super-massive black holes across the cosmic...
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Super-massive Black HolesSuper-massive Black HolesAcross the Cosmic HistoryAcross the Cosmic History
Ezequiel TreisterEzequiel TreisterEinstein Fellow Einstein Fellow ((IfAIfA, Hawaii), Hawaii)
Collaborators: Meg Urry, Priya Natarajan, Kevin Schawinski (Yale), Carie Cardamone (MIT),Eric Gawiser (Rutgers), Dave Sanders (IfA), Marta Volonteri (Michigan)
Credit: Treister & Natarajan
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Galactic CenterGalactic Center
Credit: Galactic Center Group at the University of Cologne
Mass: 4x106 Msun
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All (Massive) GalaxiesAll (Massive) Galaxieshave Super-Massive Black Holeshave Super-Massive Black Holes
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The First Black HolesThe First Black Holes
Credit: NASA / WMAP Science Team
timeredshift
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How to grow a SMBH?How to grow a SMBH?The seeds:The seeds:
Volonteri (2010)
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Seed Mass FunctionsSeed Mass Functions
Volonteri (2010)
DirectCollapse
StellarClusters
Pop IIIStars
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Further SMBH Growth:Further SMBH Growth:Active Galactic Nuclei (AGN)Active Galactic Nuclei (AGN)
Urry & Padovani (1995)
Black hole: 106-1010 Msun
Accretion disk: • ~10-4-10-2 pc (from variability)
Torus: • 105-107 Msun• ~few parsec (from IR spectrum)• Geometry unknown• Source of nuclear obscuration
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Black holeBlack hole––Galaxy ConnectionGalaxy Connection
All (massive) galaxies haveAll (massive) galaxies haveblack holesblack holes
Tight correlation of MBH with σCommon BH/SFR EvolutionAGN feedback important
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Black holeBlack hole––Galaxy ConnectionGalaxy Connection
All (massive) galaxies have blackholes
Tight correlation of MTight correlation of MBHBH with with σσCommon BH/SFR EvolutionAGN feedback important
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M-M-σσ Relation Relation
Gueltekin et al. ( 2009)
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Black holeBlack hole––Galaxy ConnectionGalaxy Connection
All (massive) galaxies have blackholes
Tight correlation of MBH with σCommon BH/SFR EvolutionCommon BH/SFR EvolutionAGN feedback important
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Common BH/Star Formation EvolutionCommon BH/Star Formation Evolution
Marconi et al. 2004
Both peak at z~2 anddecline at low z.
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Black holeBlack hole––Galaxy ConnectionGalaxy Connection
All (massive) galaxies have blackholes
Tight correlation of MBH with σCommon BH/SFR EvolutionAGN feedback importantAGN feedback important
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AGN FeedbackAGN Feedback
Springel et al. 2005
No AGN
With AGN Feedback
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Obscured AccretionObscured Accretion• Critical stage of BH-galaxy connection.• Occurs when galaxies form most of their stars.• Can represent up to 50% of matter accretion onto the central black hole.
Credit: Treister & Natarajan
How do we know that?How do we know that?
Local AGN Unification
Explain Extragalactic X-ray “Background”
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Observed X-ray Observed X-ray ““BackgroundBackground””
Treister et al. 2009
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AGN in X-raysAGN in X-raysX-ray spectrum of unobscured AGN muchsofter than X-ray background.
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AGN in X-raysAGN in X-rays
Photoelectric absorptionaffect mostly low energy emission making the observed spectrum look harder.
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AGN in X-raysAGN in X-rays
Increasing NH
Compton Thick AGN
•Defined as obscuredsources with NH>1024 cm-2.• Very hard to find (even inX-rays).• Observed locally andneeded to explain the X-ray background.• Number density highlyuncertain.
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X-ray BackgroundX-ray BackgroundXRB well explained usinga combination ofobscured and unobscuredAGN.
•Setti & Woltjer 1989•Madau et al. 1994•Comastri et al. 1995•Gilli et al. 1999,2001•Ueda et al. 2003•Treister & Urry 2005•Gilli et al. 2007•And others…
Treister et al. 2009
Only 0.1% of the XRBcomes from CT AGN inthe local Universe.
XRB not useful toconstrain CT AGN at z>1
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SwiftSwift INTEGRALINTEGRALLocal Universe (z~0)Local Universe (z~0)
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Log N-Log SLog N-Log S
Treister et al. 2009
CT AGN fraction ~7%
Significantly lowerthan previous XRBpop. synthesis models
Consistent with morerecent measurement4.6% (Burlon+10)
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Fiore et al. 2008, Treister et al. 2009b
Mid-IR SelectionMid-IR SelectionIntermediate Intermediate Redshifts Redshifts (z~1-3)(z~1-3)
• This technique selectsmostly high luminositysources (quasars)
All Sources
X-ray Detected
X-ray Undetected
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Stacking of fStacking of f2424/f/fRR>10>1033 Sources Sources
Soft (0.5-2 keV) Hard (2-8 keV)
- ~4σ detection in each band- fsoft=2.1x10-17erg cm-2s-1. fhard= 8x10-17erg cm-2s-1
- Sources can be detected individually in ~10 Msec
Treister et al. 2009b
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Rest-Frame StackingRest-Frame StackingNH=1024cm-2 Γ=1.9Γ=1.9 (reflected)Thermal kT=0.7 keVHMXBs
Combination of heavily-obscured AGN and star-formation
Treister et al. 2009b
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TheThe Merger-Quasar ConnectionMerger-Quasar Connection
Treister et al. 2010a
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MorphologiesMorphologies
Mrk 273 NGC 7674 NGC 6240
HUDF GOODS-S GOODS-S
Treister et al. 2010a
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Merger-Quasar ConnectionMerger-Quasar ConnectionObscured quasars are the product of the merger of twomassive gas-rich galaxies. After a time Δt the quasarbecomes unobscured
!
Nobsc
NUnobsc
(z) ="t d
2mergerdtdN
Ngal (> Mmin (z)) fgas(z)
NUnobsc (z)
Treister et al. 2010a
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TheThe Merger-Quasar ConnectionMerger-Quasar Connection
Treister et al. 2010a
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TheThe Merger-Quasar ConnectionMerger-Quasar Connection
Δt=96±23 Myrs
The obscured phase represents ~30% of total accretion ontosupermassive black holes
Treister et al. 2010a
Quasars outflows can get rid of most of the surroundingmaterial
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Lower Luminosity Obscured AGNLower Luminosity Obscured AGN
Treister et al. 2010b
CDF-S 4 Msec dataX-ray stacking of IR-selected galaxies
Harder X-ray spectrum for more luminous sources-> More AGN in these samples
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Rest-frame Spectral AnalysisRest-frame Spectral Analysis
Treister et al. 2010b
Combination of thermalemission, X-raybinaries and obscuredAGN
AGN Luminosities
-6x1042erg/s LIR>1011Lo-3x1042erg/s LIR>5x1010Lo-5x1041erg/s5x1010>LIR (Lo)>1010
-7x1041erg/s LIR>1010Lo
Much flatter evolution-> different triggeringmechanism?
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The Future: The Future: NuSTARNuSTAR
February 2012
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The Future:The Future: ASTRO-HASTRO-H
http://astro-h.isas.jaxa.jp
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High Energy ObservationsHigh Energy ObservationsNuSTAR and astro-Hwill directly detect alarge number ofheavily-obscuredAGN up to z~1-2
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AGN Number CountsAGN Number Counts
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Bouwens et al. 2010
Lyman Break SelectionLyman Break SelectionHigh High Redshift Redshift (z>6)(z>6)
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Treister et al. submitted
X-Ray StackingX-Ray Stackingz~6z~6
- ~5σ detection in the soft (3.5-14 keV rest frame) band- ~7σ detection in the hard (14-56 keV) band- Flux ratio ~9- Need NH~1.6x1024cm-2 to explain it- Vast majority of sources heavily obscured (4π obscuration)- No detection in any band at z~7 and z~8 (or combined)
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Accreted Mass Accreted Mass vs Redshiftvs RedshiftObserved z=0 BH MF
X-ray detected
X-ray stacked
z>7 hard band
Treister et al. submitted
z>7 soft band
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Accreted Mass Accreted Mass vs Redshiftvs Redshift
Treister et al. submitted
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Accreted Mass Accreted Mass vs Redshiftvs RedshiftDir. Coll. Self-regulated
Pop III Self-regulated
Dir. Coll., no Self-reg.
Pop III, no Self-reg
Treister et al. submitted
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Hydrogen Re-ionizationHydrogen Re-ionization
Treister et al. submitted
AGN cannot re-ionizethe Universe at z>6
This is because ofheavy obscuration. Ifunobscured, enoughUV photons to re-ionize the Universe
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SummarySummary• Most BH accretion up to z~3 identified in X-rays, eitherdirectly or via stacking.
• Vast majority of accretion, ~70%, is obscured. ~20% ofBH accretion is Compton Thick.
• Future X-ray missions (NuSTAR, Astro-H) will be criticalto study this population of CT AGN.
• Self-regulation appears to be important for BHs at allredshifts. M-σ relation at all redshifts?
• Stacked detection at z~6 in hard band implies very highobscuration in most sources -> 4π obscuration.
• Due to their high obscuration, these sources do not re-ionize the Universe.