Wide-field Surveys with SubaruToru Yamada

- A Review of Subaru Wide-Field and Deep Surveys+ some prospects for HSC/ WFMOS era

- Introduction to the two very wide-field deep survey with Subaru SCDXT, SSA22-NB surveys

MOIRCS 4x7

Kajisawa et al. 20067 arcminDistribution of Distant Red Galaxies (J-K>2.3) near HDFSubru MOIRCS

Previous wide-field observations with Suprime Cam These are not all the surveys by Subaru

FoV deg2SCamOther wavelengthnotesTeamsSubaru Deep Field*0.25BVRiz,921,816,711,503,497, IBsNIR, MIRdeepest imageswith SubaruObs. Project SDFKashikawa et al.GOODS-N0.05(0.2)BVRiz,497,(921)X, UV,HST,NIR, MIR, FIR, sub-mm, radio world standard fieldOhta et al. / Capak et al. Lockman Hole0.25BVRizX, UV, NIR, MIR, FIR, sub-mm, radiolow HI columnCapak et al.NEP Survey0.25BRizMIR, sub-mm, radioAkari surveyMatsuhara/Hanami et al.EIS0.5BRIzNIRESO fieldArimoto et al.Subaru XMM Deep Field*1.2BVRiz,921,816,711, 503,497, IBsX, UV, NIR, MIR, FIR, sub-mm, radiodeep and wideObs. Project SXDSSekiguchi, et al.COSMOS2griz,921, 816, IBs (21bands)X, UV, HST,NIR, MIR, FIR, sub-mm, radioHST ACS COSMOSCOSMOS / Taniguchi et al.PISCES*clustersBVRizNIR, HST, XSurvey at known clustersKodama et al.SSA22 *3B,V,497NIRz=3.1Hayashino et al. /Yamada et al.SCDXT*(UKIDSS/Scam)9(B),INIR/MIRUKIDSS DXSfieldsYamada et al.33 deg Survey(33)RLensing Miyazaki et al.

c.f., comoving volume sampled by Suprime Cam NB filters

Comoving Volume ( Mpc3 / [unit z] )@ z~1-10Main targets1 deg2~107Galaxy Formation/Evolution10 deg2~108The most luminous objectsClusters, LSS100 deg2~109QuasarsMass Distribution of the Universe1000 deg2~1010BAO, and other precise cosmology

Ly RedshiftV (comoving)NB497Z=3.17x105 Mpc3/deg2NB711Z=4.97x105 Mpc3/deg2NB921Z=6.61x106 Mpc3/deg2

Previous wide-field observations with Subaru

FoVSCamOther wavelengthnotesTeamsSubaru Deep Field*0.25BVRiz,921,816,711,503,497, IBsNIR, MIRdeepest imageswith SubaruObs. Project SDFKashikawa et al.GOODS-N0.05(0.2)BVRiz,497,(921)X, UV,HST,NIR, MIR, FIR, sub-mm, radio world standard fieldOhta et al. / Capak et al. Lockman Hole0.25BVRizX, UV, NIR, MIR, FIR, sub-mm, radiolow HI columnCapak et al.NEP Survey0.25BRizMIR, sub-mm, radioAkari surveyMatsuhara/Hanami et al.EIS0.5BRIzNIRESO fieldArimoto et al.Subaru XMM Deep Field*1.2BVRiz,921,816,711, 503,497, IBsX, UV, NIR, MIR, FIR, sub-mm, radiodeep and wideObs. Project SXDSSekiguchi, et al.COSMOS2griz,921, 816, IBs (21bands)X, UV, HST,NIR, MIR, FIR, sub-mm, radioHST ACS COSMOSCOSMOS / Taniguchi et al.PISCES*clustersBVRizNIR, HST, XSurvey at known clustersKodama et al.SSA22 *3B,V,497NIRz=3.1Hayashino et al. /Yamada et al.SCDXT*(UKIDSS/Scam)9(B),INIR/MIRUKIDSS DXSfieldsYamada et al.33 deg Survey(33)RLensing Miyazaki et al.

SDF (deepest) - Unveiling the Re-Ionization Era Kodaira et al. 2003, Taniguchi et al. 2004, Kashikawa et al. 2005Iye et al. 2006 (for the z=6.96 object), Ota et al. 2007 submitted(north, difficult to observe from ALMA)34Subaru Deep FieldNB980

SDFThe deepest search for the highest-redshift objectsSXDSTracing Structure Formation and Galaxy Formation/Evolution

Iye et al. 2006

Witnessing the Re-ionization of the Universe?Haiman 2002Kashikawa et al. 2006

McQuinn et al. 2007Observing Cosmic Reionization by (the clustering of) Ly Emitters average neutral fractionSDF z=6.6

Lyman Break Galaxies at z=3-7 luminosity function and star-formation history clustering Ouchi et al., Yoshida et al., Shimasaku et al., Iwata et al. (GOODS)

z~2 (BzK) galaxies Motohara et al., Kong et al. (EIS)There are also studies about continuum selected objectsYoshida et al. 2006

* TY (at least partially) involved or leadingPrevious wide-field observations with SubaruThese are not all the surveys by Subaru

FoVSCamOther wavelengthnotesTeamsSubaru Deep Field*0.25BVRiz,921,816,711,503,497, IBsNIR, MIRdeepest imageswith SubaruObs. Project SDFKashikawa et al.GOODS-N0.05(0.2)BVRiz,497,(921)X, UV,HST,NIR, MIR, FIR, sub-mm, radio world standard fieldOhta et al. / Capak et al. Lockman Hole0.25BVRizX, UV, NIR, MIR, FIR, sub-mm, radiolow HI columnCapak et al.NEP Survey0.25BRizMIR, sub-mm, radioAkari surveyMatsuhara/Hanami et al.EIS0.5BRIzNIRESO fieldArimoto et al.Subaru XMM Deep Field*1.2BVRiz,921,816,711, 503,497, IBsX, UV, NIR, MIR, FIR, sub-mm, radiodeep and wideObs. Project SXDSSekiguchi, et al.COSMOS2griz,921, 816, IBs (21bands)X, UV, HST,NIR, MIR, FIR, sub-mm, radioHST ACS COSMOSCOSMOS / Taniguchi et al.PISCES*clustersBVRizNIR, HST, XSurvey at known clustersKodama et al.SSA22 *3B,V,497NIRz=3.1Hayashino et al. /Yamada et al.SCDXT*(UKIDSS/Scam)9(B),INIR/MIRUKIDSS DXSfieldsYamada et al.33 deg Survey(33)RLensing Miyazaki et al.

Panoramic Deep Image: Subaru/XMM Deep SurveyGalaxy evolution can be studied in fairly large volume. NIR (UKIDSS UDS), MIR-FIR (SWIRE), radio (VLA), sub-mm (SHADES), etc.1.3

SDFThe deepest search for the highest-redshift objectsSXDSTracing Structure Formation and Galaxy Formation/Evolution

Distribution of Galaxies in SXDS (1)massB-drop LBGs (i

Distribution of Galaxies in SXDS (2)Yamada et al. 2005

Connecting Different Type of Galaxies at different epochby their clustering properties

UKIDSS-UDS + SXDS: K-band LF evolution up to z~2Cirasuolo et al. 2007K_AB

COSMOS Subaru provides the ground-base multi-band dataCOSMOS-21(Taniguchi+)

Broad-BandIntermediate-BandNarrow-bandMassey et al. 2006Taniguchi et al. 2007

Narrow-band Surveysat SDF, SXDS, COSMOS, SSA22.

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

Large-Scale Structure of Lyman Alpha Emitters (1) z=4.9 Shimasaku et al. 2003, 2004z=4.86z=4.79

Large-Scale Structure of Lyman Alpha Emitters (2) z=5.7 z=5.70.05Ouchi et al. 2005, ApJ, 620, L1Clump Av~ 180 km/sM~1x1013Msun

Large-Scale Structure of Lyman Alpha Emitters (3) z=3.1Subaru Narrow-Band Observation of the SSA22 Proto-cluster (z=3.1) regionLy Emitters (LA)Ly AbsorbersLAE average local density2 x 10-17 erg/s/cm2EWobs > 160 283 objectsHayashino et al. 2004Steidel et al. 2000

Some Prospects for HSC / WFMOS era Hyper Suprime Cam: ~2 deg2 [8 x FoV of Scam] (Miyazaki-sans talk)Precision Cosmology favors 1000-10000 deg2 surveys (other many talks in this WS) Broad-Band Imaging (photo-z) + Spectroscopy (z~1, z~3)

Galaxy Deep Surveys deepest ~ 10 deg2 wide and deep ~ 100 deg2 especially for NB survey

Broad-Band, Narrow-Band, maybe Intermediate Band Deep Opt & IR Spectroscopy for the selected objects

Deepest (= highest-z) Survey Strategy Primary Goals: Obtain Comprehensive View of the Re-ionization Era Synergy with ALMA (NAOJ) Thirty-Meter Telescope (Subaru/NAOJ ?) James-Webb Space Telescope ground-base deepest NIR (VISTA/WFCAM/Subaru??) space NIR Very Wide Field Imager Whatre the Desirable Deep Survey Strategies for HSC ?

surveyarea filterstimeUltra Deep 10 deg^2(HSC 5FoV*)g, r, i, z, yNB711, 816, 921, 980BB 10h (AB~27 @ z)NB 10h

Whatre the Desirable Deep Survey Strategies for HSC ?yHSC i-drop z~6 galaxies z-drop z~7 galaxies

HSC+NIR optical-drop z > 8 Ouchi 2005

Re-Ionization Era and Earliest GalaxiesImportant Questions (reionization)

When and How Cosmic Re-ionization Occurred ? LAE luminosity-dependent number-density evolution evolution of luminosity-dependent clustering

What are the source of ionization ? UV-selected objects (LBG) luminosity function, color But the knowledge of escape fraction below Lyman Limit is essential

How reionization affects galaxy formation?

Re-Ionization Era and Earliest GalaxiesImportant Questions (galaxy formation) How galaxy formation proceeds at z=5-10? ALMA .. Dust emission (for brightest objects 100M/yr)) High-J CO? (z~6 maybe detectable z~10 difficult) IR-bright objects near UV-selected sources? TMT/JWST .. redshift identification (relatively rare bright objects AB~25-26) stellar contents metal lines: metallicity, excitation, kinematics AGN signatures

Search for galaxies at z=7-10 (z-drop, y-drop) JWST: wide-field NIR imaging survey? ground-based IR camera : brightest galaxies

Thirty Meter Telescope (Caltech / UC / Canada)

Previous wide-field observations with Subaru Suprime CamThese are not all the surveys by Subaru * TY involved

FoVSCamOther wavelengthnotesTeamsSubaru Deep Field (SDF)*0.25BVRiz,921,816,711,503,497, IBsNIR, MIRdeepest imageswith SubaruObs. Project SDFKashikawa et al.GOODS-N0.05(0.2)BVRiz,497,(921)X, UV,HST,NIR, MIR, FIR, sub-mm, radio world standard fieldOhta et al. / Capak et al. Lockman Hole Deep0.25BVRizX, UV, NIR, MIR, FIR, sub-mm, radiolow HI columnCapak et al.NEP Survey0.25BRizMIR, sub-mm, radioAkari surveyMatsuhara/Hanami et al.EIS0.5BRIzNIRESO fieldArimoto et al.Kong et al.Subaru XMM Deep Survey (SXDS)*1.2BVRiz,921,816,711, 503,497, IBsX, UV, NIR, MIR, FIR, sub-mm, radiodeep and wideObs. Project SXDSSekiguchi, et al.COSMOS2griz,921, 816, IBs (21bands)X, UV, HST,NIR, MIR, FIR, sub-mm, radioHST ACS COSMOSCOSMOS / Taniguchi et al.PISCES*clustersBVRizNIR, HST, XSurvey at known clustersKodama et al.SSA22 *3B,V,497NIRz=3.1Hayashino et al. /Yamada et al.SCDXT*(UKIDSS/Scam)9(B),INIR/MIRUKIDSS DXSfieldsYamada et al.33 deg Survey(33)RLensing Miyazaki et al.

Two Subaru Very Wide Field Deep Surveys

SCDXT: Suprime Cam/ UKIDSS Deep eXtragalactic Survey (DXS) Ten Square Degrees Survey - search for clusters and proto-clusters at z=1-2 (working report)

- A Proto-cluster at z=3.1 and Galaxy Formation Subaru (Suprime Cam, FOCAS, MOIRCS) / Spitzer / / VLT (VIMOS) / JCMT-SCUBA / XMM / UKIDSS / Chandra

Suprime-Cam/UKIDSS DXS 10 aq.deg. Survey

I~26 UKIDSS DXS J~22 K~21 SWIRE IRAC/MIPS

SCDXT: Field of View Lockman Field and ELAIS N12300000 sources down to I~26 (AB: 25.5 26.0 @ ~90% completeness) Lockman HoleELAIS N1

I-band IRAC [3.6][4.5] Two-Color DiagramModel grid: Bruzual and Charlot z=0-3, Age 0-Tuniv, E(B-V)=0RedshiftedComa-elliptical passive mdels[3.6] < 20.5 sample24um>0.45mJyZ=1.0Z=2.0

Cluster Finding

Distribution of galaxies is converted tothe density map by smoothing with various kernels.(e.g., Gaussian FWHM=45)

Peak finding with the criteria matched with the smoothed scale.

Optical/NIR MOS spectroscopic follow-upBeing proposed MOIRCS / FMOS Lockman holeELAIS N11.0 < z < 1.21.2 < z < 1.41.4 < z < 1.81.0 < z < 1.21.2 < z < 1.41.4 < z < 1.8

LAE average local densitySteidel et al. 2000A Proto-clusrter around SSA22 field a z=3.1 (Steidel et al. 1998)Hayashino et al. 2004Matsuda et al. 2004 Subaru Scam NB 7h

New Very Wide-Field Ly Emitters Survey at SSA22 area2 x 10-17 erg/s/cm2EWobs > 120 Ly Emitters w/ Hayashino, Matsuda, Nakamura, et al.

Estimation of the Large-Scale Over-densityControl fieldsSDF, SXDS,(GOODS-N)Vs.CDM linear theoryVs. False LAE in Millenium SimulationMillenium SimulationOver-density distribution of SF galaxies

Malhotra et sl. 2002; Charlot and Fall 1993Ly Emission Equivalent Width and IMFConstant continuousSF history

solar metallicity

Model ASalpeter IMF x=2.35

Model BTop heavy IMF x=0.5

Ml=1 MsunMu=120 Msun~240EW0 > 240 POPIII ?If constant continuous SFH

SummaryPrevious Subaru Wide-Area Surveys The deepest search for the highest-redshift objects ~ 0.25 deg2 (1 Scam FoV) SDF, others..

Tracing Structure Formation and Galaxy Formation/Evolution ~ 1 deg2 (4 Scam FoV) SXDS, COSMOS, others..

~ 10 deg2 limited band/depth coverage

Future Prospects w/HSC Precision Cosmology favors 1000 deg2 surveys Galaxy Deep Surveys deepest ~ 10 deg2 wide and deep ~ 100 deg2 especially for NB survey