Widefield Surveys with Subaru Toru Yamada A Review

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, SSA 22 -NB surveys

MOIRCS 4’x 7’

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 Fo. V deg 2 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, submm, radio world standard field Ohta et al. / Capak et al. 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 (21 bands) X, UV, HST, NIR, MIR, FIR, submm, radio HST ACS COSMOS / Taniguchi et al. PISCES* clusters BVRiz NIR, HST, X Survey at known clusters Kodama et al. SSA 22 * 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. 他 These are not all the surveys by Subaru

Comoving Volume ( Mpc 3 / [unit z] ) @ z~1 -10 Main targets 1 deg 2 ~107 Galaxy Formation/Evolution 10 deg 2 ~108 The most luminous objects Clusters, LSS 100 deg 2 ~109 Quasars Mass Distribution of the Universe 1000 deg 2 ~1010 BAO, and other precise cosmology c. f. , comoving volume sampled by Suprime Cam NB filters Lyα Redshift V (comoving) NB 497 Z=3. 1 7 x 105 Mpc 3/deg 2 NB 711 Z=4. 9 7 x 105 Mpc 3/deg 2 NB 921 Z=6. 6 1 x 106 Mpc 3/deg 2

Previous wide-field observations with Subaru Fo. V 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, submm, radio world standard field Ohta et al. / Capak et al. 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 (21 bands) X, UV, HST, NIR, MIR, FIR, submm, radio HST ACS COSMOS / Taniguchi et al. PISCES* clusters BVRiz NIR, HST, X Survey at known clusters Kodama et al. SSA 22 * 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. 他

SDF (deepest) - Unveiling the Re-Ionization Era Subaru Deep Field NB 980 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 Mc. Quinn et al. 2007

There 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 (Bz. K) galaxies Motohara et al. , Kong et al. (EIS)

Previous wide-field observations with Subaru Fo. V 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, submm, radio world standard field Ohta et al. / Capak et al. 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 (21 bands) X, UV, HST, NIR, MIR, FIR, submm, radio HST ACS COSMOS / Taniguchi et al. PISCES* clusters BVRiz NIR, HST, X Survey at known clusters Kodama et al. SSA 22 * 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 他 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) ing r ste r ge La sc ale MDH~1012 Mo cl u 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/S 0 (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, SSA 22….

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± 0. 05 Clump ‘A’ Δv~ 180 km/s M~1 x 1013 Msun Ouchi et al. 2005, Ap. J, 620, L 1

Large-Scale Structure of Lyman Alpha Emitters (3) z=3. 1 Subaru Narrow-Band Observation of the SSA 22 Proto-cluster (z=3. 1) region Lyα Emitters (LA) Ø 2 x 10 -17 erg/s/cm 2 ØEWobs > 160 Å Ø 283 objects HDR Lyα Absorbers LAB 2 LAE average local density LAB 1 Steidel et al. 2000 Hayashino et al. 2004

Some Prospects for HSC / WFMOS era Hyper Suprime Cam: ~2 deg 2 [8 x Fo. V of Scam] (Miyazaki-san’s talk) -Precision Cosmology favors 1000 -10000 deg 2 surveys (other many talks in this WS…) Broad-Band Imaging (photo-z) + Spectroscopy (z~1, z~3) - Galaxy Deep Surveys 　deepest ~ 10 deg 2　　 wide and deep ~ 100 deg 2 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 5 Fo. V*) g, r, i, z, y NB 711, 816, 921, 980 BB 10 h (AB~27 @ z) NB 10 h - 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 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 100 M/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 Fo. V 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 (21 bands) X, UV, HST, NIR, MIR, FIR, submm, radio HST ACS COSMOS / Taniguchi et al. PISCES* clusters BVRiz NIR, HST, X Survey at known clusters Kodama et al. SSA 22 * 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 e. Xtragalactic 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 N 1 Lockman Hole ELAIS N 1 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 24 um>0. 45 m. Jy Model grid: Bruzual and Charlot z=0 -3, Age 0 -Tuniv, E(B-V)=0

Cluster Finding ELAIS N 1 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 < z < 1. 8 1. 0 < z < 1. 2 < z < 1. 4 < z < 1. 8

A Proto-clusrter around SSA 22 field a z=3. 1 (Steidel et al. 1998) 25”=190 kpc LAE average local density Steidel et al. 2000 Hayashino et al. 2004 Matsuda et al. 2004 LAB 1 Subaru Scam NB 7 h LAB 2

New Very Wide-Field Lyα Emitters Survey at ‘SSA 22’ area Ø 2 x 10 -17 erg/s/cm 2 w/ Hayashino, Matsuda, Nakamura, et al. Lyα Emitters ØEWobs > 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 １／２０ solar metallicity ~240Å Model A Salpeter IMF x=2. 35 Model B Top heavy IMF x=0. 5 　 Ml=1 Msun Mu=120 Msun EW 0 > 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 deg 2 (1 Scam Fo. V) SDF, others. . ★ Tracing Structure Formation and Galaxy Formation/Evolution ~ 1 deg 2 (4 Scam Fo. V) SXDS, COSMOS, others. . ★　~ 10 deg 2 limited band/depth coverage Future Prospects w/HSC Precision Cosmology favors 1000 deg 2 surveys Galaxy Deep Surveys 　deepest ~ 10 deg 2　　 wide and deep ~ 100 deg 2 especially for NB survey