Hidden Black Hole Activity in the Early Universe
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Hidden Black Hole Activity Hidden Black Hole Activity in the Early Universein the Early Universe
Ezequiel TreisterEzequiel Treister (Yale/U. de Chile)
Meg UrryMeg Urry (Yale)
The CYDER Team:
F. Castander, T. Maccarone, P. Coppi, E. Gawiser
The GOODS Team:
F. Bauer, D. Alexander, N. Brandt and others
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Big
Bang
CM
B
Firs
t Sta
rsB
lack
Hol
es
Bla
ck H
oles
Toda
y
Qua
sars
Gal
axie
s &
time
z=0redshift z~2-3z~15
z~1000
Larson, Bromm, Coppi
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Active Galactic Nucleus (AGN)Active Galactic Nucleus (AGN)
supermassive black hole
actively accreting matter
1-1000 x galaxy luminosity from few lt-hrs
Host Galaxy
AGN: signposts for SMBH in early Universe
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AGN-Galaxy ConnectionAGN-Galaxy Connection
All (large) galaxies have supermassive black holes
Common AGN-Galaxy evolution 0<z<2
Tight correlation of MBH with AGN host galaxies are normal
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AGN-Galaxy ConnectionAGN-Galaxy Connection
All (large) galaxies have supermassive All (large) galaxies have supermassive black holesblack holes
Common AGN-Galaxy evolution 0<z<2
Tight correlation of MBH with AGN host galaxies are normal
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AGN-Galaxy ConnectionAGN-Galaxy Connection
All (large) galaxies have supermassive black holes
Common AGN-Galaxy evolution 0<Common AGN-Galaxy evolution 0<zz<2<2
Tight correlation of MBH with AGN host galaxies are normal
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AGN-Galaxy ConnectionAGN-Galaxy Connection
All (large) galaxies have supermassive black holes
Common AGN-Galaxy evolution 0<z<2
Tight correlation of MTight correlation of MBHBH with with AGN host galaxies are normal
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MMBHBH-- Relation Relation
Tremaine et al (2002)
Black Hole mass Black Hole mass is well correlated is well correlated with velocity with velocity dispersion, even dispersion, even though they are though they are dynamically dynamically independent.independent.
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AGN-Galaxy ConnectionAGN-Galaxy Connection
All (large) galaxies have supermassive black holes
Common AGN-Galaxy evolution 0<z<2
Tight correlation of MBH with AGN host galaxies are normalAGN host galaxies are normal
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O’Dowd et al. 2002
Kormendy Kormendy relation for relation for AGN same as AGN same as for normal for normal galaxiesgalaxies
(projection of fundamental plane)
AGN
Normal galaxies
Surface brightness versus sizeSurface brightness versus size
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The AGN Unified ModelThe AGN Unified Model
blazars, Type 1 Sy/QSO
broad lines
Urry & Padovani, 1995
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Type 1 AGN SEDType 1 AGN SED
Manners, 2002mm far-IR near-IR Optical-UV
X-rays
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The AGN Unified ModelThe AGN Unified Model
radio galaxies, radio galaxies, Type 2 Sy/QSOType 2 Sy/QSO
narrow linesnarrow lines
Urry & Padovani, 1995
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Type 2 AGN SEDType 2 AGN SED
Norman et al, 2002
Radio far-IR optical-UV X-rays
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Narrow lines Narrow lines in total lightin total light
Broad lines in Broad lines in polarized lightpolarized light
Antonucci & Miller 1985, Barthel 1987
Evidence for UnificationEvidence for Unification
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More Evidence: The XRBMore Evidence: The XRB
Gruber et al. 1999
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unabsorbed AGN spectrum
Increasing NH
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Population Synthesis ModelsPopulation Synthesis Models
Gilli et al. 1999Gilli et al. 1999Gilli et al. 2001Gilli et al. 2001
Giacconi et al. 1979Giacconi et al. 1979Setti & Woltjer 1989Setti & Woltjer 1989Madau et al. 1994Madau et al. 1994Comastri et al. 1995Comastri et al. 1995
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Hasinger 2002
Gilli et al. population synthesis predictions
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Hidden Population of Hidden Population of Obscured AGN at z>1Obscured AGN at z>1
Not Found in UV/Optical Surveys.
Multiwavelength Surveys needed:
Hard X-rays (Chandra) Far-IR (Spitzer) Optical Spectroscopy (Keck-VLT-Magellan)
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Narrow Area/Deep SurveysNarrow Area/Deep Surveys Low luminosity sources Good to higher redshifts Less obscuration bias
Low numbers of high luminosity objects Large scale structure
Wide Area/Shallow SurveysWide Area/Shallow Surveys High luminosity sources Less “cosmic variance”
Low luminosity objects only at low redshift More obscuration bias
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The CYDER SurveyThe CYDER Survey
CalánYaleDeepExtragalacticResearch
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CYDER Survey CYDER Survey Optical and Near-IR Follow up of X-ray sources in Optical and Near-IR Follow up of X-ray sources in Deep Archived Chandra Fields.Deep Archived Chandra Fields.
FieldField RARA DecDec Chandra Chandra FieldField
Exp. Exp. TimeTime
C2C2 12:52:48 -09:24:30 HCG62 50 ks
C5C5 11:30:07 -14:49:27 Q1127 30 ks
D1D1 22:01:38 -31:46:30 HCG90 50 ks
D2D2 23:47:55 +00:57:21 Q2345 75 ks
D3D3 03:37:44 -05:02:39 SBS0335 60 ks
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PopulationsPopulations
Object CYDER ChaMP CDF-N CDF-S
Unobs. AGN 47.2%47.2% 52.1% 12.4% 35.0%
Obs. AGN 35.8%35.8% 23.9% 39.4% 42.7%
Galaxies 10.4%10.4% 14.1% 43.3% 17.8%
Stars 6.6%6.6% 9.9% 4.9% 4.5%
Total 106106 125 284 168
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V-magnitude DistributionV-magnitude Distribution
All X-ray Sources
Targeted for Spectroscopy
Identified Sources
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Redshift DistributionRedshift Distribution
All X-ray Sources
AGN-Dominated Sources
Unobscured AGN
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V-mag versus RedshiftV-mag versus Redshift
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V-I versus RedshiftV-I versus Redshift
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FFxx/F/Foptopt versus X-ray Luminosity versus X-ray Luminosity
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FFXX/F/Foptopt Ratio Ratio
Fiore et al, 2003
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Obscured to Total AGN RatioObscured to Total AGN RatioF
ract
ion
of O
bscu
red
AG
N Intrinsic
Hard X-ray Luminosity
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Narrow Area/Deep SurveysNarrow Area/Deep Surveys Low luminosity sources Good to higher redshifts Less obscuration bias
Low numbers of high luminosity objects Large scale structure
Wide Area/Shallow SurveysWide Area/Shallow Surveys High luminosity sources Less “cosmic variance”
Low luminosity objects only at low redshift More obscuration bias
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GOODSGOODSdesigned to find designed to find
obscured AGN obscured AGN at the quasar epoch, at the quasar epoch, z~2-3z~2-3
Chandra Deep Fields, Spitzer Legacy, HST Treasury (3.5+ Msec) (800 hrs) (600 hrs) (3.5+ Msec) (800 hrs) (600 hrs)
Very deep imagingVery deep imaging~70 times HDF area (0.1 deg~70 times HDF area (0.1 deg22))
Extensive follow-up spectroscopy (VLT, Gemini, …)Extensive follow-up spectroscopy (VLT, Gemini, …)
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HST ACS fieldsHST ACS fields5 epochs/field, spaced by 45 days, simultaneous V,i,z bands + B band5 epochs/field, spaced by 45 days, simultaneous V,i,z bands + B band
CDF-S: Aug ‘02 - Feb ‘03 HDF-N: Nov ’02 - May ’03CDF-S: Aug ‘02 - Feb ‘03 HDF-N: Nov ’02 - May ’03
done 2003
ApJ Letters 2004, 600, …
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B = 27.2
V = 27.5
i = 26.8
z = 26.7
B = 27.9
V = 28.2
I = 27.6
∆m ~ 0.7-0.8AB mag; S/N=10Diffuse source, 0.5” diameterAdd ~ 0.9 mag for stellar sources
ACS WFPC2
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GOODS X-Ray SourcesGOODS X-Ray Sources
Chandra Deep Field North: Chandra Deep Field North:
Chandra Deep Field South: Chandra Deep Field South:
2 Ms2 Ms 503 sources503 sources 1.4x101.4x10-16 -16 ergs cmergs cm-2-2ss-1-1 (2-8 keV) (2-8 keV)
1 Ms1 Ms 326 sources326 sources 4.5x104.5x10-16 -16 ergs cmergs cm-2-2ss-1-1 (2-8 keV) (2-8 keV)
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Modeling the AGN PopulationModeling the AGN Population• Grid of AGN spectra (LX,NH) with
– SDSS quasar spectrum (normalized to X-ray)– dust/gas absorption (optical/UV/soft X-ray) – infrared dust emission Nenkova et al. 2002, Elitzur et al. 2003– L* host galaxy
• Hard X-ray LF & evolution for Type 1 AGN Ueda et al. 2004
• Geometry with obscured AGN = 3 x unobscured, at all z, L
• Calculate expected redshift distribution – compare to measured redshifts of GOODS AGN
• Calculate expected optical magnitudes of X-ray sources in GOODS fields – compare to GOODS HST data
• Calculate expected N(S) for infrared sources – compare to GOODS Spitzer data
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Modeling the AGN PopulationModeling the AGN Population• Grid of AGN spectra (LX,NH) with
– SDSS quasar spectrum (normalized to X-ray)– dust/gas absorption (optical/UV/soft X-ray) – infrared dust emission Nenkova et al. 2002, Elitzur et al. 2003– L* host galaxy
• Hard X-ray LF & evolution for Type 1 AGN Ueda et al. 2004
• Geometry with obscured AGN = 3 x unobscured, at all z, L
• Calculate expected redshift distribution – compare to measured redshifts of GOODS AGN
• Calculate expected optical magnitudes of X-ray sources in GOODS fields – compare to GOODS HST data
• Calculate expected N(S) for infrared sources – compare to GOODS Spitzer data
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Treister et al. 2004
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Treister et al. 2004
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Modeling the AGN PopulationModeling the AGN Population• Grid of AGN spectra (LX,NH) with
– SDSS quasar spectrum (normalized to X-ray)– dust/gas absorption (optical/UV/soft X-ray) – infrared dust emission Nenkova et al. 2002, Elitzur et al. 2003– L* host galaxy
• Hard X-ray LF & evolution for Type 1 AGN Ueda et al. 2004
• Geometry with obscured AGN = 3 x unobscured, at all z, L
• Calculate expected redshift distribution – compare to measured redshifts of GOODS AGN
• Calculate expected optical magnitudes of X-ray sources in GOODS fields – compare to GOODS HST data
• Calculate expected N(S) for infrared sources – compare to GOODS Spitzer data
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AGN Number Counts CalculationAGN Number Counts CalculationX-Ray Luminosity FunctionX-Ray Luminosity Function
Ueda et al, 2003
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Modeling the AGN PopulationModeling the AGN Population• Grid of AGN spectra (LX,NH) with
– SDSS quasar spectrum (normalized to X-ray)– dust/gas absorption (optical/UV/soft X-ray) – infrared dust emission Nenkova et al. 2002, Elitzur et al. 2003– L* host galaxy
• Hard X-ray LF & evolution for Type 1 AGN Ueda et al. 2004
• Geometry with obscured AGN = 3 x unobscured, at all z, L
• Calculate expected redshift distribution – compare to measured redshifts of GOODS AGN
• Calculate expected optical magnitudes of X-ray sources in GOODS fields – compare to GOODS HST data
• Calculate expected N(S) for infrared sources – compare to GOODS Spitzer data
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Dust emission models from Nenkova et al. 2002, Elitzur et al. 2003
Simplest dust distribution that satisfies
NH = 1020 – 1024 cm-2
3:1 ratio (divide at 1022 cm-2)Random angles NH distribution
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Modeling the AGN PopulationModeling the AGN Population• Grid of AGN spectra (LX,NH) with
– SDSS quasar spectrum (normalized to X-ray)– dust/gas absorption (optical/UV/soft X-ray) – infrared dust emission Nenkova et al. 2002, Elitzur et al. 2003– L* host galaxy
• Hard X-ray LF & evolution for Type 1 AGN Ueda et al. 2004
• Geometry with obscured AGN = 3 x unobscured, at all z, L
• Calculate expected redshift distribution – compare to measured redshifts of GOODS AGN
• Calculate expected optical magnitudes of X-ray sources in GOODS fields – compare to GOODS HST data
• Calculate expected N(S) for infrared sources – compare to GOODS Spitzer data
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redshifts of Chandra deep X-ray sources
GOODS-N
Barger et al. 2002,3, Hasinger et al. 2002, Szokoly et al. 2004
model
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redshifts of Chandra deep X-ray sources
GOODS-N
Barger et al. 2002,3, Hasinger et al. 2002, Szokoly et al. 2004
R<24
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GOODS N+S DistributionGOODS N+S Distribution
Treister et al, 2004
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CYDER X-ray/optical survey
Treister, et al 2004
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SEXSI X-ray/optical survey
Harrison, Helfand, et al.
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Modeling the AGN PopulationModeling the AGN Population• Grid of AGN spectra (LX,NH) with
– SDSS quasar spectrum (normalized to X-ray)– dust/gas absorption (optical/UV/soft X-ray) – infrared dust emission Nenkova et al. 2002, Elitzur et al. 2003– L* host galaxy
• Hard X-ray LF & evolution for Type 1 AGN Ueda et al. 2004
• Geometry with obscured AGN = 3 x unobscured, at all z, L
• Calculate expected redshift distribution – compare to measured redshifts of GOODS AGN
• Calculate expected optical magnitudes of X-ray sources in GOODS fields – compare to GOODS HST data
• Calculate expected N(S) for infrared sources – compare to GOODS Spitzer data
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Treister et al. 2004
brightfaint
GOODS N+S
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Modeling the AGN PopulationModeling the AGN Population• Grid of AGN spectra (LX,NH) with
– SDSS quasar spectrum (normalized to X-ray)– dust/gas absorption (optical/UV/soft X-ray) – infrared dust emission Nenkova et al. 2002, Elitzur et al. 2003– L* host galaxy
• Hard X-ray LF & evolution for Type 1 AGN Ueda et al. 2004
• Geometry with obscured AGN = 3 x unobscured, at all z, L
• Calculate expected redshift distribution – compare to measured redshifts of GOODS AGN
• Calculate expected optical magnitudes of X-ray sources in GOODS fields – compare to GOODS HST data
• Calculate expected N(S) for infrared sources – compare to GOODS Spitzer data
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Treister et al, 2004
Spitzer PredictionsSpitzer Predictions
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Predicted Spitzer counts (3.6 Predicted Spitzer counts (3.6 m)m)
~1/2 AGN missing from deep Chandra samples
Will be detected with Spitzer IRAC
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Total # infrared sources in GOODS: prediction=observed
Observed distribution of infrared fluxes matches prediction.
Spitzer supports model of obscured AGNSpitzer supports model of obscured AGN
Treister, Urry, van Duyne, et al. 2004
3.6 m flux (mJy)
N(>
S)
Observed IRAC fluxes of CDF X-ray sources
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ConclusionsConclusions• Obscured AGN are host galaxy dominated in
optical light• Simple unification model explains:
– (faint) optical magnitude distribution– redshift distribution
• Previously reported dependence of obscured AGN ratio with luminosity can be a selection effect.
• This model is consistent with predictions by XRB population synthesis models:
- Broader redshift distribution with peak at z~1.3 - Type 2/Type 1~3
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Treister et al.
X-ray background synthesis
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X-ray background synthesis
Treister et al.
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Treister et al.