Black Holes in Deep Surveys

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”



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”



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

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


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


Results• Match optical counts, N(z)

50% AGN not in CDFs

• Match X-ray backgroundMatch X-ray background• Match IR counts






X-ray background synthesis


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




Near & mid-IR Spitzer

counts


Total AGN contribution to EBL <10%


Infrared “Background”


50% AGN not in CDFs



• 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


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)


50% AGN not in CDFs


– low AGN % of IR EBL



• 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

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

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

Black Holes in Deep Surveys

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