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Wide-field Surveys with Subaru Toru 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 4’x7’ Distribution of Distant Red Galaxies (J-K>2.3) near HDF 7 arcmin Subru MOIRCS Kajisawa et al. 2006 Previous wide-field observations with Suprime Cam FoV deg2 SCam Other wavelength notes Teams Subaru Deep Field* 0.25 BVRiz,921,816,71 1,503,497, IBs NIR, MIR deepest images with Subaru Obs. Project SDF Kashikawa et al. GOODS-N 0.05 (0.2) BVRiz,497,(921) X, UV,HST,NIR, MIR, FIR, sub-mm, radio world standard field Ohta et al. / Capak et al. 他 Lockman Hole 0.25 BVRiz X, UV, NIR, MIR, FIR, sub-mm, radio low HI column Capak et al. NEP Survey 0.25 BRiz MIR, sub-mm, radio Akari survey Matsuhara/Hanami et al. EIS 0.5 BRIz NIR ESO field Arimoto et al. Subaru XMM Deep Field* 1.2 BVRiz,921,816,71 1, 503,497, IBs X, UV, NIR, MIR, FIR, sub-mm, radio deep and wide Obs. Project SXDS Sekiguchi, et al. COSMOS 2 griz,921, 816, IBs (21bands) X, UV, HST,NIR, MIR, FIR, sub-mm, radio HST ACS COSMOS COSMOS / Taniguchi et al. PISCES* clusters BVRiz NIR, HST, X Survey at known clusters Kodama et al. SSA22 * 3 B,V,497’ NIR z=3.1 Hayashino et al. / Yamada et al. SCDXT* (UKIDSS/Scam) 9 (B),I NIR/MIR UKIDSS DXS fields Yamada et al. 33 deg Survey (33) R Lensing Miyazaki et al. These are not all the surveys by Subaru Comoving Volume ( Mpc3 / [unit z] ) @ z~1-10 Main targets 1 deg2 ~107 Galaxy Formation/Evolution 10 deg2 ~108 The most luminous objects Clusters, LSS 100 deg2 ~109 Quasars Mass Distribution of the Universe 1000 deg2 ~1010 BAO, and other precise cosmology c.f., comoving volume sampled by Suprime Cam NB filters Lyα Redshift V (comoving) NB497 Z=3.1 7x105 Mpc3/deg2 NB711 Z=4.9 7x105 Mpc3/deg2 NB921 Z=6.6 1x106 Mpc3/deg2 Previous wide-field observations with Subaru FoV SCam Other wavelength notes Teams Subaru Deep Field* 0.25 BVRiz,921,816,71 1,503,497, IBs NIR, MIR deepest images with Subaru Obs. Project SDF Kashikawa et al. GOODS-N 0.05 (0.2) BVRiz,497,(921) X, UV,HST,NIR, MIR, FIR, sub-mm, radio world standard field Ohta et al. / Capak et al. 他 Lockman Hole 0.25 BVRiz X, UV, NIR, MIR, FIR, sub-mm, radio low HI column Capak et al. NEP Survey 0.25 BRiz MIR, sub-mm, radio Akari survey Matsuhara/Hanami et al. EIS 0.5 BRIz NIR ESO field Arimoto et al. Subaru XMM Deep Field* 1.2 BVRiz,921,816,71 1, 503,497, IBs X, UV, NIR, MIR, FIR, sub-mm, radio deep and wide Obs. Project SXDS Sekiguchi, et al. COSMOS 2 griz,921, 816, IBs (21bands) X, UV, HST,NIR, MIR, FIR, sub-mm, radio HST ACS COSMOS COSMOS / Taniguchi et al. PISCES* clusters BVRiz NIR, HST, X Survey at known clusters Kodama et al. SSA22 * 3 B,V,497’ NIR z=3.1 Hayashino et al. / Yamada et al. SCDXT* (UKIDSS/Scam) 9 (B),I NIR/MIR UKIDSS DXS fields Yamada et al. 33 deg Survey (33) R Lensing Miyazaki et al. SDF (deepest) - Unveiling the Re-Ionization Era Subaru Deep Field NB980 34’ (north, difficult to observe from ALMA) Kodaira et al. 2003, Taniguchi et al. 2004, Kashikawa et al. 2005 Iye et al. 2006 (for the z=6.96 object), Ota et al. 2007 submitted SDF The deepest search for the highest-redshift objects SXDS Tracing Structure Formation and Galaxy Formation/Evolution Iye et al. 2006 Witnessing the Re-ionization of the Universe? Kashikawa et al. 2006 Haiman 2002 Observing Cosmic Reionization by (the clustering of) Lyα Emitters average neutral fraction SDF z=6.6 McQuinn et al. 2007 There are also studies about continuum selected objects - 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) Yoshida et al. 2006 - z~2 (BzK) galaxies Motohara et al., Kong et al. (EIS) Previous wide-field observations with Subaru FoV SCam Other wavelength notes Teams Subaru Deep Field* 0.25 BVRiz,921,816,71 1,503,497, IBs NIR, MIR deepest images with Subaru Obs. Project SDF Kashikawa et al. GOODS-N 0.05 (0.2) BVRiz,497,(921) X, UV,HST,NIR, MIR, FIR, sub-mm, radio world standard field Ohta et al. / Capak et al. 他 Lockman Hole 0.25 BVRiz X, UV, NIR, MIR, FIR, sub-mm, radio low HI column Capak et al. NEP Survey 0.25 BRiz MIR, sub-mm, radio Akari survey Matsuhara/Hanami et al. EIS 0.5 BRIz NIR ESO field Arimoto et al. Subaru XMM Deep Field* 1.2 BVRiz,921,816,71 1, 503,497, IBs X, UV, NIR, MIR, FIR, sub-mm, radio deep and wide Obs. Project SXDS Sekiguchi, et al. COSMOS 2 griz,921, 816, IBs (21bands) X, UV, HST,NIR, MIR, FIR, sub-mm, radio HST ACS COSMOS COSMOS / Taniguchi et al. PISCES* clusters BVRiz NIR, HST, X Survey at known clusters Kodama et al. SSA22 * 3 B,V,497’ NIR z=3.1 Hayashino et al. / Yamada et al. SCDXT* (UKIDSS/Scam) 9 (B),I NIR/MIR UKIDSS DXS fields Yamada et al. 33 deg Survey (33) R Lensing Miyazaki et al. * TY (at least partially) involved or leading These are not all the surveys by Subaru Panoramic Deep Image: Subaru/XMM Deep Survey Galaxy evolution can be studied in fairly large volume. 1.3° UKIDSS UDS K<23 (Vega) NIR (UKIDSS UDS), MIR-FIR (SWIRE), radio (VLA), sub-mm (SHADES), etc. SDF The deepest search for the highest-redshift objects SXDS Tracing Structure Formation and Galaxy Formation/Evolution Distribution of Galaxies in SXDS (1) MDH~1012Mo B-drop LBGs (i<27) mass Small scale clustering Ouchi et al. 2005 Distribution of Galaxies in SXDS (2) ＳＤＳＳ Red galaxies z=0 SDSS Morphological E/S0 (Nakamura et al.) Passive Evolution zf=3 and 5 Yamada et al. 2005 Connecting Different Type of Galaxies at different epoch by their clustering properties UKIDSS-UDS + SXDS: K-band LF evolution up to z~2 Cirasuolo et al. 2007 K_AB<22.5 22000 sources (0.6 deg^2) Number density evolution of red and blue bright objects COSMOS – Subaru provides the ground-base multi-band data Massey et al. 2006 Taniguchi et al. 2007 COSMOS-21 (Taniguchi+) Broad-Band Intermediate-Band Narrow-band Narrow-band Surveys at SDF, SXDS, COSMOS, SSA22…. 141 h-1 Mpc z=3 simulation at larger scale (Benson et al. 2001) N-body + semi-analytic treatment B&W :CDM Colord: Galaxies Large-Scale Structure of Lyman Alpha Emitters (1) z=4.9 z=4.79 z=4.86 Shimasaku et al. 2003, 2004 Large-Scale Structure of Lyman Alpha Emitters (2) z=5.7 z=5.7±0.05 Clump ‘A’ Δv~ 180 km/s M~1x1013Msun Ouchi et al. 2005, ApJ, 620, L1 Large-Scale Structure of Lyman Alpha Emitters (3) z=3.1 Subaru Narrow-Band Observation of the SSA22 Proto-cluster (z=3.1) region Lyα Emitters (LA) 2 x 10-17 erg/s/cm2 EWobs > 160 Å 283 objects Lyα Absorbers HDR LAB2 LAE average local density LAB1 Steidel et al. 2000 Hayashino et al. 2004 Some Prospects for HSC / WFMOS era Hyper Suprime Cam: ~2 deg2 [8 x FoV of Scam] (Miyazaki-san’s 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 What’re the Desirable “Deep” Survey Strategies for HSC ? “Deepest (= highest-z) Survey” Strategy survey area filters time Ultra Deep 10 deg^2 (HSC 5FoV*) g, r, i, z, y NB711, 816, 921, 980 BB 10h (AB~27 @ z) NB 10h - 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 What’re the Desirable “Deep” Survey Strategies for HSC ? y HSC i-drop z~6 galaxies z-drop z~7 galaxies HSC+NIR optical-drop z > 8 Ouchi 2005 Re-Ionization Era and Earliest Galaxies Important 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 Galaxies Important 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 Cam FoV SCam Other wavelength notes Teams Subaru Deep Field (SDF)* 0.25 BVRiz,921,816,7 11,503,497, IBs NIR, MIR deepest images with Subaru Obs. Project SDF Kashikawa et al. GOODS-N 0.05 (0.2) BVRiz,497,(921) X, UV,HST,NIR, MIR, FIR, submm, radio world standard field Ohta et al. / Capak et al. 他 Lockman Hole Deep 0.25 BVRiz X, UV, NIR, MIR, FIR, sub-mm, radio low HI column Capak et al. NEP Survey 0.25 BRiz MIR, sub-mm, radio Akari survey Matsuhara/Hanami et al. EIS 0.5 BRIz NIR ESO field Arimoto et al. Kong et al. Subaru XMM Deep Survey (SXDS)* 1.2 BVRiz,921,816,7 11, 503,497, IBs X, UV, NIR, MIR, FIR, sub-mm, radio deep and wide Obs. Project SXDS Sekiguchi, et al. COSMOS 2 griz,921, 816, IBs (21bands) X, UV, HST,NIR, MIR, FIR, submm, radio HST ACS COSMOS COSMOS / Taniguchi et al. PISCES* clusters BVRiz NIR, HST, X Survey at known clusters Kodama et al. SSA22 * 3 B,V,497’ NIR z=3.1 Hayashino et al. / Yamada et al. SCDXT* (UKIDSS/Scam) 9 (B),I NIR/MIR UKIDSS DXS fields Yamada et al. 33 deg Survey (33) R Lensing Miyazaki et al. * TY involved These are not all the surveys by Subaru 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 N1 Lockman Hole ELAIS N1 2300000 sources down to I’~26 (AB: 25.5 – 26.0 @ ~90% completeness) I’-band – IRAC [3.6][4.5] Two-Color Diagram [3.6] < 20.5 sample Redshifted Coma-elliptical passive mdels Z=2.0 Z=1.0 24um>0.45mJy Model grid: Bruzual and Charlot z=0-3, Age 0-Tuniv, E(B-V)=0 Cluster Finding ELAIS N1 Distribution of galaxies is converted to the density map by smoothing with various kernels. 1.0 < z < 1.2 (e.g., Gaussian FWHM=45”) Peak finding with the criteria matched with the smoothed scale. Optical/NIR MOS spectroscopic follow-up Being proposed MOIRCS / FMOS Lockman hole 1.2 < z < 1.4 1.4 < z < 1.8 1.0 < z < 1.2 1.2 < z < 1.4 1.4 < z < 1.8 A Proto-clusrter around SSA22 field a z=3.1 (Steidel et al. 1998) 25”=190kpc HDR LAB2 LAE average local density LAB1 Steidel et al. 2000 Hayashino et al. 2004 Matsuda et al. 2004 LAB1 Subaru Scam NB 7h LAB2 New Very Wide-Field Lyα Emitters Survey at ‘SSA22’ area 2 x 10-17 erg/s/cm2 w/ Hayashino, Matsuda, Nakamura, et al. Lyα Emitters EWobs > 120 Å Estimation of the Large-Scale Over-density Control fields SDF, SXDS, (GOODS-N) Vs.CDM linear theory Millenium Simulation Over-density distribution of SF galaxies Vs. False LAE in Millenium Simulation Lyα Emission Equivalent Width and IMF Constant continuous SF history １／２０solar metallicity ~240Å Model A Salpeter IMF x=2.35 Model B Top heavy IMF x=0.5 Ml=1 Msun Mu=120 Msun EW0 > 240 Å POPIII ? If constant continuous SFH Malhotra et sl. 2002; Charlot and Fall 1993 Summary Previous 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