Panoramic Survey of the Deep Universe

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

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1. Panoramic Deep Surveys

• - Subaru Deep Field Surveys
• - Subaru/XMM-Newton Deep Survey
• - EISSubaru Survey
• - COSMOS
• NEP Deep Survey (Astro-F)
• SSA22 Emission Line Galaxy Survey
• UKIDSS-DXS/Scam 10 deg2 Survey
• etc, etc

T.Y. involved
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Cosmic Microwave Background measured by WMAP
age of the Universe 380 kyrs
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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.
BWmass (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)
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z3 simulation at larger scale (Benson et al.
2001)
141 h-1 Mpc
N-body semi-analytic treatment
BW CDM Colord Galaxies
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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 z4
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, sgb s
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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
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ACS F435W (B) F606W (V) F775W (I) F840LP (z)
Deepest Image of the Universe we have Hubble
Ultra Deep Field (2004)
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3 arcmin x 3 arcmin 9 arcmin2 Vcomoving
(z lt 1) 1 x 104 Mpc3 (O00.3O?0.7 H070
km/s/Mpc) Vcomoving (z lt 2) 4 x 104 Mpc3
Local Universe f 5 x 10-3 Mpc-3 (SDSS, r)
If uniform, 200 L or brighter galaxies at z2
/unit redshift Physical dimension 1 - 1.5 Mpc
(Just twice of the distance between M31 and MW )
M31 d0.7 Mpc
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From STScI HUDF web page
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2. Subaru/XMM-Newton Deep Survey an example of
deep panoramic survey in multi wavelength
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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.
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MB 5 log h
-19.0
-22.0
-21.5
-21.0
-20.5
-20.0
-19.5
B-V
-0.1
0.9
SXDS
HDF
141h-1 Mpc
2.5
GOODS
2x10x16
COSMOS
SXDS
2 sq. deg
z 3.0
(From Benson et al. 2001)
thin slice
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z4 Star-Forming Galaxies in SXDS B-Drop Lyman
Break Galaxies
6000 B-drop LBGs ? i lt 24 ? 24 lt i lt 25 ? 25
lt i lt 26
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z1 Evolved Quiescent Galaxies Old
Passively-Evolving Galaxies (OPEGs)
zf2-10
3900 OPEGs selected Riz colors to z25
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Zgt4
Lyman Beake Galaxies
Dark Matter Halo
z4
gas
1 lt z lt 4
OPEGs
z1
?????????
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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 z4
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, sgb s
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Hamana, TY, et al.
Halo Occupation Model
bias
lt Host Mass gt
Galaxy Density
Halo Occupation Number
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Preliminary results
z 4 LBGs ? ???????? ??????
Mmin 1x1012 Msun
ltMhalogt 2.6x1012 Msun
M1 3x1011 Msun

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Statistical fate of z4 DM halo with 2.6x1012
h-1 Msun (calculated using the Extended
Press-Schechter model )
Preliminary results
T. Hamana, TY, et al.
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Our Results
Preliminary results
Solid line Halo mass growth curve In CDM
Dashed lines68 interval
z4 LBGs
z1 OPEGs
Average host halo mass of galaxies obtained from
their clustering properties
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Discovery of the two seed clusters in SXDS
(Ouchi et al. 2005)
Deep NB816 Narrow-Band Survey (8160Å, for z5.7
Lyaemitters)
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Clump A ?v 180 km/s M1x1013Msun
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Color-Magnitude Diagram for z1 galaxies
Kodama, TY et al. 2004
C-M sequence expected for passive evolution
1.2?
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Galaxy Color Evolution in HDF-N (Kajisawa and
Yamada 2004)
Results obtained with a pencil-beam survey ?
EXTEND TO SXDS !
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3. Extensive Study of Lya Blobs at High Redshift
-Large-Scale Structure of Lya Emitters and
Massive Galaxy Formation-
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z3 simulation
141 h-1 Mpc
BW CDM Colored Galaxies
N-body semi-analytic treatment
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SSA22 Proto-cluster at z3.1
Discovery of the SSA22 proto-cluster of Lyman
Break Galaxies at z3.1 (Steidel et al. 1998)
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Extended LyaEmitters Lya Blobs (LABs)

• Giant LyaEmission-Line Nebulae
• gt 100 kpc (physical scale)
• (Steidel et al. 1998, Keel et al. 1999)
• Internal velocity structure ?vgt1000 km/s
• (Ohyama et al. 2004, Bower et al. 2004)
• Not enough UV by the apparent SFR
• 4 previous examples of LAB with gt
• 100 kpc at z23 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?
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Subaru Narrow-Band Observation of the SSA22
Proto-cluster region
Lya Emitters (LA)

• 2 x 10-17 erg/s/cm2
• EWobs gt 160 Å
• 283?

HDR
Lya absorbers
Hayashino et al. 2004
LAE average local density
Steidel et al. 2000
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Redshift Distribution of LAEs
Obs Subaru FOCAS 56 objects
LAEs
Redshift
LAB1, LAB2
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(No Transcript)
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LAE survey extension to the North-West area
SSA22-Sb2 (2004?8?)
50 Mpc (comoving)

• 2 x 10-17 erg/s/cm2
• EWobs gt 120 Å
• Sb1Sb2 600 ?

SSA22-Sb1 (Hayashino et al. 2004)
HDR (LAE NB497 lt 26.0 EW gt 120Å)
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Subaru 7h image of LAB1
25 190 kpc
How ordinary these gigantic LABs are ? What are
their size, luminosity, and spatial distribution?
z3.1 LBG
Lya image (after continuum subtraction)
(before subtraction)
B, V, NB. Lya green
Cont. subtracted image
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35 ?? Lya Blobs (Matsuda et al. 2004)
25 or 190 kpc at z 3.1
First large sample of LABs
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900 kpc2 at z3.1
or, d30kpc !

• gt16 arcsec2
• gt7sin isophotal aperture

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Sky distribution 35 LABs () and LAEs (?)
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LAB origins of the Lya
(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..
Lyaexcess is seen for 14/35 objects (in the
apparent flux)
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Hidden star formation/AGN ??
Lya peak is displaced from the continuum peak
25 190 kpc
Cont. ?
Lyapeak
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Superwind ? Cooling flow ?
25 190 kpc
Also see Ohyama et al. 2003, Bower et al. 2004
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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
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Results of SCUBA sub-mm observations w/
Smail, Chapman, et al.
LAB1
LAB18 (XMM source!)
c.f., Lyman Break ?????5??
LAB14 detected in Barger et al., Chapman et al.
2004 so to be confirmed
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53W002 No.18 LAB Keel et al. (1999)
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Detected in Sub-mm observation (Smail et al. 2003)
Lyacont
Lya
SCUBA Source SMM 02399-0136 (z2.8)
Slit direction
LyaHalo
NV
LABs in Matsuda et al.
Lya
wavelength
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LABs in the new survey field
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LABs in the new survey field
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LABs in the new survey field
A New Gigantic LAB with gt 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.
25190 kpc
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Slit spectroscopy of LABs with Keck DEIMOS
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Relatively compact Lya emitters ?v lt 500 km/s
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Lya Blobs many have ?v gt 500 km/s, absorption
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Slit spectroscopy of LABs with Keck DEIMOS
FWHM500 km/s
LAB
16 sq.arcsec d30 kpc
Gaussian fit s
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Mass of the LABs

• 1. (Lower limit of) their mass can be evaluated
  from their size,
• assuming that they are collapsed objects
  (before z3.1),
• if we apply the spherical collapse model.
• Mvir 4/3pRvir3 ?crit(z) ?c(z) gt
  4x1010 (RLya / 26kpc)3 Msun
• Assuming that they are bounded objects,
• their mass can be evaluated from their
  size and internal velocity
• Mdyn 1012-13 Msun
• 3. Strong clustering ? associated with more
  massive DM halos ?
• 4. Possibly higher sub-mm detection rate
  (massive SF)

Massive Galaxies in Their Forming Phase
Large Lya Luminosity, Extension, Clustering, High
sub-mm ditection rate
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Summary

• Deep Panoramic Surveys probe the universe
• Galaxy evolutions are being studied
• in large-volume, highly statistically
  accurate
• sample of the SXDS galaxies
• - connection between z4 LBGs and z1
  OPEGs
• - seed cluster at z5.7 discovered in the
  NB search
• - nature of the optically-faint X-ray
  sources
• - mass dependency of galaxy evolution
• We discovered 100 Mpc LSS of LAE at z3.1.
• LyaBlobs, candidates of massive forming
  galaxies
• are distributed along the LSS.

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Future Prospects
SWIRE IRAC(blue) MIPS(red) Scam(white)
Extension of z3 LSS and LAB/LAA/LAE search
ELAIS N1
Lockman Hole
Covered by UKIDSS DXS
SCam / UKIDSS DXS 10 deg2 survey
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Future Prospects
A New Mission
Subaru New NIR Camera and Spectrograph MOIRCS
4x7
Hubble Origins Probe Very Wide Field Imager
GOODS-N