Masami Ouchi (STScI)

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1 Perspectives from the Subaru Wide-Field Deep Survey -- Suprime-Cam+FOCAS to HySuprime+WFMOS -- Cosmic Web Made of 515 Galaxies at z=5.7 Ouchi et al ApJ, 620, L1 Masami Ouchi (STScI) for the SXDS Collaboration

with Suprime-Cam + FOCAS Angular correlation of LBGs at z=3-6

2 Overview Suprime-Cam 1. Highlight clustering results of our on-going wide-field deep survey with Suprime-Cam + FOCAS Angular correlation of LBGs at z=3-6 Large-scale structures/clusters of LAEs at z= Future Prospects for the survey with HyperSuprime + WFMOS 8m-SUBARU

3 Subaru/XMM Deep Survey (SXDS) Field SXDS(1.3 deg 2 ) [2 h 18 m 00 s,-5 o ] ~150 Mpc at z=3-6 Very Deep + wide-field data A multi-wavelength data X-ray:XMM (Watson et al.) UV: GALEX Optical: Subaru (Sekiguchi et al.) NIR: UKIRT (UKDISS[K=25]Almaini et al.) IR: Spitzer/IRAC (Swire: Lonsdale et al.) Sub-mm:SCUBA (SHADES;Dunlop et al.) Sub-mm:BLAST (Hughs et al.) Radio:VLA (Rawlings et al.) (GMRT; Rawlings et al.) The optical data set BVRiz with Subaru/Suprime-Cam (Furusawa et al. in prep)~5hr/band/pointing B 28.2 V 27.2 R NB530, NB570=25.0, NB816=26.0, NB921~25.5 (50% done) Subaru/FOCAS (Akiyama et al. in Prep.) VLT/VIMOS (Simpson/ Saito et al. in prep) i z

4 Comparison of Surveyed Areas: Very Deep Multi-band Surveys (i ~27) SXDS(1.3 deg 2 ) COSMOS complimentary data (2deg 2 ; but ~1/4 exp. time in BVRz) GOODS (0.09 deg 2 ) FDF(0.01deg 2 ) HUDF(0.002deg 2 ) HDF(0.001deg 2 ) Appropriate data for clustering of high-z galaxies

5 High-z Galaxy Samples Lyman Break Galaxy (LBG or dropouts) z~4: 16,920 (i <27.5; BRi 2 colors) z~5: 2,768 (z <26.5; Viz 2 colors + no flux in B) z~5: 1,293 (z <26.5; Riz 2 colors + no flux in B,V) z~6: 133 (z <26.0; i-z>2 + no flux in B,V,R) Ly Emitter (LAE) z=3.1: 356 (NB503<25.3; BVNB 2 colors) z=3.7: 101 (NB570<24.7; BVNB 2 colors) z=5.7: 515 (NB816<26.0; RiNB 2 colors+ no flux in BV) z=6.6: % of data obtained this fall --- (Goal: 5xSDF) Thanks to the deep & wide field imaging data, we have obtained ~20,000 LBGs and ~1,000 LAEs at z= (6.6) (~x10 times in number on 1 deg 2 sky )

6 Results of Spectroscopic Follow-up Part of galaxies in these samples are spectroscopically confirmed. e.g. 19/515 for z=5.7 LAEs spectroscopic obs. continue Part of results (for z=5.7 Ly emitters) Ouchi et al. 2005, ApJ, 620, L1

7 Sky Distribution z~4 BRi-LBGs (z= ) N=16,920 Red=bright Blue=intermediate Black=faint Gray=masked regions

8 Sky Distribution z~5 Viz-LBGs (z= ) N=2,768 Red=bright Blue=intermediate Black=faint Gray=masked regions

9 Sky Distribution z~5 Riz-LBGs (z= ) N=1,293 Red=bright Blue=intermediate Black=faint Gray=masked regions

10 Sky Distribution z~6 i-dropouts (z= ) N= 133 Red=bright Blue=intermediate Gray=masked regions

11 Sky Distribution z~3 Ly Emitters Red=bright Blue=intermediate Gray=masked regions

12 Sky Distribution z~4 Ly Emitters Red=bright Blue=intermediate Gray=masked regions

13 Sky Distribution z~6 Ly Emitters Red=bright Blue=intermediate Gray=masked regions

14 Close Companions z=4 LBGs : example i band 10 =70kpc (physical)

15 i ) Angular Correlation Functions of LBGs at z=4-6

16 Angular Correlation Function of z=4 LBGs Dark Matter

17 Angular Correlation Function of z=4 LBGs Dark Matter

18 Angular Correlation Function of z=4 LBGs Dark Matter

19 Angular Correlation Function of z=4 LBGs Dark Matter

20 Angular Correlation Function of z=4 LBGs Dark Matter

21 Definitive Identification of the Transition between Small and Large Scale Clustering 1. Small scale excess at <~7 r_vir of dark halos with ~ h -1 Mo z~4 N=16,920 Large-scale clustering M DH ~ Mo Approach to Dark Side of Galaxy Formation Dark matter 2. Large-scale bias (@8Mpc) = 3 ~ h -1 Mo Small scale clustering Ouchi et al. 2005, submitted to ApJ (astro-ph/ )

22 Fitting the CDM model to ( ) and number density z=4 z=5 z=6

23 Mass of Hosting Dark Halos And their evolution at z=4-6 Hosting halo mass decreases from z=4 to 6. what does it mean?? UV luminosity (SFR) increases at higher-z for the given hosting halo mass. z=4 z=5 z=6 Active star-formation can be triggered in less massive halos at earlier epoch This may explain the antihierarchical behavior of star formation history?(i.e. Numerous less massive halos finish convert gas into stars at early epoch.) M uv (AB) ~SFR bright

24 ii ) Clustering of Ly Emitters at z=5.7

25 Sky Distribution of Ly Emitters shows individual structures For LBGs, individual clustering properties are erased by the wide-redshift selection window ( z~1 400Mpc: 2D distribution) Ly Emitters (LAEs) are selected in a slice of universe ( z~0.1 40Mpc: 2.5D distribution) Ideal for studying properties of individual structures Narrow-band selection ( z<0.1) LBG selection ( z=1) observer z=3 z=4 z=5

26 Large-Scale Structures at z=5.7 - Galaxy concentrations connected with filaments Mpc scale voids Large-scale structures of LAEs are qualitatively similar to those of present-day Universe. Voids z=5.7± 0.05 N= 515 ~40Mpc in line of sight Very early formation of filamentary LSSs made of galaxies The large-scale bias b=3.4 ±1.8 is comparable to the LBG clustering (b=3-5) Ouchi et al. 2005, ApJ, 620, L1

27 Densest concentrations of Ly Emitters in 1x10 6 Mpc 3 concentration B concentration A 5 -level excess Ouchi et al. 2005, ApJ, 620, L1 We made spectroscopic follow-up for densest regions of LAEs (A and B). We have identified two dense concentrations of LAEs. Densest concentrations in th suveyed comoving volume Progenitors of massive cluster with 1-3x10 14 Mo?

28 Dense Concentrations of LAEs at z=5.7: Facts: v~ km/s ( 8-10x10 12 Mo, if virialized) 80 SFRD(cluster) ~130 SFRD(field) Facts and Implications Implications: If these are ancestors of today s massive clusters, the beginning stage of formation of cluster/cluster core whose members will become subsequently old ellipticals Forming cluster candidates Intensive galaxy formation takes place at a specific place of the high-z Universe? Significant contribution to reionization?? 1 Mpc at z=5.69 Close-up view of the concentration A SXDF/FCC-A: Forming Cluster Candidate at z=5.69

29 Future Prospects for the Survey with HySuprime & WFMOS

30 Precision Measurements of Correlation Function For very high-z galaxies (z>5), more accuracy for small-scale CF Galaxy distribution follow the halo profile? (e.g. NFW for high-z galaxy distribution??) HySPCAM+WFMOS profil e + DH mass Where galaxy formation is triggered in a DH?

31 High-z Star-Formaing Cluster Search Mass function z=6 z=0 1/V s A few high-z clusters made of SF galaxies are found. HySPCAM+WFMOS A number of high-z clusters with mass. Mass function of SF galaxy clusters cluster evolution

32 Luminosity Function of High-z Galaxies Color Selected Sample (LBG) v.s. Spectroscopic Sample We may miss a large fraction of high-z galaxies with a color-selected sample Classical magnitude-limit spectroscopic survey (Le Fevre et al. 2005). WFMOS + HySPCAM rough pre-selection with color magnitude-limit like spectroscopic survey for high-z galaxies Conclude luminosity function at z=3-7 Le Fevre et al Color selection misses galaxies by a factor of two or more??

33 Narrow-band selected z=3.1±0.03 objects for 1 hour(5 ) for NB imaging ~1 hour for spectroscopy Ouchi et al. in prep BAO survey?? Pros: Success rate of spectroscopy ~100% with Ly by ~1 hour exp. Cons: NB=25.0 (5 : 1 hr) = 200 objects/deg 2 (Not dense enough for WFMOS) Redshifts of Ly may be messy ).

Extended Ly Sources Un, NB497, NBcorr, BV, R Volume limit of SPCAM search Saito et al., 2005, Submitted to ApJ (in SXDS field) Matsuda et al. 2004, ApJ, 128, 569 SSA22 field (in Steidel s z=3.

34 Extended Ly Sources Un, NB497, NBcorr, BV, R Volume limit of SPCAM search Saito et al., 2005, Submitted to ApJ (in SXDS field) Matsuda et al. 2004, ApJ, 128, 569 SSA22 field (in Steidel s z=3.1 cluster) Extended Ly Sources (cooling cloud??) are quite rare (n~10-5 Mpc). HySPCAM (+WFMOS) Statistical number of extended Ly sources. Unveiling the nature of extended Ly sources with a statistical number of sample

35 Summary 1. Highlight some results of our on-going wide-field deep survey Angular correlation of LBGs Definitive detection of small & large-scale clustering multiple LBGs residing in a ~ Mo halo. Hosting Halo mass decreases from z=4 to 6. Active star-formation can be triggerd in less massive halos at earlier epoch? Large-scale strucutres of LAEs Detection of filamentary structures with Mpc scale voids (large-scale bias b=3.4 ±1.8) Early formation of filamentary structures of galaxies Identification of LAE concentrations at z=5.69 and Overdensity ~80, SFR density excess ~ 130 Intensive galaxy formation takes place at the beginning stage of cluster formation? Significant contribution to reionization?? 2. Future Prospects for the survey with HyperSuprime + WFMOS - CF of high-z galaxies Relation between galaxy formation and structure formation (DH). - High-z star-forming cluster search Cluster evolution - Precise Luminosity functions with spectroscopic sample Most basic measurements to understand galaxy formation - Systematic extended Ly source search Nature of unknown objects

Discovery of Primeval Large-Scale Structures with Forming Clusters at Redshift z=5.7

Discovery of Primeval Large-Scale Structures with Forming Clusters at Redshift z=5.7 Sadanori Okamura Department of Astronomy, and Research Center for the Early Universe, University of Tokyo Collaborators