high-z (z > 3) qsos studied with subaru/hsc
DESCRIPTION
High-z (z > 3) QSOs studied with Subaru/HSC. Masa Imanishi (NAOJ) Tohru Nagao (NAOJ). Outline. Importance and current understanding of high-z QSOs (AGNs). 2. QSOs at z > 7. (M.Imanishi). (Subaru/HSC + UKIRT/WFCAM). 3. Low-luminosity QSOs at z = 3-6. (Subaru/HSC). (T.Nagao). - PowerPoint PPT PresentationTRANSCRIPT
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High-z (z > 3) QSOs studied with Subaru/HSC
Masa Imanishi (NAOJ)
Tohru Nagao (NAOJ)
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Outline
1. Importance and current understanding of high-z QSOs (AGNs)
3. Low-luminosity QSOs at z = 3-6
2. QSOs at z > 7
(Subaru/HSC + UKIRT/WFCAM)
(Subaru/HSC)
(M.Imanishi)
(T.Nagao)
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Why High-z QSOs(AGNs) ?
(1) Very bright
(2) Co-Evolution of SMBHs and Galaxies
SMBHs are ubiquitous in spheroid galaxies
M(gal)M
(BH
)
IGM properties (re-ionization)
DLA, LyA forest
MBH =106-9Msun
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High-z QSO found by SDSS
z>7 QSO not detectablein the optical
z=6.42:Most distant
1um @z~7
Fan 2006
>1000 QSOs at z>3
Bright QSOs only !
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Post SDSS QSO Survey
(2) Search for lower-Luminosity QSOs at z = 3-6
(1) Search for z > 7 QSOs
What next?
NIR data required
(UKIRT/WFCAM)
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1. z>7 QSOs
Very deep Moderately deep
Z Y J H K
NIRoptical
filters
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UKIRT/WFCAM/LAS
Northern: 1907.6 deg^2
Equatorial: 1907.6 deg^2
Y=20.5,J=20.0,H=18.8,K=18.4
z>7 QSOs:~10 expected
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No deep z-band image:z>7 QSO candidates cannot be selected
z>7 QSO:z– NIR = very large
SDSS + >2 magneededJ - KJ - K
z’ -
J
z’ -
J
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WFCAM team compromise Y-band
i ,Y: limiting mag differs only 2mag
Green: QSO
Red: BD
Y-J color difference (small)
Severe contamination
i z Y
J
i’ -
Y
Y - J
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Proposal
>1000 deg 2(wide), z>23.5mag (deep) surveyPossible only with Subaru/HSC
The planned Subaru/HSC >1000 deg 2 survey be executed at (northern) WFCAM/LAS
RA widely distributed
RA
DE
C
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Why Japan?
Japan can lead this area, if we do follow-up before HSC data become archival !
Deep, wide z-band survey only possible with HSC
Subaru/MOIRCS can
At z~7, z-ID requires 0.9-1.5um spectroscopy
Southern VISTA : Z<21.5 ( ?)
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Issues to be solved
SDSS z or Z
SDSS z
Z-band
1 (um)0.8
Y dwarf
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2. low-luminosity QSOs (z=3-6)
Croom et al. (2001)
2dFz<2.3
faint bright
Fan et al. (2001) bright
SDSSz>3.6
QSO LF:
bright end only at z>3
QSO UV background:dominated by faint end
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QSO (Mathews & Ferland 1989)
Starburst, Z=0.05 Zsolar
Starburst, Z=1.00 Zsolar
13.6eV24.6eV
54.4eV
(Leitherer et al. 1999)
UV Background from QSOs at z=3-6
QSO UV is hard
QSOs
Stars
HeII re-ionization
Effect on galaxy formation
Energy (Rydberg)
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QSO Correlation Func.
Faint, numerous QSOs
Corr.Func. bias M(halo) QSO lifetime
Croom et al. (2005)
Redshift0 1 2
bia
s
z < 3
z > 3:unknown
Enoki et al. (2003)
108yr
107yrb e
ff
4
5
6
7
z3 3.5 4 4.5 5
4
5
6
7log MDH/Msun=12.5
12.0
11.5
3
bia
s
Redshift
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Strategy
SDSS ~ too shallow…Deep Surveys (UDF, SDF) ~ too narrow…
Moderately Deep andModerately Wide QSO Surveys
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Multi-band Selection
3000 Wavelength(A) 10000
Richards et al. (2001)g’ — r’ r’ — i’
r’ —
i’
i’ —
z’
Selection in Color-Color Diagram g’r’i’ 3.6 < z < 4.4 r’i’z’ 4.6 < z < 5.1
u g r i z
Survey Strategy
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Multi-band HSC Survey g’ r’ i’ z’ (3mag deeper than SDSS)
g’r’i’z’
26.6mag (23.3)
26.2mag (23.1)
25.5mag (22.3)
24.4mag (20.8)
20min/band/FOV(5σ, 0.7”seeing, 2”φ)
100 QSOs ~ 140 sq.deg. ~ 100 FOV ~ 400 pointing ~ 2 weeks
HSC
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Summary
2. Low-luminosity QSOs at z = 3-6
1. QSOs at z > 7
(Subaru/HSC + UKIRT/WFCAM)
(Subaru/HSC)
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End
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QSO Environment
QSO Activity Interaction
Results at z=0.2 (McLure & Dunlop 2001)
Borne et al. (2000)
Bright galaxy number excess around QSOs
excess QSOsBlank-field
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Strategy
Trigger of QSO ActivityGrowth of SMBHs in QSOsRelation with Galaxy Evolution
Luminosity Function of QSOsCorrelation Function of QSOsEnvironments of QSOs
We need a QSO sample~ with wide luminosity range~ with enough number density
SDSS ~ too shallow…Deep Surveys (UDF, SDF) ~ too narrow…
Moderately Deepand
Moderately WideQSO Surveys
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QSO Correlation Func. Croom et al. (2005)
Redshift
b eff
4
5
6
7
z3 3.5 4 4.5 5
4
5
6
7log MDH/Msun=12.5
12.0
11.5
tQ=3x108 yr
tQ=3x107 yr
Enoki et al. (2003)
~ Corr.Func. bias Mhalo
~ bias QSO Lifetime — mass-accretion timescale
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Co-Evolution of SMBHs and Galaxies
Ferrarese & Meritt (2000)
MBH
[Msu
n]stellar velocity dispersion
Non-AGNs
Marconi & Hunt (2004)
log Mgal [Msun]
log
MBH
[Msu
n]
MBH/Mgal ~ 0.002
~ Evolutionary link between SMBHs and galaxies~ Every galaxies may once experienced an AGN phase
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SDSS QSO Survey: Redshift Distribution
Richards et al. (2006)
Schneider et al. (2005)
46420 QSOsin SDSS DR3
0 1 2 3 4 5Redshift
u’-
dro
pout
g’-
dro
pout