Obscured AGN in the COSMOS field the multiwavelength

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Obscured AGN in the COSMOS field: the multiwavelength challenge Marcella Brusa (MPE) Collaborators: F.

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. Mc. Cracken, D. Thompson + (optical catalogs) M. Salvato, O. Ilbert, H. Aussel + S-COSMOS (Spitzer) November, 7 2006 CXC Extragalactic Surveys workshop J. Trump + IMACS, S. Lilly + z. COSMOS (redshifts)

Motivation of the XMM-COSMOS project (One of the) Main goal of the XMM-Newton Wide

Motivation of the XMM-COSMOS project (One of the) Main goal of the XMM-Newton Wide field survey in the COSMOS field is: „study the evolution of (obscured) Active Galactic Nuclei over the cosmic time and the dependence of black hole growth on galaxy morphology and environment“ (Hard) X-ray selection Large, contiguous area High resolution optical data Massive Redshift campaigns 1) Deep multiwavelength coverage needed to properly study and characterize AGN population as a whole: Check for selection 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 November, 7 2006 CXC Extragalactic Surveys workshop

Cosmos Survey 2 deg 2 (PI: N. Scoville) COSMOS major components (in order of

Cosmos Survey 2 deg 2 (PI: N. Scoville) COSMOS major components (in order of appearance) : XMM-Newton PI: G. Hasinger 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) S O M S O 2004 -2005: C C XMM-Newton (600 ks)Ms ) 1&. 8 Magellan VLT (540 hours) Elvis(12+ nights) AO 3: 800 ks of XMM [25 x 32 ks pointings] reduction/analysis completed ~1400 AGN detected ~70 clusters/diffuse sources AO 4: 600 ks (Total = 1. 4 Ms) of XMM reduction on-going ~2000 November, sources 7 expected at the 2006 completion of the survey M. hours - ~1 μJy) SPITZER-IRACPI (200 ( 2006: SPITZER-MIPS (200 hours - ~70 μJy) Chandra (1. 8 Ms) + MAMBO, CFHT, Bolocam and (future) others CXC Extragalactic Surveys workshop http: //www. astro. caltech. edu/cosmos/ soft 0. 5 -2. 0 ke. V medium 2. 0 -4. 5 ke. V hard 4. 5 -10. 0 ke. V Hasinger et al. 2007

XMM-COSMOS in a context CDFN-CDFS 0. 1 deg 2 Barger et al. 2003; Szokoly

XMM-COSMOS in a context CDFN-CDFS 0. 1 deg 2 Barger et al. 2003; Szokoly et al. 2004 -16 Flux 2 -10 ke. V (cgs) E-CDFS 0. 3 deg 2 Lehmer et al. 2005 C-COSMOS 0. 9 deg 2 -15 ELAIS-S 1 0. 5 deg 2 Puccetti et al. 2006 XMM-COSMOS 2 deg 2 -14 EGS/AEGIS 0. 5 deg 2 Nandra et al. 2006 HELLAS 2 XMM 1. 4 deg 2 Cocchia et al. 2006 Champ 1. 5 deg 2 Silverman et al. 2005 SEXSI 2 deg 2 Eckart et al. 2006 -13 XBOOTES 9 deg 2 Murray et al. 2005, Brand et al. 2005 November, 7 2006 CXC Extragalactic Surveys workshop (see Brandt & Hasinger 2005 review (ARA&A 43, 827)Area

COSMOS source counts log. N-log. S (normalized to Euclidean slope) 0. 5 -2 ke.

COSMOS source counts log. N-log. S (normalized to Euclidean slope) 0. 5 -2 ke. V Confirm previous results with unprecedent accuracy in the flux range 8 x 10 -16 -5 x 10 -12 cgs: 5 -10 ke. V In between previous determinations in the flux range 10 -14 - 5 x 10 -12 cgs November, 7 2006 Cappelluti et al. 2007 Able to explain most of differences in source counts from different surveys as a combination of Poissonian noise and clustering effects CXC Extragalactic Surveys workshop

From X-ray counts to bolometric properties l (First) Crucial step is X-ray source identification

From X-ray counts to bolometric properties l (First) Crucial step is X-ray source identification assign redshift, investigate extinction properties, derive physical quantities l COSMOS has (or will have soon) all the data to make the source identification at best l “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 November, 7 2006 CXC Extragalactic Surveys workshop

l optically faint (I>24) difficult to identify using optical bands only Optical identification X/O

l optically faint (I>24) difficult to identify using optical bands only Optical identification X/O diagram Ex tre me [see also Alexander et al. 2001] l ~200 sources in the XMMCOSMOS sample: candidate high-z (z>1) obscured QSO, z>4 QSO… l Efficiency of combination of IR+hard X-ray surveys [Mignoli et ra y EX /opt Os ica lo bje ~1300 cts sources al. 2004, Koekemoer et al. 2004, Brusa et al. 2005, Severgnini et al. 2005, Maiolino et al. 2006 and many others!] November, 7 2006 X- CXC Extragalactic Surveys workshop Brandt & Hasinger 2005

From optical bands to IRAC/MIPS Courtesy: Salvato, Ilbert + S-COSMOS l ~100 objects in

From optical bands to IRAC/MIPS Courtesy: Salvato, Ilbert + S-COSMOS l ~100 objects in XMM-COSMOS identified through IRAC (most of them EROs/red objects/optically faint) IRAC 3. 6 l November, 7 2006 IRAC 8. 0 ACS ACS [Koekemoer et al. 2004, Mainieri et al. 2005, Maiolino et al. 2006] See Anton’s talk IRAC 4. 5 Very hard to get redshift from optical alternative approaches: ISAAC/IRS spectroscopy and/or SED fitting IRAC 8. 0 IRAC 3. 6 Importance of MIPS data for identification of optically faint AGN (see Fabrizio’s talk) CXC Extragalactic Surveys workshop

Examples of XMM/IRAC coincidences on bright/ambiguous sources l ~100 objects in XMM-COSMOS with multiple/none

Examples of XMM/IRAC coincidences on bright/ambiguous sources l ~100 objects in XMM-COSMOS with multiple/none IRAC cps more accurate X-ray positions needed to pick up the right cp C-COSMOS IRAC 3. 6 IRAC 4. 5 IRAC 8. 0 ACS Both can be counterparts Try to put BOTH in slits In spectroscopic programs November, 7 2006 IRAC 4. 5 Courtesy: Salvato, Ilbert + S-COSMOS CXC Extragalactic Surveys workshop

Redshift distribution compilation from ongoing spectroscopic projects [IMACS/z. COSMOS + SDSS + literature data]

Redshift distribution compilation from ongoing spectroscopic projects [IMACS/z. COSMOS + SDSS + literature data] l ~380 “secure” spectroscopic identifications (z>0) [25% of the full sample, 50% completeness in the I<22 sample] l BL AGNs dominate at z>1 High redshift type 2 objects missing (partly selection effect) [see also results from HELLAS 2 XMM, Cocchia et al. 2006 and from the SEXSI survey, Eckart et al. 2006] Brusa et al. 2007 Ap. JS November, 7 2006 CXC Extragalactic Surveys workshop

Optical/IR Colors of X-ray sources (1) BL AGN occupy the classic QSO locus in

Optical/IR Colors of X-ray sources (1) BL AGN occupy the classic QSO locus in UBBV diagrams and are mostly (80%) associated with pointlike sources BL AGN (from spectroscopy) occupy the expected locus also in IRAC diagrams (steep PL SED) Lacy et al. 2004 locus (Updated) Stern et al. 2005 locus Brusa et al. 2007, Ap. JS November, 7 2006 See also results in Heng Hao poster CXC Extragalactic Surveys workshop

Optical/IR Colors of X-ray sources (2) Obscured sources (NOT BL AGN and hard sources)

Optical/IR Colors of X-ray sources (2) Obscured sources (NOT BL AGN and hard sources) are preferentially associated with “red” objects Brusa et al. 2007 Ap. JS 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 Lacy et al. 2004 locus (“dichotomy” confirmed by spectral analysis, Mainieri et al. 2006) November, 7 2006 CXC Extragalactic Surveys workshop

Summary l Full multiwavelength coverage needed to: - correctly identify the X-ray counterparts (at

Summary l Full multiwavelength coverage needed to: - correctly identify the X-ray counterparts (at least for XMM!) - properly study and characterize AGN population as a whole l First results from XMM-COSMOS - log. N-log. S: 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 November, 7 2006 CXC Extragalactic Surveys workshop

XMM-COSMOS on-going projects q Hasinger+2007 Survey description and X-ray properties q Cappelluti, Hasinger, Brusa

XMM-COSMOS on-going projects q Hasinger+2007 Survey description and X-ray properties q Cappelluti, Hasinger, Brusa et al. 2007 Source counts, Log. N-Log. S q Brusa, Zamorani, Comastri, Hasinger et al. 2007 AGN identification, classification + multiwave properties q Mainieri+2007 X-ray spectral analysis of point-like sources q Miyaji+2007 Angular Correlation Function q Finoguenov+2007 Study of groups and clusters in XMM-COSMOS to appear in an Ap. JS 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. November, 7 2006 CXC Extragalactic Surveys workshop

FAQ on XMM-COSMOS 1) Where do we find all the things you showed? q

FAQ on XMM-COSMOS 1) Where do we find all the things you showed? q q Hasinger+2007 Survey description and X-ray properties Cappelluti, Hasinger, Brusa et al. 2007 Source counts, Log. N-Log. S q Brusa, Zamorani, Comastri, Hasinger et al. 2007 AGN identification, classification + multiwave properties q Mainieri+2007 q q 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 Ap. JS 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 November, 7 2006 CXC Extragalactic Surveys workshop

First look at ACS morphologies Pointlike z=1. 236 Images: 20‘‘ x 20‘‘ in size

First look at ACS morphologies Pointlike z=1. 236 Images: 20‘‘ x 20‘‘ in size z=1. 506 z=2. 008 z=2. 454 Extended z=0. 044 z=0. 552 November, 7 2006 z=0. 125 z=0. 623 z=0. 365 z=0. 863 CXC Extragalactic Surveys workshop z=0. 349 z=0. 969