1. Panoramic Survey of the Deep Universe Observing Galaxy Formation at High Redshift Toru Yamada National Astronomical Observatory of Japan Opt/IR Div., Subaru Telescope

2. 1.Needs for Panoramic Deep Surveys 2.Subaru/XMM-Newton Deep Survey 3.Extensive Study of Lyα Blobs and High Redshift Large-Scale Structure

3. 1. Panoramic Deep Surveys - Subaru Deep Field Surveys * - Subaru/XMM-Newton Deep Survey * - EIS+Subaru Survey - COSMOS - NEP Deep Survey (+Astro-F) - SSA22 Emission Line Galaxy Survey * -UKIDSS-DXS/Scam 10 deg 2 Survey * etc, etc…… * T.Y. involved

4. Cosmic Microwave Background measured by WMAP age of the Universe: 380 kyrs

5. B&W ： mass （ CDM ） Joerg Colberg and Antonaldo Diaferio http://www.mpa-garching.mpg.de/GIF/ 21 Mpc (Comoving) Early (massive) galaxy formation preferentially occurs in the region of large-scale density peaks which will evolve to massive clusters. → Cluster galaxies are old → Spatial distribution of high-z galaxies is much inhomogeneous than that of mass. Galaxy Formation occurs in the ‘Biased’ manner due to the collapse of ‘high peak’ of CDM fluctuation and some local physical processes (Feedback; UV/Xray heating, Super-galactic wind). Blue● Young Gals Red ● Old Gals （１９９９） N-body + Semi-analytic treatment

6. z=3 simulation at larger scale (Benson et al. 2001) B&W :CDM Colord: Galaxies 141 h -1 Mpc N-body + semi-analytic treatment

7. Two-Point Correlation Function of ~6000 z~4 ‘B-drop’ Lyman Break Galaxies In the Subaru SXDS Field Strong clustering of high-z Star-Forming galaxies = bias to the mass (Steidel et al. 1998. Adelberger et al. 1999) bias mass galaxies at high-z large scale (~10 Mpc), bias is likely to be treated as ‘linear bias’, σ g =b σ

8. Whole picture of structure formation Events with shorter time scale (e.g., QSO) Rare objects ＋ High Statistical Accuracy Deep Imaging of High-z Universe Pencil-Beam Surveys are not sufficient. Panoramic Surveys over large comoving volume are needed.

9. Deepest Image of the Universe we have: Hubble Ultra Deep Field (2004) 3’ ACS F435W (B) F606W (V) F775W (I) F840LP (z)

10. Size of HUDF 3 arcmin x 3 arcmin … 9 arcmin 2 V comoving (z < 1) ~ 1 x 10 4 Mpc 3 (Ω 0 =0.3:Ω Λ =0.7: H 0 =70 km/s/Mpc) V comoving (z < 2) ~ 4 x 10 4 Mpc 3 Local Universe φ* = 5 x 10 -3 Mpc -3 (SDSS, r*) If uniform, ~200 L* or brighter galaxies at z~2 /unit redshift Physical dimension~ 1 - 1.5 Mpc （ Just twice of the distance between M31 and MW ) M31 d=0.7 Mpc

11. From STScI HUDF web page

12. 2. Subaru/XMM-Newton Deep Survey an example of deep panoramic survey in multi wavelength

13. Subaru/XMM-Newton Deep Survey (SXDS) Galaxy evolution can be studied in sufficiently large volume. Optical (Subaru)X-ray (XMM-Newton) 1.2 deg 2 SXDS is observed in NIR (UKIDSS UDS), radio (VLA), sub-mm (SHADES), etc. HUDF

14. (From Benson et al. 2001) 141h -1 Mpc z = 3.0 B-V -0.10.9 -22.0-21.5-21.0-20.5-20.0-19.5 -19.0 M B – 5 log h GOODS COSMOS SXDS HDF 2x10’x16’ 2 sq. deg 2.5’ SXDS thin slice

15. z~4 Star-Forming Galaxies in SXDS B-Drop Lyman Break Galaxies ~6000 B-drop LBGs ● i < 24 ● 24 < i ’ < 25 ● 25 < i ’ < 26

16. z~1 Evolved Quiescent Galaxies Old Passively-Evolving Galaxies (OPEGs) z f =2-10 3900 OPEGs selected Ri’z’ colors to z’=25

17. z=4 z=1 1 < z < 4 Dark Matter Halo Lyman Beake Galaxies gas OPEGs ダークマターハロー Z>4

18. Two-Point Correlation Function of ~6000 z~4 ‘B-drop’ Lyman Break Galaxies In the Subaru SXDS Field Strong clustering of high-z Star-Forming galaxies = bias to the mass (Steidel et al. 1998. Adelberger et al. 1999) bias mass galaxies at high-z large scale (~10 Mpc), bias is likely to be treated as ‘linear bias’, σ g =b σ Preliminary results

19. bias Halo Occupation Model Galaxy Density Halo Occupation Number Hamana, TY, et al.

20. z = 4 LBGs の クラスタリングと ホスト・ハロー M min 1x10 12 M sun 2.6x10 12 M sun M 1 3x10 11 M sun Preliminary results

21. Statistical fate of z=4 DM halo with 2.6x10 12 h -1 M sun (calculated using the Extended Press-Schechter model ) T. Hamana, TY, et al. Preliminary results

22. Our Results Solid line ： Halo mass growth curve In CDM Dashed lines ： 68% interval Average host halo mass of galaxies obtained from their clustering properties z~4 LBGs z~1 OPEGs Preliminary results

23. Discovery of the two ‘seed’ clusters in SXDS (Ouchi et al. 2005) Deep NB816 Narrow-Band Survey (8160 Å, for z=5.7 Lyαemitters)

24. Clump ‘A’ Δv~ 180 km/s M~1x10 13 M sun

25. C-M sequence expected for passive evolution Kodama, TY et al. 2004 Color-Magnitude Diagram for z~1 galaxies 1.2 度

26. Galaxy Color Evolution in HDF-N (Kajisawa and Yamada 2004) Results obtained with a pencil-beam survey  EXTEND TO SXDS !

27. － Large-Scale Structure of Lyα Emitters and Massive Galaxy Formation － 3. Extensive Study of Lyα Blobs at High Redshift

28. B&W :CDM Colored: Galaxies 141 h -1 Mpc N-body + semi-analytic treatment z~3 simulation

29. SSA22 Proto-cluster at z=3.1 Discovery of the SSA22 proto-cluster of Lyman Break Galaxies at z=3.1 (Steidel et al. 1998) Narrow-band imaging (Steidel et al. 2000)

30. Extended LyαEmitters: Lyα Blobs (LABs)  Giant LyαEmission-Line Nebulae > 100 kpc (physical scale) (Steidel et al. 1998, Keel et al. 1999)  Internal velocity structure Δv>1000 km/s (Ohyama et al. 2004, Bower et al. 2004)  Not enough UV by the apparent SFR  4 previous examples of LAB with > 100 kpc at z=2~3 are all in the high density regions of LAE LABs are mysterious objects… How frequent are they? How they related with galaxy-formation phenomena? LAB1 LAB2

31. Subaru Narrow-Band Observation of the SSA22 Proto-cluster region Lyα Emitters (LA) Lyα absorbers LAE average local density  2 x 10 -17 erg/s/cm 2  EWobs > 160 Å  ２８３個 Hayashino et al. 2004 Steidel et al. 2000 HDR

32. Redshift Distribution of LAEs Redshift LAEs LAB1, LAB2 Obs: Subaru FOCAS 56 objects

33. LAEs z=3.05-3.08 z=3.08-3.10 z=3.10-3.12 giant Lyα blob

34. LAE survey: extension to the North-West area SSA22-Sb2 （２００４年８月） SSA22-Sb1 (Hayashino et al. 2004) 50 Mpc (comoving) ＨＤＲ （ LAE NB497 120 Å）  2 x 10 -17 erg/s/cm 2  EWobs > 120 Å  Sb1+Sb2 ~600 個

35. Lyα image (after continuum subtraction) z=3.1 LBG 25” = 190 kpc sub-mm / CO source (before subtraction) B, V, NB. Lyα= green Cont. subtracted image Subaru 7h image of LAB1 How ordinary these gigantic LABs are ? What are their size, luminosity, and spatial distribution?

36. 25 ” or 190 kpc at z = 3.1 35 個の Lyα Blobs (Matsuda et al. 2004) First large sample of LABs

37.  >16 arcsec 2  >7σ in isophotal aperture or, d~30kpc ! 900 kpc 2 at z=3.1

38. Sky distribution ： 35 LABs （ ■ ） and LAEs （ ● ）

39. Lyαexcess is seen for 14/35 objects (in the apparent flux) LAB: origins of the Lyα Lyα Excess (1) Photoionization by massive stars or by AGN (in some cases … may be hidden by dust) by diffuse background UV ? (2) Atomic cooling radiation (early phase of galaxy formation) (3) Superwind (late phase of intense star formation) Plus, scattering..

40. Hidden star formation/AGN ?? 25” =190 kpc Lyαpeak Cont. ? Lyα peak is displaced from the continuum peak

41. Superwind ? Cooling flow ? Also see Ohyama et al. 2003, Bower et al. 2004 25” =190 kpc

42. Atomic cooling emission from a proto galaxy ?? - Diffuse morphology - No plausible continuum source 25” =190 kpc Turned out to be associated with X-ray (XMM) and sub-mm source

43. Results of SCUBA sub-mm observations w/ Smail, Chapman, et al. LAB1 LAB18 (XMM source!) LAB14 … detected in Barger et al., Chapman et al. 2004 so to be confirmed c.f., Lyman Break 銀河・・・検出率５％以下

44. 53W002 No.18 LAB … Keel et al. (1999) SCUBA Source SMM 02399-0136 (z=2.8) Detected in Sub-mm observation (Smail et al. 2003) 10” Lyα Lyα+cont Lyα NVNV LyαHalo Slit direction wavelength LABs in Matsuda et al.

45. LABs in the new survey field

47. A New Gigantic LAB with > 100 kpc in SSA22-Sb2 fielfd, which is comparable with LAB1, LAB2 in the SSA22-Sb1 field 25”=190 kpc 2005/08 3D spextroscopy with VLT VIMOS Matsuda et al. LABs in the new survey field

48. Slit spectroscopy of LABs with Keck DEIMOS

49. Relatively compact Lyα emitters Δv < 500 km/s

50. Lyα Blobs : many have Δv > 500 km/s, absorption

51. [Gaussian fit σ] LAB 16 sq.arcsec … d~30 kpc FWHM~500 km/s Slit spectroscopy of LABs with Keck DEIMOS

52. 1. (Lower limit of) their mass can be evaluated from their size, assuming that they are collapsed objects (before z=3.1), if we apply the spherical collapse model. M vir = 4/3πR vir 3 ρ crit (z) Δ c (z) > 4x10 10 (R Lyα / 26kpc) 3 M sun 2. Assuming that they are bounded objects, their mass can be evaluated from their size and internal velocity M dyn ~10 12-13 M sun 3. Strong clustering  associated with more massive DM halos ? 4. Possibly higher sub-mm detection rate (massive SF) Mass of the LABs Massive Galaxies in Their Forming Phase Large Lyα Luminosity, Extension, Clustering, High sub-mm ditection rate

53. Summary 1.Deep Panoramic Surveys probe the universe 2.Galaxy evolutions are being studied in large-volume, highly statistically accurate sample of the SXDS galaxies - connection between z~4 LBGs and z~1 OPEGs - seed cluster at z=5.7 discovered in the NB search - nature of the optically-faint X-ray sources - mass dependency of galaxy evolution 3.We discovered ~100 Mpc LSS of LAE at z~3.1. LyαBlobs, candidates of massive forming galaxies are distributed along the LSS.

54. Future Prospects SCam / UKIDSS DXS 10 deg2 survey ELAIS N1 Lockman Hole Extension of z~3 LSS and LAB/LAA/LAE search Covered by UKIDSS DXS SWIRE IRAC(blue) MIPS(red) Scam(white)

55. Future Prospects Subaru New NIR Camera and Spectrograph “MOIRCS” A New Mission Hubble Origins Probe Very Wide Field Imager 4’x7’ GOODS-N