Black Holes in Black Holes in Deep Deep SurveysSurveys
Meg UrryYale University
The formation and evolution of galaxiesis closely tied to
the growth of black holes
Cosmic accretion (AGN) important for galaxy formation for black hole physics for understanding ionization, backgrounds, etc.
Cosmic Accretion• Opticallyselected quasars not
representative, do not fairly sample cosmic accretion
• Need less biased surveys
Supermassive Supermassive black holesblack holes
likely obscuredobscured by gas and dust:
1.1. Local AGN UnificationLocal AGN Unification
2.More likely in early Universe (“Grand Unification”)
3.Explains hard X-ray “background”
Supermassive Supermassive black holesblack holes
likely obscuredobscured by gas and dust:
1.Local AGN Unification
2.2. More likely in early More likely in early Universe (“Grand Universe (“Grand Unification”)Unification”)
3.Explains hard X-ray “background”
Supermassive Supermassive black holesblack holes
likely obscuredobscured by gas and dust:
1.Local AGN Unification
2.More likely in early Universe (“Grand Unification”)
3.3. Explains hard X-ray Explains hard X-ray “background”“background”
X-Ray “background” spectrum (superposition of unresolved AGN) is very hard
Courtesy Brusa, Comastri, Gilli, Hasinger
unabsorbed AGN spectrum
Increasing NH
Deep Surveys for Obscured Accretion
• Hard X-rays penetrate most obscuration
• Energy re-radiated in infrared
• High resolution optical separates host galaxy
Chandra
Spitzer
HST
GOODSGOODSGreat
Great
Observatories
Observatories
Origins
Origins
Deep
Deep
Survey
Survey
GOODSGOODSdesigned to find
obscured AGN out to
the quasar epoch, z2-3
Spitzer Legacy, HST Treasury, Chandra Deep Fields Spitzer Legacy, HST Treasury, Chandra Deep Fields
Dickinson, Giavalisco, Giacconi, Garmire
MUSYC
MUltiw
avelength
MUltiw
avelength
Survey
Survey byYale Yale &ChileChile
Gawiser, van Dokkum, CMU, Lira, Maza
Extended Chandra Deep Field Extended Chandra Deep Field SouthSouth
Do GOODS/MUSYC/ surveys reveal hidden populations of obscured
AGN?
Virani et al. 2006, Lehmer et al. 2006
HST ACS color image (0.3% of GOODS)
HST+Spitzer color image (0.3% of GOODS)
Understanding AGN Demographics Quantitatively
• Model X-ray spectrum constrain N(L,z,NH) w XRBG spectrum, N(Sx), N(z)
• Model full SED constrain N(L,z,NH) w XRBG spectrum, N(Sx), N(z),
plus N(Sopt), N(SIR), …Also, can assess selection effects in any filter or spectroscopy
OR
CreateCreate ensemble of AGNAGN, with continuous range of obscuration, correct SEDs for Unification (model),
known luminosity distribution, known cosmic evolutionGenerate expected survey Generate expected survey
content content at X-ray, Optical, Infrared, or any
wavelengths,as function of flux and redshiftCompare to dataCompare to data
GOODS, MUSYC,GOODS, MUSYC,SEXSI, SWIRE, CLASXS, H2XMM, AMSS,
GROTH, Lockman, Champ, …
Assumptions• Hard X-ray LF & LDDE evolution for Type 1 AGN Ueda et al. 2003• 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
• NH distribution corresponding to torus geometry (matches obs)– obscured AGN = 3 x unobscured (matches local obs)– No dependence on z (for now)– Simple linear dependence on luminosity (matches obs)
Ezequiel TreisterEzequiel 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) 2004, ApJ, 616, 123
Also Treister et al. 2005, 2006a, 2006b, 2007
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 (divided at 1022 cm-2)Random angles NH distribution
Treister et al. 2004
Treister et al. 2004
Results• Match optical counts, N(z) Match optical counts, N(z)
50% AGN not in CDFs50% AGN not in CDFs
• Match X-ray background• Match IR counts
– AGN are low % of IR EBL
• Integral & Swift surveys for Compton-thick AGN– Number of Compton-thick AGN may be lower
than assumed – Gives limit on reflection, accretion efficiency
• Meta-analysis obs/unobs ratio increases with z
Treister et al. 2004
GOODS N+S
redshifts of Chandra deep X-ray sources
GOODS-N
Barger et al. 2002,3, Hasinger et al. 2002, Szokoly et al. 2004
Treister et al. 2004
redshifts of Chandra deep X-ray sources
GOODS-N
Barger et al. 2002,3, Hasinger et al. 2002, Szokoly et al. 2004
Treister et al. 2004
Results• Match optical counts, N(z)
50% AGN not in CDFs
• Match X-ray backgroundMatch X-ray background• Match IR counts
– AGN are low % of IR EBL
• Integral & Swift surveys for Compton-thick AGN– Number of Compton-thick AGN may be lower
than assumed – Gives limit on reflection, accretion efficiency
• Meta-analysis obs/unobs ratio increases with z
Treister et al. 2005
X-ray background synthesis
Treister et al. 2005
X-ray background synthesis
Treister et al. 2005
X-ray background synthesis
Results• Match optical counts, N(z)
50% AGN not in CDFs
• Match X-ray background• Match IR countsMatch IR counts
– AGN are low % of IR EBLAGN are low % of IR EBL
• Integral & Swift surveys for Compton-thick AGN– Number of Compton-thick AGN may be lower
than assumed – Gives limit on reflection, accretion efficiency
• Meta-analysis obs/unobs ratio increases with z
Near & mid-IR Spitzer
counts
Treister et al. 2005
Total AGN contribution to EBL <10%
Treister et al. 2005
Infrared “Background”
Results• Match optical counts, N(z)
50% AGN not in CDFs
• Match X-ray background• Match IR counts
– AGN are low % of IR EBL
• Integral & Swift surveys for Compton-thick Integral & Swift surveys for Compton-thick AGNAGN– Number of Compton-thick AGN may be lower Number of Compton-thick AGN may be lower
than assumed than assumed – Gives limit on reflection, accretion efficiencyGives limit on reflection, accretion efficiency
• Meta-analysis obs/unobs ratio increases with z
X-Ray “Background” Spectrum
1 5 10 50 100 500 Energy (keV)
100
60
40
20
10
6
4
E F
(E)
[ke
V2 c
m2 s
1 k
eV
1 s
tr1]
Treister & Urry 2005
0 0.2 0.4 0.6 0.8 1
10
1
3
3
1
1
# o
f Co
mp
ton
Th
ick
AG
N
Normalization of Reflection Component
Integral & SWIRE
Treister et al. (2007)
0 0.2 0.4 0.6 0.8 1
Normalization of Reflection Component
10
8
6
4
2
Loc
al B
lack
Ho
le M
ass
Den
sity
(1
05 M
o
Mp
c3)
Marconi et al. (2004)
Shankar et al. (2004)
Treister et al. (2007)
Results• Match optical counts, N(z)
50% AGN not in CDFs
• Match X-ray background• Match IR counts
– low AGN % of IR EBL
• Integral & Swift surveys for Compton-thick AGN– Number of Compton-thick AGN may be lower
than assumed – Gives limit on reflection, accretion efficiency
• Meta-analysis Meta-analysis obs/unobs ratio increases obs/unobs ratio increases with zwith z
7 surveys2341 AGN1229 with z
BL=unobscuredNL=obscured
Area as function of X-ray flux & optical mag
Treister & Urry 2006b
Treister & Urry 2006b
Treister & Urry 2006b
Black Hole Accretion• Obscured AGN dominate at 0<z<2
– Obscuration decreases w luminosity– Obscuration increases w redshift– Explains X-ray “background” & surveys– True z-distr does peak at z>1 (incomplete spectra)
• Limits on Compton Thick AGN integral, swift, spitzer– High degree of Compton reflection
• to match observed low #s of CT AGN• to avoid overproducing local BH density
• Total bolometric AGN light < 10% of extragalactic light (mostly stars)
• Compare to local BH mass efficiency of accretion, 0.1-0.2, where
=L/mc2
Carie Cardamone Shanil ViraniJeff van DuyneBrooke SimmonsEzequiel Treister (PhD 2005) Jonghak Woo (PhD 2005)Matt O’Dowd (PhD 2004)
Yasunobu UchiyamaEleni Chatzichristou
Graduate students:
Postdocs:
Luminosity-dependent density evolution
Hasinger et al. 2005
>1046 ergs/s
1045-6 ergs/s
1044-5 ergs/s
1043-4 ergs/s
1042-3 ergs/s
Van Duyne et al. 2007
Objects with Objects with hard hard (absorbed) X-X-ray spectra:ray spectra:
(weak) AGN or galaxy in optical
luminous thermal infrared emission
AGN SEDs in GOODS
Van Duyne et al. 2007
Van Duyne et al. 2007
Van Duyne et al. 2007
Host galaxy morphologies
Direct view of galaxy formationSimmons et al. 2007
Deep Integral Survey of the XMM-LSS region
300 ksec of our 2 Msec Integral Treister et al. 2007
1 Msec Integral (300 ksec of our 2 Msec)
1 Compton-Thick 1 Compton-Thick AGNAGN
in in 150 deg150 deg22
Deep Integral Survey of the Greater XMM-LSS region
Hard X-ray Counts0.1
0.01
103
104
105
1012 1011 1010 109
Treister et al. (2007)F(20-40 keV) [erg cm2 s 1]
N(>
S)
[de
g2]
Inte
gra
l
“EXO” Extreme X-ray-to-Optical AGN
B V R BVR
Z J K
KAB = 21.4
R-K = 7.88
X-ray
ECDFS ID: 29
Blue Green Red Composite optical
Redder Near-IR Reddest Near-IR
•very high redshift AGN with z > 6, or •very obscured AGN w old/dusty host galaxies at z~2
EXOs in MUSYC ECDFS
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