Panoramic Survey of the Deep UniverseObserving Galaxy Formation at High RedshiftToru Yamada National Astronomical Observatory of JapanOpt/IR Div., Subaru Telescope

Needs for Panoramic Deep SurveysSubaru/XMM-Newton Deep SurveyExtensive Study of Ly Blobs and High Redshift Large-Scale Structure

1. Panoramic Deep Surveys- Subaru Deep Field Surveys *- Subaru/XMM-Newton Deep Survey *- EIS+Subaru Survey- COSMOS NEP Deep Survey (+Astro-F) SSA22 Emission Line Galaxy Survey *UKIDSS-DXS/Scam 10 deg2 Survey *etc, etc* T.Y. involved

Cosmic Microwave Background measured by WMAPage of the Universe: 380 kyrs

B&WmassCDMJoerg Colberg and Antonaldo Diaferio http://www.mpa-garching.mpg.de/GIF/21 Mpc (Comoving)Early (massive) galaxy formation preferentiallyoccurs in the region of large-scale density peakswhich will evolve to massive clusters. Cluster galaxies are old Spatial distribution of high-z galaxies is much inhomogeneous than that of mass.Galaxy Formation occurs in the Biased mannerdue to the collapse of high peak of CDM fluctuationand some local physical processes (Feedback;UV/Xray heating, Super-galactic wind).BlueYoung GalsRed Old GalsN-body+ Semi-analytic treatment

z=3 simulation at larger scale(Benson et al. 2001)B&W :CDMColord: Galaxies141 h-1 MpcN-body + semi-analytic treatment

Two-Point Correlation Function of ~6000 z~4 B-drop Lyman Break Galaxies In the Subaru SXDS Field Strong clustering of high-z Star-Forming galaxies = bias to the mass (Steidel et al. 1998. Adelberger et al. 1999)biasmassgalaxiesat high-z large scale (~10 Mpc), bias is likely to be treated as linear bias, g=b

Whole picture of structure formationEvents with shorter time scale (e.g., QSO)Rare objectsHigh Statistical AccuracyDeep Imaging of High-z Universe Pencil-Beam Surveys are not sufficient. Panoramic Surveys over large comoving volume are needed.

Deepest Image of the Universe we have: Hubble Ultra Deep Field (2004) 3ACSF435W (B)F606W (V)F775W (I)F840LP (z)

3 arcmin x 3 arcmin 9 arcmin2 Vcomoving (z < 1) ~ 1 x 104 Mpc3 (0=0.3:=0.7: H0=70 km/s/Mpc) Vcomoving (z < 2) ~ 4 x 104 Mpc3 Local Universe * = 5 x 10-3 Mpc-3 (SDSS, r*) If uniform, ~200 L* or brighter galaxies at z~2 /unit redshiftPhysical dimension~ 1 - 1.5 Mpc Just twice of the distance between M31 and MW ) M31 d=0.7 Mpc

From STScI HUDF web page

2. Subaru/XMM-Newton Deep Surveyan example of deep panoramic survey in multi wavelength

Subaru/XMM-Newton Deep Survey (SXDS)Galaxy evolution can be studied in sufficiently large volume. Optical (Subaru) X-ray (XMM-Newton)1.2 deg2SXDS is observed in NIR (UKIDSS UDS), radio (VLA), sub-mm (SHADES), etc.HUDF

(From Benson et al. 2001)141h-1 Mpcz = 3.0B-V-0.10.9-22.0-21.5-21.0-20.5-20.0-19.5-19.0MB 5 log hGOODSCOSMOSSXDSHDF2x10x162 sq. deg2.5SXDSthin slice

z~4 Star-Forming Galaxies in SXDS B-Drop Lyman Break Galaxies ~6000 B-drop LBGs i < 24 24 < i < 25 25 < i < 26

z~1 Evolved Quiescent Galaxies Old Passively-Evolving Galaxies (OPEGs)zf=2-103900 OPEGs selected Riz colors to z=25

z=4z=11 < z < 4Dark Matter HaloLyman Beake GalaxiesgasOPEGsZ>4

Two-Point Correlation Function of ~6000 z~4 B-drop Lyman Break Galaxies In the Subaru SXDS Field Strong clustering of high-z Star-Forming galaxies = bias to the mass (Steidel et al. 1998. Adelberger et al. 1999)biasmassgalaxiesat high-z large scale (~10 Mpc), bias is likely to be treated as linear bias, g=b Preliminary results

biasHalo Occupation Model< Host Mass >Galaxy DensityHalo OccupationNumberHamana, TY, et al.

z = 4 LBGs

Preliminary results

Mmin1x1012 Msun2.6x1012 Msun M13x1011 Msun

Statistical fate of z=4 DM halo with 2.6x1012 h-1 Msun(calculated using the Extended Press-Schechter model )T. Hamana, TY, et al.Preliminary results

Our ResultsSolid lineHalo mass growth curveIn CDMDashed lines68% intervalAverage host halo mass ofgalaxies obtained from their clustering propertiesz~4 LBGsz~1 OPEGsPreliminary results

Discovery of the two seed clusters in SXDS (Ouchi et al. 2005)Deep NB816 Narrow-Band Survey (8160, for z=5.7 Lyemitters)

Clump Av~ 180 km/sM~1x1013Msun

C-M sequence expected forpassive evolutionKodama, TY et al. 2004Color-Magnitude Diagram for z~1 galaxies1.2

Galaxy Color Evolution in HDF-N (Kajisawa and Yamada 2004)Results obtained with a pencil-beam survey EXTEND TO SXDS !

Large-Scale Structure of Ly Emitters and Massive Galaxy Formation3. Extensive Study of Ly Blobs at High Redshift

B&W :CDMColored: Galaxies141 h-1 MpcN-body + semi-analytic treatmentz~3simulation

SSA22 Proto-cluster at z=3.1Discovery of the SSA22 proto-cluster of Lyman Break Galaxiesat z=3.1 (Steidel et al. 1998)

Extended LyEmitters: Ly Blobs (LABs) Giant LyEmission-Line Nebulae> 100 kpc (physical scale) (Steidel et al. 1998, Keel et al. 1999)

Internal velocity structure v>1000 km/s (Ohyama et al. 2004, Bower et al. 2004)

Not enough UV by the apparent SFR

4 previous examples of LAB with > 100 kpc at z=2~3 are all in the high density regions of LAELABs are mysterious objectsHow frequent are they?How they related with galaxy-formation phenomena?LAB1LAB2

Subaru Narrow-Band Observation of the SSA22 Proto-cluster regionLy Emitters (LA)Ly absorbersLAE average local density2 x 10-17 erg/s/cm2EWobs > 160 Hayashino et al. 2004Steidel et al. 2000HDR

Redshift Distribution of LAEsRedshiftLAEsLAB1, LAB2Obs: Subaru FOCAS56 objects

LAE survey: extension to the North-West area SSA22-Sb2 SSA22-Sb1 (Hayashino et al. 2004)50 Mpc (comoving)LAE NB497 < 26.0 EW > 1202 x 10-17 erg/s/cm2EWobs > 120 Sb1+Sb2 ~600

Ly image(after continuum subtraction)z=3.1LBG25 = 190 kpc (before subtraction)B, V, NB. Ly= greenCont. subtracted image Subaru 7h image of LAB1How ordinary these gigantic LABs are ?What are their size, luminosity, and spatial distribution?

25 or 190 kpc at z = 3.135 Ly Blobs (Matsuda et al. 2004)First large sample of LABs

>16 arcsec2>7in isophotal apertureor, d~30kpc !900 kpc2at z=3.1

Sky distribution 35 LABs and LAEs

Lyexcess is seen for 14/35 objects(in the apparent flux)LAB: origins of the Ly

(1) Photoionization by massive stars or by AGN (in some cases may be hidden by dust) by diffuse background UV ?(2) Atomic cooling radiation (early phase of galaxy formation)(3) Superwind (late phase of intense star formation)

Plus, scattering..

Hidden star formation/AGN ??25=190 kpcLypeakCont. ?Ly peak is displaced from the continuum peak

Superwind ? Cooling flow ? Also see Ohyama et al. 2003, Bower et al. 2004 25=190 kpc

Atomic cooling emission from a proto galaxy ??- Diffuse morphology - No plausible continuum source 25=190 kpcTurned out to be associated with X-ray (XMM) and sub-mm source

Results of SCUBA sub-mm observations w/ Smail, Chapman, et al.LAB1LAB18 (XMM source!)LAB14 detected in Barger et al., Chapman et al. 2004 so to be confirmedc.f., Lyman Break

53W002 No.18 LAB Keel et al. (1999)SCUBA Source SMM 02399-0136 (z=2.8) Detected inSub-mm observation(Smail et al. 2003)10LyLy+contLyNVLyHaloSlit directionwavelengthLABs in Matsuda et al.

LABs in the new survey field

LABs in the new survey field

A New Gigantic LAB with > 100 kpc in SSA22-Sb2 fielfd, which iscomparable with LAB1, LAB2 in the SSA22-Sb1 field25=190 kpc2005/08 3D spextroscopywith VLT VIMOSMatsuda et al.LABs in the new survey field

Slit spectroscopy of LABs with Keck DEIMOS

Relatively compact Ly emitters v < 500 km/s

Ly Blobs : many have v > 500 km/s, absorption

[Gaussian fit ]LAB16 sq.arcsec d~30 kpcFWHM~500 km/sSlit spectroscopy of LABs with Keck DEIMOS

1. (Lower limit of) their mass can be evaluated from their size, assuming that they are collapsed objects (before z=3.1), if we apply the spherical collapse model.

Mvir = 4/3Rvir3 crit(z) c(z) > 4x1010 (RLy / 26kpc)3 Msun

Assuming that they are bounded objects, their mass can be evaluated from their size and internal velocity Mdyn ~1012-13 Msun

3. Strong clustering associated with more massive DM halos ?

4. Possibly higher sub-mm detection rate (massive SF)Mass of the LABsMassive Galaxies in Their Forming PhaseLarge Ly Luminosity, Extension, Clustering, High sub-mm ditection rate

SummaryDeep Panoramic Surveys probe the universe

Galaxy evolutions are being studied in large-volume, highly statistically accurate sample of the SXDS galaxies - connection between z~4 LBGs and z~1 OPEGs - seed cluster at z=5.7 discovered in the NB search - nature of the optically-faint X-ray sources - mass dependency of galaxy evolution

We discovered ~100 Mpc LSS of LAE at z~3.1. LyBlobs, candidates of massive forming galaxies are distributed along the LSS.

Future ProspectsSCam / UKIDSS DXS 10 deg2 surveyELAIS N1LockmanHoleExtension of z~3 LSS andLAB/LAA/LAE searchCovered by UKIDSS DXSSWIREIRAC(blue)MIPS(red)

Scam(white)

Future ProspectsSubaru New NIR Camera andSpectrograph MOIRCSA New Mission Hubble Origins ProbeVery Wide Field Imager4x7GOODS-N