november, 7 2006cxc extragalactic surveys workshop obscured agn in the cosmos field: the...

November, 7 2006 CXC Extragalactic Surveys workshop

Obscured AGN in the COSMOS field: the multiwavelength challenge

Obscured AGN in the COSMOS field: the multiwavelength challenge

Marcella Brusa (MPE)

Collaborators:F. Civano, A. Comastri, G. Zamorani, F. Fiore (optical ID)+ XMM-COSMOS team: G. Hasinger (PI), N. Cappelluti, M. Elvis, A.

Finoguenov, R. Gilli, V. Mainieri, T. Miyaji, C. Vignali ...+ P. Capak, H. McCracken, D. Thompson + (optical catalogs)M. Salvato, O. Ilbert, H. Aussel + S-COSMOS (Spitzer)J. Trump + IMACS, S.Lilly + zCOSMOS (redshifts)


Motivation of the XMM-COSMOS project

Deep multiwavelength coverage needed to properly study and characterize AGN population as a whole:

Check for selection criteriaselection criteria (X-ray vs. optical vs. IR vs. radio) Determine bolometric output obscured sources and low-L objects Complete picture of AGN/galaxy (co)-evolution

(One of the) Main goal of the XMM-Newton Wide field survey in the (One of the) Main goal of the XMM-Newton Wide field survey in the COSMOS field is: COSMOS field is: „„study the study the evolution of evolution of (obscured)(obscured) Active Galactic Nuclei Active Galactic Nuclei over the over the cosmic timecosmic time and the dependence of and the dependence of black hole growthblack hole growth on on galaxy galaxy morphologymorphology and and environmentenvironment““

(Hard) X-ray selection

Large, contiguous area

Massive Redshift campaigns

High resolutionoptical data


+ MAMBO, CFHT, Bolocam and (future) others

COSMOS major components (in order of appearance) :

HST/ACS (I-band – 590 orbits – I(AB)~27)

2002-2003: Subaru imaging (~25 nights - b,v,r,i,z=26/27) VLA (265 hours – 24 μJy) GALEX deep (200 ks, AB~25) XMM-Newton (800 ks – 10-15 cgs)

2004-2005: XMM-Newton (600 ks) VLT (540 hours) & Magellan (12+ nights) SPITZER-IRAC (200 hours - ~1 μJy)

2006: SPITZER-MIPS (200 hours - ~70 μJy) Chandra (1.8 Ms)

Cosmos Survey2 deg2 (PI: N. Scoville)

AO3: 800 ks of XMM[25x32 ks pointings] reduction/analysis completed ~1400 AGN detected~70 clusters/diffuse sources

AO4: 600 ks (Total = 1.4 Ms) of XMM reduction on-going ~2000 sources expected at the completion of the survey

http://www.astro.caltech.edu/cosmos/

XMM-NewtonPI: G. Hasinger

Hasinger et al. 2007

soft 0.5-2.0 keVmedium 2.0-4.5 keV

hard 4.5-10.0 keV

C-COSMOS

1.8 Ms

(PI M. Elvis)


XMM-COSMOS 2 deg2

-16

-15

-14

-13

Flu

x 2

-10

keV

(cg

s)

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

EGS/AEGIS 0.5deg2Nandra et al. 2006

HELLAS2XMM 1.4 deg2Cocchia et al. 2006Champ 1.5deg2Silverman et al. 2005

XBOOTES 9 deg2Murray et al. 2005, Brand et al. 2005

XMM-COSMOS in a context

SEXSI 2 deg2 Eckart et al. 2006

Area(see Brandt & Hasinger 2005 review (ARA&A 43, 827)

C-COSMOS 0.9 deg2

E-CDFS 0.3deg2 Lehmer et al. 2005

ELAIS-S1 0.5deg2Puccetti et al. 2006


COSMOS source counts

logN-logS (normalized to Euclidean slope)

0.5-2 keV Confirm previous results with unprecedent accuracy in the flux range 8x10-16-5x10-12 cgs:

5-10 keV In between previous determinations in the flux range 10-14- 5x10-12 cgs

Able to explain most of differences in source counts from different surveys as a combination of Poissonian noise and clustering effects

Cappelluti et al. 2007


From X-ray counts to bolometric properties

(First) Crucial step is X-ray source identification assign redshift, investigate extinction properties,

derive physical quantities

COSMOS has (or will have soon) all the data to make the source identification at best

“Problem”: XMM-Newton PSF is 6” optical data “too” deep (Scoville et al. 2007) ~1 object expected by chance in a 5” error box at the 24-26 mag large spread on X/O ratios for X-ray sources


Brandt & Hasinger 2005

Extreme X-ray/optical objects

EXOs

Optical identificationX/O diagram

optically faint (I>24) difficult to identify using optical bands only [see also Alexander et al. 2001]

~200 sources in the XMM-COSMOS sample:

candidate high-z (z>1) obscured QSO, z>4 QSO…

Efficiency of combination of IR+hard X-ray surveys [Mignoli et al. 2004, Koekemoer et al. 2004, Brusa et al. 2005, Severgnini et al. 2005, Maiolino et al. 2006 and many others!]

~1300 sources


IRAC 3.6 IRAC 4.5

IRAC 8.0 ACS

~100 objects in XMM-COSMOS identified through IRAC (most of them EROs/red objects/optically faint)

Very hard to get redshift from optical alternative approaches: ISAAC/IRS spectroscopy and/or SED fitting

[Koekemoer et al. 2004, Mainieri et al. 2005, Maiolino et al. 2006]

See Anton’s talk

From optical bands to IRAC/MIPS Courtesy: Salvato, Ilbert + S-COSMOS

Importance of MIPS data for identification of optically faint AGN (see Fabrizio’s talk)

IRAC 3.6 IRAC 4.5

IRAC 8.0 ACSACS

IRAC 3.6 IRAC 4.5

IRAC 8.0


IRAC 3.6 IRAC 4.5

IRAC 8.0

ACS

Both can be counterpartsTry to put BOTH in slits In spectroscopic programs

Examples of XMM/IRAC coincidenceson bright/ambiguous sources

IRAC 3.6 IRAC 4.5

IRAC 8.0

ACS

~100 objects in XMM-COSMOS with multiple/none IRAC cps more accurate X-ray positions needed to pick up the

right cp C-COSMOS

Courtesy: Salvato, Ilbert + S-COSMOS


compilation from ongoing spectroscopic projects [IMACS/zCOSMOS + SDSS + literature data] ~380 “secure”

spectroscopic identifications (z>0)

[25% of the full sample, 50% completeness in the I<22 sample]

BL AGNs dominate at z>1 High redshift type 2

objects missing (partly selection effect)

[see also results from HELLAS2XMM, Cocchia et al. 2006 and from the SEXSI survey, Eckart et al. 2006]

Redshift distribution

Brusa et al. 2007 ApJS


Optical/IR Colors of X-ray sources (1)

Brusa et al. 2007, ApJS

Lacy et al. 2004 locus

Stern et al. 2005locus

BL AGN occupy the classic QSO locus in UBBV diagrams and are mostly (80%) associated with pointlike sources

(Updated)

BL AGN (from spectroscopy) occupy the expected locus also in IRAC diagrams (steep PL SED)

See also results in Heng Hao poster


Optical/IR Colors of X-ray sources (2)

Lacy et al. 2004 locus

Obscured sources (NOT BL AGN and hardsources) are preferentially associated with“red” objects

IRAC colours of NL AGN (RED) and galaxies(CYAN) show significant contribution from host galaxy light Optically faint (i>25 or undetected) sources have steep PL SED OBSCURED AGN

Brusa et al. 2007ApJS

(“dichotomy” confirmed by spectral analysis, Mainieri et al. 2006)


Full multiwavelength coverage needed to:

- correctly identify the X-ray counterparts (at least for XMM!)

- properly study and characterize AGN population as a whole

First results from XMM-COSMOS

- logN-logS: excellent agreement with XRB modeling (Cappelluti et al. 2007)

- multicolor analysis of the “optically bright sample” suggests 80% agreement between spectroscopic, morphological and X-ray properties (as expected from unified schemes) – Brusa et al. 2007

- candidate obscured QSOs isolated through K/IRAC photometry among the optically “unidentified” (faint) sources

Summary


Hasinger+2007 Survey description and X-ray properties Cappelluti, Hasinger, Brusa et al. 2007 Source counts, LogN-LogS Brusa, Zamorani, Comastri, Hasinger et al. 2007 AGN identification, classification + multiwave properties Mainieri+2007 X-ray spectral analysis of point-like sources Miyaji+2007 Angular Correlation Function Finoguenov+2007 Study of groups and clusters in XMM-COSMOS

to appear in an ApJS special issue (2007) http://www.mpe.mpg.de/XMMCosmos/PAPERS/

..and many others projects on-going!including X-EROs (F. Civano), 3-D correlation function (R. Gilli), EXOs (A.

Koekemoer), photoz (M. Salvato), Type 1 QSO host (K. Jahnke) etc.

XMM-COSMOS on-going projects


1) Where do we find all the things you showed? Hasinger+2007 Survey description and X-ray properties Cappelluti, Hasinger, Brusa et al. 2007 Source counts, LogN-LogS Brusa, Zamorani, Comastri, Hasinger et al. 2007 AGN identification, classification + multiwave properties Mainieri+2007 X-ray spectral analysis of point-like sources Miyaji+2007 Angular Correlation Function Finoguenov+2007 Study of groups and clusters in XMM-COSMOS

to appear in an ApJS special issue (2007) http://www.mpe.mpg.de/XMMCosmos/PAPERS/ ..and many others projects on-going!including X-EROs (F. Civano), 3-D correlation function (R. Gilli), EXOs (A.

Koekemoer), photoz (M. Salvato), Type 1 QSO host (K. Jahnke) etc.

2) When will the public data release be? January 2007 (XMM products + multiwave data – ACS, Subaru,

catalogs

FAQ on XMM-COSMOS


First look at ACS morphologiesPointlike

Extended

Images: 20‘‘ x 20‘‘ in size

z=0.552z=0.623

z=0.365

z=1.236 z=1.506 z=2.454z=2.008

z=0.125z=0.044 z=0.349

z=0.863 z=0.969

november, 7 2006cxc extragalactic surveys workshop obscured agn in the cosmos field: the...

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