SlideServe
Télécharger Obtenir Pro
Menu
Accueil Pro
Préférences
ApparenceLight Aide et commentaires
© SlideServe · v2026

Panoramic Survey of the Deep Universe

havyn avatar
havyn
55 diapositives · 739 Views · Oct 22, 2014

Panoramic Survey of the Deep Universe. Observing Galaxy Formation at High Redshift. Toru Yamada National Astronomical Observatory of Japan Opt/IR Div., Subaru Telescope. Needs for Panoramic Deep Surveys Subaru/XMM-Newton Deep Survey Extensive Study of Lyα Blobs

#panoramic survey of the deep universe #panoramic survey of the deep universe ppt #powerpoint #presentation
Panoramic Survey of the Deep Universe - slide 1
01 / 55Panoramic Survey of the Deep Universe
1 / 17

Télécharger la présentation

Panoramic Survey of the Deep Universe
Une image / un lien ci-dessous est fourni (tel quel) pour télécharger la présentation

Politique de téléchargement : le contenu du site vous est fourni TEL QUEL pour votre information et votre usage personnel ; il ne peut être vendu, concédé sous licence ni partagé sur d’autres sites sans l’accord de son auteur.Le contenu vous est fourni TEL QUEL, pour votre information et votre usage personnel uniquement. Téléchargez la présentation en cliquant sur ce lien. Lors du téléchargement, si vous ne parvenez pas à télécharger une présentation, l’éditeur a peut-être supprimé le fichier de son serveur.Pendant le téléchargement, si vous ne parvenez pas à obtenir une présentation, le fichier a peut-être été supprimé par l’éditeur.

F I N

Plus de contenu associé

Transcription de la présentation

  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. Needs for Panoramic Deep Surveys • Subaru/XMM-Newton Deep Survey • 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 deg2 Survey * • etc, etc…… * T.Y. involved

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

  5. N-body + Semi-analytic treatment 21 Mpc (Comoving) Blue●Young Gals Red ●Old Gals 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. B&W：mass 　　（CDM） 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). Joerg Colberg and Antonaldo Diaferio http://www.mpa-garching.mpg.de/GIF/ （１９９９）

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

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

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

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

  10. Size of HUDF 3 arcmin x 3 arcmin … 9 arcmin2 Vcomoving (z < 1) ~ 1 x 104 Mpc3(Ω0=0.3:ΩΛ=0.7: H0=70 km/s/Mpc) Vcomoving (z < 2) ~ 4 x 104 Mpc3 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 andMW ) 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. 1.2 deg2 Optical (Subaru) X-ray (XMM-Newton) HUDF SXDS is observed in NIR (UKIDSS UDS), radio (VLA), sub-mm (SHADES), etc.

  14. MB – 5 log h -19.0 -19.5 -20.0 -20.5 -21.0 -21.5 -22.0 -0.1 B-V 0.9 SXDS HDF 141h-1 Mpc 2.5’ GOODS 2x10’x16’ COSMOS SXDS 2 sq. deg z = 3.0 (From Benson et al. 2001) 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) zf=2-10 3900 OPEGs selected Ri’z’ colors to z’=25

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

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

  19. Hamana, TY, et al. Halo Occupation Model bias < Host Mass > Galaxy Density Halo Occupation Number

  20. Preliminary results z = 4 LBGs の クラスタリングと ホスト・ハロー

  21. Statistical fate of z=4 DM halo with2.6x1012 h-1 Msun (calculated using the Extended Press-Schechter model ) Preliminary results T. Hamana, TY, et al.

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

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

  24. Clump ‘A’ Δv~ 180 km/s M~1x1013Msun

  25. Color-Magnitude Diagram for z~1 galaxies Kodama, TY et al. 2004 C-M sequence expected for passive evolution 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. 3. Extensive Study of Lyα Blobs at High Redshift －Large-Scale Structure of Lyα Emitters and Massive Galaxy Formation－

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

  29. Narrow-band imaging (Steidel et al. 2000) 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)

  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 LAB1 LAB2 LABs are mysterious objects… How frequent are they? How they related with galaxy-formation phenomena?

  31. Subaru Narrow-Band Observation of the SSA22 Proto-cluster region Lyα Emitters (LA) • 2 x 10-17erg/s/cm2 • EWobs> 160 Å • ２８３個 HDR Lyα absorbers Hayashino et al. 2004 LAE average local density Steidel et al. 2000

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

  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） 50 Mpc (comoving) • 2 x 10-17erg/s/cm2 • EWobs> 120 Å • Sb1+Sb2 ~600 個 SSA22-Sb1 (Hayashino et al. 2004) ＨＤＲ　（LAE NB497 < 26.0 EW > 120Å）

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

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

  37. 900 kpc2at z=3.1 or, d~30kpc ! • >16 arcsec2 • >7σin isophotal aperture

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

  39. Lyα Excess LAB: origins of the Lyα (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.. Lyαexcess is seen for 14/35 objects (in the apparent flux)

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

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

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

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

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

  45. LABs in the new survey field

  46. LABs in the new survey field

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

  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