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Mapping the Early Universe with Galaxies at z=3-6

Mapping the Early Universe with Galaxies at z=3-6. Cosmic Web Made of 515 Galaxies at z=5.7. Ouchi et al. 2005 ApJ, 620, L1. Masami Ouchi (Space Telescope Science Institute)

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Mapping the Early Universe with Galaxies at z=3-6

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  1. Mapping the Early Universe with Galaxies at z=3-6 Cosmic Web Made of 515 Galaxies at z=5.7 Ouchi et al. 2005 ApJ, 620, L1 Masami Ouchi (Space Telescope Science Institute) for the SXDS Collaboration Kona 2005

  2. Outline • I will report our results for high-z galaxy clustering obtained by the Subaru/XMM-Newton Deep Survey (SXDS). I will show the SXDS data, and highlight 3 results 1) Angular correlation functions of LBGs at z=4 2) Large-scale structures made of Lyα Emitters at z=5.7 3) Forming cluster candidates at z=5.69 and 5.67 • I will introduce our on-going studies with HST, Spitzer, and Gemini data in the GOODS fields

  3. Highly Biased High-z Universe • Dense galaxy concentrations←Understood with DH distribution (+GF bias). • Distribution of high-z galaxies are highly biased against DM (b=3-5 at z=3-5). • How does the large-scale structure of high-z galaxies look like? • How do galaxies relate to dark halos? → Wider & deeper survey is needed. N=1192 8 arcmin Ouchi et al. (2001) Proto-cluster: Redshift spike of Ly break galaxies at z=3.1 (Steidel et al. 1998) r0 and bias of Ly break galaxies with L>L* (Ouchi et al. 2004)

  4. Mapping the high-z UniverseSubaru/XMM Deep Survey (SXDS) SXDS(1.3 deg2) [2h18m00s ,-5o00’00”] • A multi-wavelength survey under the international collaboration • 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 • Subaru Observatory Key Project (Sekiguchi et al. 2004) • BVRiz with Subaru/Suprime-Cam (Furusawa et al. in prep)~5hr/band/pointing • NB530, NB570=25.3, NB816=26.0 • Subaru/FOCAS (Akiyama et al. in Prep.) • VLT/VIMOS (Simpson/ Saito et al. in prep) ~150 Mpc for z=3-6 Very Deep + wide-field images

  5. Comparison of Surveyed Areas: Very Deep Multi-band Surveys (i’~27) COSMOS (2deg2; 1/4-1/5 integration in BVRz) • The best data set for clustering of high-z galaxies SXDS(1.3 deg2) GOODS (0.09 deg2) FDF(0.01deg2) HUDF(0.002deg2) HDF(0.001deg2)

  6. Large High-z Galaxy Samples • Lyman Break Galaxy (LBG) • 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; iz 1 color + no flux in B,V,R) • Lyα Emitter (LAE) • z~3: 332 (NB503<25.2; BRNB 2 colors) • z~4: 175 (NB570<25.0; BRNB 2 colors) • z~6: 515 (NB816<26.0; RiNB 2 colors) • Thanks to the deep & wide field imaging data, we have obtained ~20,000 LBGs and ~1,000 LAEs at z=3.5-6.2 (~x20 times in number on 1 deg2 sky) Red galaxies at z~1 is discussed in Kodama et al. (2004; MNRAS, 350, 1005)

  7. Results of Spectroscopic Follow-up • Part of galaxies in these samples are spectroscopically confirmed. e.g. results in 2003 • 20/16920 for z=4 LBGs • 19/515 for z=5.7 LAEs Part of results (for z=5.7 Lyα emitters) Ouchi et al. 2005, ApJ, 620, L1

  8. Sky Distribution z~4 BRi-LBGs (z=3.5-4.5) Red=bright Blue=intermediate Black=faint Gray=masked regions N=16,920

  9. Sky Distribution z~5 Viz-LBGs (z=4.2-5.2) Red=bright Blue=intermediate Black=faint Gray=masked regions N=2,768

  10. Sky Distribution z~5 Riz-LBGs (z=4.6-5.2) Red=bright Blue=intermediate Black=faint Gray=masked regions N=1,293

  11. Sky Distribution z~6 i-dropouts (z=5.6-6.2) Red=bright Blue=intermediate Gray=masked regions N= 133

  12. Sky Distributionz=3.1 LAEs yellow=LAEs Red =density contour Background: Image N= 332

  13. Sky Distributionz=5.7 LAEs yellow=LAEs Red =density contour Background: Image N= 515

  14. 1. Angular correlation functions of LBGs at z=4

  15. Close Companions of LBGsExample i’ band 10”=350kpc(comoving)

  16. Close companions • Many LBGs have (a) close companion(s). • Npairs~1,385 for 1”<θ<5” i.e, ~10- 40 h70-1kpc (physical) → for more quantitative analysis, we derive the angular correlation function of LBGs at z=4

  17. Definitive Detection of the Transitionfrom One-Halo to Halo-Halo Clustering at z=4 MDH~1011-12Mo Large-scale clustering z~4 1. Small scale excess at θ<~5” →r_vir of dark halos with ~1011-1012 h-1Mo N=16,920 Dark matter (non-linear model) 2. Large-scale bias (@8Mpc) = 3→ ~1011-1012 h-1Mo b=(ωg/ωm)1/2 Small scale clustering

  18. 2. Large-scale structures made of Lyα Emitters at z=5.7

  19. Large-Scale Structures at z=5.7 • - Galaxy concentrations connected with filaments • 10-40 Mpc scale voids • Large-scale structures of LAEs are qualitatively similar to those of present-day Universe. • →Very early formation of filamentary LSSs made of galaxies • The large-scale bias • b=3.4 ±1.8 • (σ20 =0.4 for r=20Mpc) • is comparable to the LBG clustering (b=3-5) z=5.7±0.05 ~40Mpc in line of sight Voids N= 515 Ouchi et al. 2005, ApJ, 620, L1

  20. 3. Forming cluster candidates at z=5.69 and 5.67

  21. Densest concentrations of Lyα Emitters in 1x106Mpc3 concentration A concentration B Ouchi et al. 2005, ApJ, 620, L1 5σ-level excess We made spectroscopic follow-up for densest regions of LAEs (A and B). We have identified two dense concentrations of LAEs. Densest concentrations in the suvey comoving volume→ Progenitors of massive cluster with 1-3x1014Mo?

  22. Dense Concentrations of LAEs at z=5.7:Facts and Implications • Facts: • v~150-180 km/s (→8-10x1012Mo, if virialized) • δ～80 • SFRD(cluster) =130 SFRD(field) • 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

  23. Conclusions • I introduced the SXDS optical data and highlighted 3 results for clustering of galaxies at z=3-6, • Angular correlation functions of LBGs at z=4 Definitive detection of small & large-scale clustering →two pieces of evidence suggests that LBGs residing in a ~1012Mo halo. 2) Large-scale structures made of Lyα Emitters at z=5.7 Detection of filamentary structures with 10-40 Mpc scale voids (large-scale biasb=3.4 ±1.8) → Early formation of filamentary structures of galaxies 3) Forming cluster candidates at z=5.69 and 5.67 Identification of LAE concentrations at z=5.69 and 5.67. Overdensity δ~80, SFR density excess ~ 130 →Intensive galaxy formation takes place at the beginning stage of cluster formation?

  24. Spectroscopic Identificationfor Spitzer/IRAC-bright LBGs in the GOODS-N for the GOODS team

  25. Spectroscopic Identification for Most Massive Galaxies at z=3-6 ACS z’ IRAC(ch1/ch2) Our on-going Project

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