectroscopy

From Akiyama


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)


SIRIUS JHKs coverage of the SXDF

From Takata et al.


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.


Red: EROViolet:VLA RadioGreen:X-ray

From Takata et al.


From Takata et al.


Sky Distribution of EROs (R-Ks>5.3 & i’-Ks>4.0 & Ks<19.2)

From Takata et al.


WFCAM Cryostat


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


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


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


1.3º

02h18m

-5º00’


・ 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.


・ 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 observing galaxy mass assembly at z > 1 in the sxdf fmos science...

Documents

median z

spectroscopic z

gemini deep deep servey

galaxies arcmin

massive galaxies

lowz tail

giant galaxies

lbg of higher redshifts