black hole growth and galaxy evolution
DESCRIPTION
Black Hole Growth and Galaxy Evolution. Meg Urry Yale University. ~All galaxies host supermassive black holes. The formation and evolution of galaxies is closely tied to the growth of black holes. ~All galaxies have SMBH Contemporaneous growth of SMBH & stars M- relation. - PowerPoint PPT PresentationTRANSCRIPT
Black Hole Growthand Galaxy Evolution
Meg UrryYale University
~All galaxies host supermassive black holes
The formation and evolution of galaxies
is closely tied tothe growth of black holes~All galaxies have SMBHContemporaneous growth of SMBH & starsM- relation
The formation and evolution of galaxies
is closely tied tothe growth of black holes~All galaxies have SMBHContemporaneous growth of SMBH & starsM- relation
The formation and evolution of galaxies
is closely tied tothe growth of black holes~All galaxies have SMBHContemporaneous growth of SMBH & starsM- relation
M- RelationBl
ack
Hole
Mas
s
Stellar Velocity Dispersion
Effect of Black Hole on Galaxy
Demographics of supermassive black holes
What we learned from multiwavelength surveys
Deep surveys show mostaccretion is obscured
• GOODS, COSMOS, MUSYC, ECDFS, AGES, Lockman Hole, HDF-N/S, NDWFS, XBootes, XMM/LSS, …
• Hard X-rays penetrate obscuration• Energy re-radiated in infrared• High resolution optical separates
host galaxy, constrains redshifts
GOODS
Chandra
Spitzer
HSTXMM
+60
+40
+20
0
20
40
60
ECDFS
GOODS-S UDF
SDSS1030
1256
HDF-S
“COSMOS”
“MUSYC”
GOODS-N HDF
not to scale
HST ACS color image (0.3% of GOODS)
HST+Spitzer color image (0.3% of GOODS)
Treister, Urry & Virani 2009
Survey Results Treister et al. …
• Most BH accretion obscured– Log N-Log S infrared, optical, X-ray, -ray– Fits AGN redshift distribution– Fits X-ray “background”
• Obscuration increases with redshift– NH, narrow lines, infrared selection
Compton-thick & Heavily Obscured AGN
Ultra-Deep INTEGRAL SurveySwift BAT SurveyInfrared excess
Ultra-Deep INTEGRAL Survey
Treister, Urry & Virani 2009, Virani et al. 2009
3 Msec UDIS
Treister, Urry & Virani 2009, Virani et al. 2009
NuSTAR
EXIST
Virani et al. 2009
Compton-thick & Heavily Obscured AGN
Ultra-Deep INTEGRAL SurveySwift BAT SurveyInfrared excess
Heavily obscured &higher redshift AGN
• Not detected in deep Chandra/XMM surveys (nearby AGN detected w INTEGRAL/Swift)• Infrared-bright (high & low redshift)• How to distinguish AGN from starbursts? (X-ray stacking)
2 4 6 8
R K (Vega)
4
3
2
1
0
1
Log
F 24/F
R
Fiore et al. 2008, Treister et al. 2009b
Infrared-excess sources
Daddi et al. 2007, Fiore et al. 2008
24 m “normal” 24 m “excess”
X-Ray Stacked Spectra
Daddi et al. 2007
Redshift
(Mp
c3 )
Treister et al. 2009b
How do quasars form?Sanders et al. 1988 mergers ULIRGsULIRGs quasars
Redshift
Obscured
/Unobscu
red Quas
ars
Obscured to Unobscured Quasar Ratio
Treister et al., submitted
Obscured to Unobscured Quasar Ratio
Treister et al. submitted
X-ray selected
Redshift
Obscured
/Unobscu
red Quas
ars
Local ULIRGs
IR-selected
Treister et al., submitted
The Interplay of Black Holes & Star Formation
First scenario• Common trigger (e.g., merger)?• Star formation starts (delay?)• BH accretion delayed (angular momentum)• AGN turns on, heats ISM/IGM• Star formation turns off• Stars age from blue to red
red
blue
bright faint
Galaxy Colors
red sequence
blue cloud
galaxies merging
stars aging
Schawinski et al. 2009
red
blue
bright faint
Galaxy Colors
Schawinski et al. 2009
red
blue
bright faintSchawinski et al. 2009
Galaxy Colors
red
blue
bright faint
Galaxy Colors
Schawinski et al. 2009
red
blue
bright faint
AGN avoid the blue cloud
Schawinski et al. 2009
Galaxy Colors
Schawinski et al. 2009
red
blueyoung old
1 Gyr
The Future of Deep SurveysWider areasDeep X-ray (NuSTAR)Far-infrared, submm (Herschel, ALMA)
Survey Goals• Cosmic history of BH growth (Treister, Glikman, Virani)
– Herschel, NuSTAR deep surveys (COSMOS)– WFC3 imaging (to separate host and nucleus)
• Form of AGN energy injection – Narrow-band imaging of winds (SINFONI, Paulina Lira)– Absorption spectroscopy in rest-frame UV
• Phasing of AGN turn-on and SF turn-off (Schawinski)– Galaxy colors – Spectral signatures (better)
• Role of mergers (Schawinski)– Major vs. minor mergers (Galaxy Zoo, Cardamone)– Connection to cosmological simulations (Kyoungsoo Lee)
Galaxy Morphology
“Galaxy Zoo”www.galaxyzoo.org
Host Galaxy Morphologies
Disks
Spheroids
u-r c
olor
Log Stellar Mass (Mo)9.0 10.0 11.0 12.0
3.0
2.5
2.0
1.5
1.0
AGN Duty Cycle
Log Stellar Mass (Mo)9.0 10.0 11.0 12.0
u-r c
olor
3.0
2.5
2.0
1.5
1.0
AGN Duty Cycle
0 5 10 15
Time (Gyr) now Big Bang
Number of
obscured AGN
0 5 10 15
Time (Gyr) now Big Bang
Number of
obscured AGN
0 5 10 15
Time (Gyr) now Big Bang
Number of AGN
0 5 10 15
Time (Gyr) now Big Bang
Number of AGN
t
0 5 10 15
Time (Gyr) now Big Bang