Supermassive Black Holes in Deep Multiwavelength Surveys

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Supermassive Black Holes in Deep Multiwavelength
Surveys

• Meg Urry
• Yale University

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HDF-S
lots of (unobscured) quasars at zgt2 (SDSS) fewer
at z6 (opt, X-ray) Are we missing obscured
quasars? (not found in UV/optical surveys)

3

• Supermassive black holes likely obscured by gas
  and dust
• True for local AGN
• Explains hard X-ray background
• More likely in early Universe (Grand
  Unification)

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GOODS

• designed to find
• obscured AGN out to
• the quasar epoch, z2-3

Hard X-rays less attenuated than
optical Mid-infrared re-radiated energy (mixed w
starlight) Deep optical host galaxies v. nuclei
Spitzer Legacy, HST Treasury, Chandra Deep Fields
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MUltiwavelength Survey by Yale-Chile
UBVRIzJHKNB, Spitzer, HST, Chandra, XMM,
Galex VLT, Magellan, Gemini
dec
ECDFS
van Dokkum, Gawiser, Lira, Maza, Urry,
RA
0
24
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Chandra image of E-CDFS
Virani et al. astro-ph/0506551, Lehmer et al.
astro-ph/0506607
Do GOODS/MUSYC (and other ??? surveys) reveal
obscured quasars?
Redshifts of X-ray sources too low
Obscuredunobscured lt 31
But need to take selection effects into account
Find 31 ratio, flat or increasing with redshift
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HST ACS color image (0.3 of GOODS)
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HSTSpitzer color image (0.3 of GOODS)
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HST ACS color image (0.3 of GOODS)
Not What do we see?
What would we see if there were a significant
population of obscured AGN at zgt1?
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Create ensemble of AGN, obscured
unobscured,with correct SEDs for
Unification,evolving N(L) (w LDDE)
Generate N(S), N(z)at X-ray, Optical, Infrared
Compare to dataGOODS, MUSYC,CYDER, SEXSI,
SWIRE, MIPS GTO, GROTH, Lockman,
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Results

• Treister et al. 2004 optical counts, N(z) well
  fit by 31 ratio, 50 AGN not in CDFs
• Treister et al. 2005 fits X-ray background
• Treister et al. 2006a fits IR counts low AGN
  of IR EBL LAGN,IR ?10x LGal,IR
• Treister et al. 2006b Integral survey for
  Compton-thick AGN, BH accretion history
• Treister Urry 2006 meta-analysis shows
  obs/unobs ratio flat or increases with z

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GOODS NS
bright
faint
Treister et al. 2004
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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
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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
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Results

• Treister et al. 2004 optical counts, N(z) well
  fit by 31 ratio, 50 AGN not in CDFs
• Treister et al. 2005 fits X-ray background
• Treister et al. 2006a fits IR counts low AGN
  of IR EBL LAGN,IR ?10x LGal,IR
• Treister et al. 2006b Integral survey for
  Compton-thick AGN, BH accretion history
• Treister Urry 2006 meta-analysis shows
  obs/unobs ratio flat or increases with z

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X-ray background synthesis
Treister et al. 2005
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X-ray background synthesis
Treister et al. 2005
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X-ray background synthesis
Treister et al. 2005
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Results

• Treister et al. 2004 optical counts, N(z) well
  fit by 31 ratio, 50 AGN not in CDFs
• Treister et al. 2005 fits X-ray background
• Treister et al. 2006a fits IR counts low AGN
  of IR EBL LAGN,IR ?10x LGal,IR
• Treister et al. 2006b Integral survey for
  Compton-thick AGN, BH accretion history
• Treister Urry 2006 meta-analysis shows
  obs/unobs ratio flat or increases with z

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Near- mid-IR Spitzer counts
Treister et al. 2005
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Infrared Background
Total AGN contribution to EBL lt10
Treister et al. 2005
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AGN dominate at bright 24 ?m fluxes
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Total 24 ?m luminosities
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Results

• Treister et al. 2004 optical counts, N(z) well
  fit by 31 ratio, 50 AGN not in CDFs
• Treister et al. 2005 fits X-ray background
• Treister et al. 2006a fits IR counts low AGN
  of IR EBL LAGN,IR ?10x LGal,IR
• Treister et al. 2006b Integral survey for
  Compton-thick AGN, BH accretion history
• Treister Urry 2006 meta-analysis shows
  obs/unobs ratio flat or increases with z

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Obscured Accretion Black Hole Growth
Treister et al. 2006b
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Results

• Treister et al. 2004 optical counts, N(z) well
  fit by 31 ratio, 50 AGN not in CDFs
• Treister et al. 2005 fits X-ray background
• Treister et al. 2006a fits IR counts low AGN
  of IR EBL LAGN,IR ?10x LGal,IR
• Treister et al. 2006b Integral survey for
  Compton-thick AGN, BH accretion history
• Treister Urry 2006 meta-analysis shows
  obs/unobs ratio flat or increases with z

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Evolution of obscuration w redshift?

• ?1200 AGN from wide deep surveys
• gt40 spectroscopic redshifts
• Consider X-ray and optical flux limits
• Unobscured ? broad lines
• Obscured ? narrow lines or galaxy-like
• Measure observed ratio, correct for sensitivity

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Dependence on redshift ?
to 22.1 (J,K)
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Observed ratio
Relative to constant
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Even with strong galaxy evolution, ratio appears
to increase with redshift
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AGN SEDs in GOODS
Objects with hard (absorbed) X-ray
spectra (weak) AGN or galaxy in optical luminous
thermal infrared emission
Van Duyne et al. 2006
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Van Duyne et al. 2006
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Van Duyne et al. 2006
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Van Duyne et al. 2006
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Example EXO
B V R
BVR
R-K 7.88
Z J K

KAB 21.4
F0.5-8 keV 2.16x10-14
ECDFS ID 29
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EXOs in MUSYC ECDFS
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EXOs in GOODS-South
Koekemoer et al. 2004, ApJL 600,
L123
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Host galaxy morphologies
Direct view of galaxy formation
Simmons et al. 2006
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Findings Issues

• Lots of obscured AGN out to zgt2
• Compton-thick population not well sampled
  (constrained by XRBG)
• Numbers, evolution still uncertain
• Source of obscuration unclear (nuclear, or
  galaxy?)
• Co-evolution of galaxies and black holes

?
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Ezequiel Treister (PhD 2005) Jeff van
DuyneBrooke SimmonsShanil ViraniCarie
CardamoneJonghak Woo (PhD 2005)Matt ODowd (PhD
2004)Yasunobu UchiyamaEleni Chatzichristou
Graduate students Postdocs
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X-Ray background spectrum very hard
30 keV
Gruber et al. 1999
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unabsorbed AGN spectrum
Increasing NH
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• Ezequiel Treister, CMU, Jeffrey van Duyne, Brooke
  Simmons, Eleni Chatzichristou (Yale U.), David
  Alexander, Franz Bauer, Niel Brandt (Penn State
  U.), Anton Koekemoer, Leonidas Moustakas (STScI),
  Jacqueline Bergeron (IAP), Ranga-Ram Chary (SSC),
  Christopher Conselice (Caltech), Stefano
  Cristiani (Padova), Norman Grogin (JHU) ApJ, in
  press
• Hard X-ray LF evolution for Type 1 AGN Ueda et
  al. 2004
• 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
• Geometry with obscured AGN 3 x unobscured, at
  all z
• 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

47

• Ezequiel Treister, CMU, Jeffrey van Duyne, Brooke
  Simmons, Eleni Chatzichristou (Yale U.), David
  Alexander, Franz Bauer, Niel Brandt (Penn State
  U.), Anton Koekemoer, Leonidas Moustakas (STScI),
  Jacqueline Bergeron (IAP), Ranga-Ram Chary (SSC),
  Christopher Conselice (Caltech), Stefano
  Cristiani (Padova), Norman Grogin (JHU) ApJ, in
  press
• Hard X-ray LF evolution for Type 1 AGN Ueda et
  al. 2004
• 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
• Geometry with obscured AGN 3 x unobscured, at
  all z
• 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

48

• Ezequiel Treister, CMU, Jeffrey van Duyne, Brooke
  Simmons, Eleni Chatzichristou (Yale U.), David
  Alexander, Franz Bauer, Niel Brandt (Penn State
  U.), Anton Koekemoer, Leonidas Moustakas (STScI),
  Jacqueline Bergeron (IAP), Ranga-Ram Chary (SSC),
  Christopher Conselice (Caltech), Stefano
  Cristiani (Padova), Norman Grogin (JHU) ApJ, in
  press
• Hard X-ray LF evolution for Type 1 AGN Ueda et
  al. 2004
• 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
• Geometry with obscured AGN 3 x unobscured, at
  all z
• 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

49

• Ezequiel Treister, CMU, Jeffrey van Duyne, Brooke
  Simmons, Eleni Chatzichristou (Yale U.), David
  Alexander, Franz Bauer, Niel Brandt (Penn State
  U.), Anton Koekemoer, Leonidas Moustakas (STScI),
  Jacqueline Bergeron (IAP), Ranga-Ram Chary (SSC),
  Christopher Conselice (Caltech), Stefano
  Cristiani (Padova), Norman Grogin (JHU) ApJ, in
  press
• Hard X-ray LF evolution for Type 1 AGN Ueda et
  al. 2004
• 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
• Geometry with obscured AGN 3 x unobscured, at
  all z
• 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 31 ratio (divide at 1022
cm-2) Random angles ? NH distribution
51

• Ezequiel Treister, CMU, Jeffrey van Duyne, Brooke
  Simmons, Eleni Chatzichristou (Yale U.), David
  Alexander, Franz Bauer, Niel Brandt (Penn State
  U.), Anton Koekemoer, Leonidas Moustakas (STScI),
  Jacqueline Bergeron (IAP), Ranga-Ram Chary (SSC),
  Christopher Conselice (Caltech), Stefano
  Cristiani (Padova), Norman Grogin (JHU) ApJ, in
  press
• Hard X-ray LF evolution for Type 1 AGN Ueda et
  al. 2004
• 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
• Geometry with obscured AGN 3 x unobscured, at
  all z
• 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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U,B,R26 (5?)
SDSS 103005 z6.3 QSO Field
Chandra Deep Field South
Castanders Window (125601)
Hubble Deep Field South
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Rate of cosmic BH/star formation
(measured) BH growth rate star formation rate
(GOODS)
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Dependence on luminosity
Simple unification Modified unification
Barger et al. 2005, Treister et al. 2005