AGN deep multiwavelength AGN deep multiwavelength surveys:surveys:

the case of the Chandra Deep Field South the case of the Chandra Deep Field South

AGN deep multiwavelength AGN deep multiwavelength surveys:surveys:

the case of the Chandra Deep Field South the case of the Chandra Deep Field South

Fabrizio FioreFabrizio FioreSimonetta Puccetti, Giorgio LanzuisiSimonetta Puccetti, Giorgio Lanzuisi

Table of contentTable of content Introduction

Big scenario for structure formation: AGN & galaxy co-evolution

SMBH census: search for highly obscured AGN X-ray surveys

Unobscured and moderately obscured AGN density Infrared surveys

Compton thick AGN CDFS 2Msec observation: the X-ray view of IR

bright AGN: Spectra of IR sources directly detected in X-rays X-ray “stacking” analysis of the sources not directly

detected.

Introduction Big scenario for structure formation: AGN & galaxy

co-evolution SMBH census: search for highly obscured AGN

X-ray surveys Unobscured and moderately obscured AGN density

Infrared surveys Compton thick AGN

CDFS 2Msec observation: the X-ray view of IR bright AGN: Spectra of IR sources directly detected in X-rays X-ray “stacking” analysis of the sources not directly

detected.

Co-evolution of galaxies and SMBHCo-evolution of galaxies and SMBH

Two seminal results:1. The discovery of SMBH in the

most local bulges; tight correlation between MBH and bulge properties.

2. The BH mass density obtained integrating the AGN L.-F. and the CXB ~ that obtained from local bulges

most BH mass accreted during luminous AGN phases!

Most bulges passed a phase of activity:

1) Complete SMBH census, 2) full understanding of AGN

feedback are key ingredients to understand

galaxy evolution

QuickTime™ e undecompressore

sono necessari per visualizzare quest'immagine.

AGN and galaxy co-evolutionAGN and galaxy co-evolution Early on

Strong galaxy interactions= violent star-bursts

Heavily obscured QSOs

When galaxies coalesce accretion peaks QSO becomes

optically visible as AGN winds blow out gas.

Later times SF & accretion

quenched red spheroid,

passive evolution

Early on Strong galaxy

interactions= violent star-bursts

Heavily obscured QSOs

When galaxies coalesce accretion peaks QSO becomes

optically visible as AGN winds blow out gas.

Later times SF & accretion

quenched red spheroid,

passive evolution

To prove this scenario we need to have:

1) Complete SMBH census, 2) Physical models for AGN feedbacks 3) Observational constraints to these models

Evidences for missing SMBH Evidences for missing SMBH While the CXB energy density providesa statistical estimate of SMBH growth, the lack, so far, of focusing instrument above 10 keV (where the CXB energy density peaks), frustrates our effort to obtain a comprehensive picture of the SMBH evolutionary properties.

Gilli et al. 2007

Marconi 2004-2007Menci , Fiore et al. 2004, 2006, 2008

43-44

44-44.5

AGN densityAGN density

43-44

44-44.5

44.5-45.5

>45.5

42-43

La Franca, Fiore et al. 2005Menci, Fiore et al. 2008

Paucity of Seyfert like sources @ z>1 is real? Or, is it, at least partly, a selection effect?

Are we missing in Chandra and XMM surveys highly obscured (NH1024 cm-2) AGN? Which are common in the local Universe…

Paucity of Seyfert like sources @ z>1 is real? Or, is it, at least partly, a selection effect?

Are we missing in Chandra and XMM surveys highly obscured (NH1024 cm-2) AGN? Which are common in the local Universe…

Highly obscured

Mildly Compton thick

INTEGRAL survey ~ 100 AGN

Sazonov et al. 2006

Completing the census of SMBHCompleting the census of SMBH

X-ray surveys: very efficient in selecting

unobscured and moderately obscured AGN

Highly obscured AGN recovered only in ultra-deep exposures

IR surveys: AGNs highly obscured at optical

and X-ray wavelengths shine in the MIR thanks to the reprocessing of the nuclear radiation by dust

X-ray surveys: very efficient in selecting

unobscured and moderately obscured AGN

Highly obscured AGN recovered only in ultra-deep exposures

IR surveys: AGNs highly obscured at optical

and X-ray wavelengths shine in the MIR thanks to the reprocessing of the nuclear radiation by dust

Dusty

torus

Central engine

X-ray-MIR surveysX-ray-MIR surveys CDFS-Goods MUSIC catalog (Grazian et al. 2006, Brusa, FF et al. 2008) Area

0.04 deg2 ~200 X-ray sources, 2-10 keV down to 210-16 cgs, 0.5-2 keV down to 510-17

cgs 150 spectroscopic redshifts 1100 MIPS sources down to 40 Jy, 3.6m detection down to 0.08 Jy Ultradeep Optical/NIR photometry, R~27.5, K~24 ELAIS-S1 SWIRE/XMM/Chandra survey (Puccetti, FF et al. 2006, Feruglio,FF et

al. 2007, La Franca, FF et al. 2008). Area 0.5 deg2 500 XMM sources, 205 2-10 keV down to 310-15 cgs, >half with spectroscopic

redshifts. 2600 MIPS sources down to 100 Jy, 3.6m detection down to 6 Jy Relatively deep Optical/NIR photometry, R~25, K~19 COSMOS XMM/Chandra/Spitzer. Area ~1 deg2

~1700 Chandra sources down to 610-16 cgs, >half with spectroscopic redshifts. 900 MIPS sources down to 500 Jy, 3.6m detection down to 10 Jy, R~26.5 In future we will add: CDFS-Goods, Chandra 2Msec observation CDFN-Goods COSMOS deep MIPS survey

CDFS-Goods MUSIC catalog (Grazian et al. 2006, Brusa, FF et al. 2008) Area 0.04 deg2

~200 X-ray sources, 2-10 keV down to 210-16 cgs, 0.5-2 keV down to 510-17 cgs 150 spectroscopic redshifts

1100 MIPS sources down to 40 Jy, 3.6m detection down to 0.08 Jy Ultradeep Optical/NIR photometry, R~27.5, K~24 ELAIS-S1 SWIRE/XMM/Chandra survey (Puccetti, FF et al. 2006, Feruglio,FF et

al. 2007, La Franca, FF et al. 2008). Area 0.5 deg2 500 XMM sources, 205 2-10 keV down to 310-15 cgs, >half with spectroscopic

redshifts. 2600 MIPS sources down to 100 Jy, 3.6m detection down to 6 Jy Relatively deep Optical/NIR photometry, R~25, K~19 COSMOS XMM/Chandra/Spitzer. Area ~1 deg2

~1700 Chandra sources down to 610-16 cgs, >half with spectroscopic redshifts. 900 MIPS sources down to 500 Jy, 3.6m detection down to 10 Jy, R~26.5 In future we will add: CDFS-Goods, Chandra 2Msec observation CDFN-Goods COSMOS deep MIPS survey

40

arcmi

n

52

arcmin

z = 0.73 structure

z-COSMOS faint

Color: XMM first year

Full COSMOS field

Chandra deep and wide fieldsChandra deep and wide fieldsCDFS 2Msec 0.05deg2 CCOSMOS 200ksec 0.5deg2 100ksec 0.4deg2

~400 sources 1.8 Msec ~1800 sources Elvis et al. 2008

20 arcmin 1 deg

AGN directly detected in X-raysAGN directly detected in X-rays

Open circles=logNH>23 Open squares = MIR/O>1000 sources

(Tozzi et al. 2003)

MIR selection of CT AGNMIR selection of CT AGN

ELAIS-S1 obs. AGN ELAIS-S1 24mm galaxies HELLAS2XMMCDFS obs. AGN

Fiore et al. 2003

Open symbols = unobscured AGNFilled symbols = optically obscured AGN

Unobscured obscured

X/0

MIR/O

MIR selection of CT AGNMIR selection of CT AGN

CDFS X-rayHELLAS2XMM GOODS 24um galaxies

COSMOS X-ray COSMOS 24um galaxies

R-K

Fiore et al. 2008a Fiore et al. 2008b

Open symbols = unobscured AGNFilled symbols = optically obscured AGN* = photo-z

GOODS MIR AGNsGOODS MIR AGNs

Fiore et. al. 2008a

Stack of Chandra images of MIR sources not directly directly detected in X-rays

F24um/FR>1000 R-K>4.5logF(1.5-4keV) stacked sources=-17 @z~2 logLobs(2-8keV) stacked sources ~41.8log<LIR>~44.8 ==> logL(2-8keV) unabs.~43Difference implies logNH~24

F24/FR>1000 R-K>4.5 <SFR-IR>~200!! Msun/yr <SFR-UV>~7!! Msun/yr <SFR-X>~65 Msun/yrF24um/FR<200 R-K>4.5 <SFR-IR> ~ 18 Msun/yr

<SFR-UV> ~13 Msun/yr

<SFR-X>~20 Msun/yr

F24/FR>1000 R-K>4.5 <SFR-IR>~200!! Msun/yr <SFR-UV>~7!! Msun/yr <SFR-X>~65 Msun/yrF24um/FR<200 R-K>4.5 <SFR-IR> ~ 18 Msun/yr

<SFR-UV> ~13 Msun/yr

<SFR-X>~20 Msun/yr

Program of the project (1) Program of the project (1)

Selection of IR sources with X-ray detection which are likely to host a highly obscured AGN

Extraction of the Chandra spectra of these sources from the event files

Characterization of the X-ray spectra: estimate of the absorbing column density

Evaluation of systematic errors: Background evaluation Combination of data from

different observations

Selection of IR sources with X-ray detection which are likely to host a highly obscured AGN

Extraction of the Chandra spectra of these sources from the event files

Characterization of the X-ray spectra: estimate of the absorbing column density

Evaluation of systematic errors: Background evaluation Combination of data from

different observations

Program of project (2)Program of project (2) Selection of IR

sources without a direct X-ray detection which are likely to host a highly obscured AGN

‘Stacking’ of X-ray images at the position of these sources

Analysis of the ‘stacked’ images

Selection of IR sources without a direct X-ray detection which are likely to host a highly obscured AGN

‘Stacking’ of X-ray images at the position of these sources

Analysis of the ‘stacked’ images

X-ray (and multiwavelength) surveys

X-ray (and multiwavelength) surveys

Fabrizio FioreFabrizio Fiore

Table of contentTable of content

A historical perspective Tools for the interpretation of survey data

Number counts Luminosity functions

Main current X-ray surveys What next

A historical perspective Tools for the interpretation of survey data

Number counts Luminosity functions

Main current X-ray surveys What next

A historical perspectiveA historical perspective First survey of cosmological objects:

radio galaxies and radio loud AGN The discovery of the Cosmic X-ray

Background The first imaging of the sources making

the CXB The resolution of the CXB What next?

First survey of cosmological objects: radio galaxies and radio loud AGN

The discovery of the Cosmic X-ray Background

The first imaging of the sources making the CXB

The resolution of the CXB What next?

Radio sources number counts

First results from Cambridge surveys during the 50’: RyleNumber counts steeper than expected from Euclidean universe

Number countsFlux limited sample: all sources in a given region of the sky with flux > thansome detection limit Flim.

• Consider a population of objects with the same L • Assume Euclidean space

€

n(r) = space density; dN(r) = n(r)dV = n(r)r2drdΩ total number of sources

dN(r)

dΩ= n(r)r2dr surface density; F =

L

4πr2 Flux; F > Flim rmax =

L

4πFlim

⎛

⎝ ⎜

⎞

⎠ ⎟

1/ 2

N(Flim) =dN

dΩ∫ F > Flim( ) =

dN

dΩ∫ r < rmax( ) n(r)r2dr

0

rmax

∫

Total number of sources per unit solid angle (cumulative distribution)

Uniform density of objects ⇒ n(r) = n0

N(Flim ) = n0

rmax3

3=

n0

3

L

4πFlim

⎛

⎝ ⎜

⎞

⎠ ⎟

3 / 2

log N(Flim )( ) = logn0L

3 / 2

3 4π( )3 / 2

⎛

⎝ ⎜ ⎜

⎞

⎠ ⎟ ⎟−

3

2log Flim( ) ⇒ α = −1.5

Number counts

Test of evolution of a source population (e.g. radio sources). Distances of individual sources are not required, just fluxes or magnitudes: the number of objects increases by a factor of 100.6=4 with each magnitude.So, for a constant space density, 80% of the sample will be within 1 mag from the survey detection limit.

( ) ( )

( ) m. N(m)mF

m . -F F.m

60log 6.0log2

3

40log so log52

lim

limlim

∝⇒=−

∝−∝

If the sources have some distribution in L:

€

n(r,L)drdL = n(r)Φ(L)drdL

Φ(L)dL ≡ Luminosity Function

N(r) = n(r,L)r 2drdL =0

rmax(L)

∫∫ n0

34πFlim( )

−3/ 2L3/ 2∫ Φ(L)dL

Problems with the derivation of the number counts

• Completeness of the samples.

• Eddington bias: random error on mag measurements can alter the number counts. Since the logN-logFlim are steep, there are more sources at faint fluxes, so random errors tend to increase the differential number counts. If the tipical error is of 0.3 mag near the flux limit, than the correction is 15%.

• Variability.

• Internal absorption affects “color” selection.

• SED, ‘K-correction’, redshift dependence of the flux (magnitude).

Galaxy number counts

Optically selected AGN number counts

z<2.2B=22.5 100 deg-2

B=19.5 10 deg-2

z>2.2B=22.5 50 deg-2

B=19.5 1 deg-2

B-R=0.5

X-ray AGN number counts

<X/O> OUV sel. AGN=0.3

R=22 ==> 310-15 1000deg-2 R=19 ==> 510-14 25deg-2

The surface density of X-ray selected AGNis 2-10 times higher than OUV selected AGN

The cosmic backgrounds energy densities

The Cosmic X-ray BackgroundThe Cosmic X-ray BackgroundGiacconi (and collaborators) program:1962 sounding rocket1970 Uhuru1978 HEAO11978 Einstein1999 Chandra!

The Cosmic X-ray BackgroundThe Cosmic X-ray Background The CXB energy density: Collimated instruments:

1978 HEAO1 2006 BeppoSAX PDS 2006 Integral 2008 Swift BAT

Focusing instruments: 1980 Einstein 0.3-3.5 keV 1990 Rosat 0.5-2 keV 1996 ASCA 2-10 keV 1998 BeppoSAX 2-10 keV 2000 RXTE 3-20 keV 2002 XMM 0.5-10 keV 2002 Chandra 0.5-10 keV 2012 NuSTAR 6-100 keV 2014 Simbol-X 1-100 keV 2014 NeXT 1-100 keV 2012 eROSITA 0.5-10 keV 2020 IXO 0.5-40 keV

The CXB energy density: Collimated instruments:

1978 HEAO1 2006 BeppoSAX PDS 2006 Integral 2008 Swift BAT

Focusing instruments: 1980 Einstein 0.3-3.5 keV 1990 Rosat 0.5-2 keV 1996 ASCA 2-10 keV 1998 BeppoSAX 2-10 keV 2000 RXTE 3-20 keV 2002 XMM 0.5-10 keV 2002 Chandra 0.5-10 keV 2012 NuSTAR 6-100 keV 2014 Simbol-X 1-100 keV 2014 NeXT 1-100 keV 2012 eROSITA 0.5-10 keV 2020 IXO 0.5-40 keV

The V/Vmax test

Marteen Schmidt (1968) developed a test for evolution not sensitive tothe completeness of the sample.Suppose we detect a source of luminosity L and flux F >Flim at a distance

r in Euclidean space:

€

r =L

4πF

⎛

⎝ ⎜

⎞

⎠ ⎟

1/ 2

the same source could have been detected at a distance rmax =L

4πFlim

⎛

⎝ ⎜

⎞

⎠ ⎟

1/ 2

So we can define 2 spherical volumes : V =4πr3

3 ; Vmax =

4πrmax3

3

If we consider a sample of sources distributed uniformly, we expect that half will be found in the inner half of the volume Vmax and half in the outerhalf. So, on average, we expect V/Vmax=0.5

The V/Vmax test

€

V =

4πr3 / 3( )0

rmax

∫Ω

∫ n(r)r2drdΩ

n(r)r2drdΩ0

rmax

∫Ω

∫=

4πn0

3r5dr

0

rmax

∫

n0 r2dr0

rmax

∫

=4π

3

rmax6 /6

rmax3 / 3

=4π

3

rmax3

2 so :

V

Vmax

= 0.5

In an expanding Universe the luminosity distance must be used in placeof r and rmax and the constant density assumption becomes one ofconstant density per unit comuving volume .

∑=

=N

i i

i

zV

zV

V

V

1 maxmax )(

)(

Luminosity function

In most samples of AGN <V/Vmax> > 0.5. This means that the luminosityfunction cannot be computed from a sample of AGN regardless of their z.Rather we need to consider restricted z bins.

maxmax

1

)(

:sample limited volumea fromdrawn are sources theIf

V

N

VlL L==ΔΦ ∑

More often sources are drawn from flux-limited samples, and the volumesurveyed is a function of the Luminosity L. Therefore, we need to accountfor the fact that more luminous objects can be detected at larger distances and are thus over-represented in flux limited samples. This is done by weighting each source by the reciprocal of the volume over whichit could have been found:

∑=Φi i zV

dLzL)(

1),(

max

Assume that the intrinsicspectrum of the sourcesmaking the CXB has E=1

I0=9.810-8 erg/cm2/s/sr

’=4I0/c

Optical (and soft X-ray) surveys gives values 2-3 times lower than those obtained from the CXB (and of the F.&M. and G. et al. estimates)

Flu

x 0.

5-10

keV

(cg

s)

Area

HELLAS2XMM 1.4 deg2

Cocchia et al. 2006Champ 1.5deg2Silverman et al. 2005

XBOOTES 9 deg2

Murray et al. 2005, Brand et al. 2005

XMM-COSMOS 2 deg2

-16

-15

-14

-13

CDFN-CDFS 0.1deg2 Barger et al. 2003; Szokoly et al. 2004

EGS/AEGIS 0.5deg2

Nandra et al. 2006

SEXSI 2 deg2 Eckart et al. 2006

C-COSMOS 0.9 deg2

E-CDFS 0.3deg2

Lehmer et al. 2005

ELAIS-S1 0.5 deg2

Puccetti et al. 2006

Pizza Plot

A survey of X-ray surveysA survey of X-ray surveys

A survey of X-ray surveysA survey of X-ray surveys

Point sources Clusters of galaxies

A survey of surveysA survey of surveysMain areas with large multiwavelength coverage:

CDFS-GOODS 0.05 deg2: HST, Chandra, XMM, Spitzer, ESO, Herschel, ALMA

CDFN-GOODS 0.05 deg2: HST, Chandra, VLA, Spitzer, Hawaii, Herschel

AEGIS(GS) 0.5 deg2: HST, Chandra, Spitzer, VLA, Hawaii, Herschel

COSMOS 2 deg2: HST, Chandra, XMM, Spitzer, VLA, ESO, Hawaii, LBT, Herschel, ALMA

NOAO DWFS 9 deg2 : Chandra, Spitzer, MMT, Hawaii, LBT SWIRE 50 deg2 (Lockman hole, ELAIS, XMMLSS,ECDFS):

Spitzer, some Chandra/XMM, some HST, Herschel

eROSITA! 20.000 deg2 10-14 cgs 200 deg2 310-15 cgs

Main areas with large multiwavelength coverage:

CDFS-GOODS 0.05 deg2: HST, Chandra, XMM, Spitzer, ESO, Herschel, ALMA

CDFN-GOODS 0.05 deg2: HST, Chandra, VLA, Spitzer, Hawaii, Herschel

AEGIS(GS) 0.5 deg2: HST, Chandra, Spitzer, VLA, Hawaii, Herschel

COSMOS 2 deg2: HST, Chandra, XMM, Spitzer, VLA, ESO, Hawaii, LBT, Herschel, ALMA

NOAO DWFS 9 deg2 : Chandra, Spitzer, MMT, Hawaii, LBT SWIRE 50 deg2 (Lockman hole, ELAIS, XMMLSS,ECDFS):

Spitzer, some Chandra/XMM, some HST, Herschel

eROSITA! 20.000 deg2 10-14 cgs 200 deg2 310-15 cgs

40

arcmi

n

52

arcmin

z = 0.73 structure

z-COSMOS faint

Color: XMM first year

Full COSMOS field

Chandra deep and wide fieldsChandra deep and wide fieldsCDFS 2Msec 0.05deg2 CCOSMOS 200ksec 0.5deg2 100ksec 0.4deg2

~400 sources 1.8 Msec ~1800 sources Elvis et al. 2008

20 arcmin 1 deg

XMM surveysXMM surveysCOSMOS 1.4Msec 2deg2

Lockman Hole 0.7Msec 0.3deg2

Chandra surveysChandra surveysAEGIS: Extended Groth Strip Bootes field

Spitzer large area surveys: SWIRE

Spitzer large area surveys: SWIRE

Elais-N1 Elais-N2

XMM-LSS

Elais-S1

Lockman Hole

eROSITAeROSITA

~30ks on poles, ~1.7ksec equatorial

What next? The X-ray survey discovery space

What next? The X-ray survey discovery space

-13 -15 -17 cgs

log Sensitivity

log

Ene

rgy

rang

e

1

10

100

keV

Log

Area

deg2

4

2

0

Einstein ROSATEinstein ROSAT

ROSAT ROSAT eROSITAeROSITA

ASCA/BSAX ASCA/BSAX XMM ChandraXMM Chandra IXOIXO

IXOIXO

NS NeXT SXNS NeXT SX

BSAX/ASCA BSAX/ASCA XMMXMMSwiftSwift