November, CXC Extragalactic Surveys workshop 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)

November, CXC Extragalactic Surveys workshop Motivation of the XMM-COSMOS project Deep multiwavelength coverage needed to properly study and characterize AGN population as a whole: selection criteria  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 (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“ „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 Massive Redshift campaigns High resolution optical data

November, CXC Extragalactic Surveys workshop + MAMBO, CFHT, Bolocam and (future) others COSMOS major components (in order of appearance) : HST/ACS (I-band – 590 orbits – I(AB)~27) : 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 – cgs) : 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 Survey 2 deg 2 (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 XMM-Newton PI: G. Hasinger Hasinger et al soft keV medium keV hard keV C-COSMOS 1.8 Ms (PI M. Elvis)

November, CXC Extragalactic Surveys workshop XMM-COSMOS 2 deg Flux 2-10 keV (cgs) CDFN-CDFS 0.1deg2 Barger et al. 2003; Szokoly et al EGS/AEGIS 0.5deg2 Nandra et al HELLAS2XMM 1.4 deg2 Cocchia et al Champ 1.5deg2 Silverman et al XBOOTES 9 deg2 Murray et al. 2005, Brand et al XMM-COSMOS in a context SEXSI 2 deg2 Eckart et al Area (see Brandt & Hasinger 2005 review (ARA&A 43, 827) C-COSMOS 0.9 deg2 E-CDFS 0.3deg2 Lehmer et al ELAIS-S1 0.5deg2 Puccetti et al. 2006

November, CXC Extragalactic Surveys workshop COSMOS source counts logN-logS (normalized to Euclidean slope)  keV Confirm previous results with unprecedent accuracy in the flux range 8x x cgs:  5-10 keV In between previous determinations in the flux range x 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

November, CXC Extragalactic Surveys workshop 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 mag  large spread on X/O ratios for X-ray sources

November, CXC Extragalactic Surveys workshop Brandt & Hasinger 2005 Extreme X-ray/optical objects EXOs Optical identification X/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 and many others!] ~1300 sources

November, CXC Extragalactic Surveys workshop IRAC 3.6IRAC 4.5 IRAC 8.0ACS ~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 3.6IRAC 4.5 IRAC 8.0ACS IRAC 3.6IRAC 4.5 IRAC 8.0

November, CXC Extragalactic Surveys workshop IRAC 3.6 IRAC 4.5 IRAC 8.0 ACS Both can be counterparts  Try to put BOTH in slits In spectroscopic programs Examples of XMM/IRAC coincidences on 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

November, CXC Extragalactic Surveys workshop 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 and from the SEXSI survey, Eckart et al. 2006] Redshift distribution Brusa et al ApJS

November, CXC Extragalactic Surveys workshop Optical/IR Colors of X-ray sources (1) Brusa et al. 2007, ApJS Lacy et al locus Stern et al locus 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

November, CXC Extragalactic Surveys workshop Optical/IR Colors of X-ray sources (2) Lacy et al locus Obscured sources (NOT BL AGN and hard sources) 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 ApJS (“dichotomy” confirmed by spectral analysis, Mainieri et al. 2006)

November, CXC Extragalactic Surveys workshop 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 candidate obscured QSOs isolated through K/IRAC photometry among the optically “unidentified” (faint) sources Summary

November, CXC Extragalactic Surveys workshop  Hasinger+2007 Survey description and X-ray properties  Cappelluti, Hasinger, Brusa et al Source counts, LogN-LogS  Brusa, Zamorani, Comastri, Hasinger et al 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) 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

November, CXC Extragalactic Surveys workshop 1) Where do we find all the things you showed?  Hasinger+2007 Survey description and X-ray properties  Cappelluti, Hasinger, Brusa et al Source counts, LogN-LogS  Brusa, Zamorani, Comastri, Hasinger et al 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) 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

November, CXC Extragalactic Surveys workshop First look at ACS morphologies Pointlike Extended Images: 20‘‘ x 20‘‘ in size z=0.552 z=0.623 z=0.365 z=1.236 z=1.506 z=2.454 z=2.008 z=0.125 z=0.044 z=0.349 z=0.863 z=0.969

November, CXC Extragalactic Surveys workshop COSMOS major components : HST/ACS (i-band – 590 orbits – I(AB)~27) Subaru imaging (~25 nights, b,v,r,i,z,) VLT (540 hours) & Magellan (12 nights) XMM-Newton (1.4 Ms) VLA (265 hours) GALEX deep (200 ks, AB~25) SPITZER (200 hours) all underway ! + MAMBO, CFHT, TNG and others

November, CXC Extragalactic Surveys workshop 1390 X-ray sources (from 23 fields sample) Identification in the optical (I) band using a statistical method to match the X-ray error box to the most likely optical cp (“likelihood ratio technique”, Sutherland & Saunders 1992 ) Method tested and described in Brusa et al. ApJS paper Refined with the (old) K-band catalog (but too shallow..) - “identified” sample (optically/secure identified, 80%)  quite solid, large sample  statistical properties (colors/redshifts/morphologies/selection effects) - “ambiguous/unidentified” sample (problems with ID, 20%)  most interesting sources  candidate high-z, obscured QSO Optical identifications in XMM-COSMOS

November, CXC Extragalactic Surveys workshop Examples of XMM/IRAC coincidences ~120 objects in XMM-COSMOS identified through K and/or IRAC (most of them EROs) Very hard to get redshift from optical  alternative approaches: ISAAC/IRS spectroscopy and/or SED fitting [Maiolino et al. 2006, Koekemoer et al. 2004] [ Cfr. Also sample of highly obscured objects in Martinez Sansigre et al. 2005] ACSIRAC 3.6 micron (Courtesy M. Salvato, D. Sanders)

November, CXC Extragalactic Surveys workshop [First] morphological test on identifications About 50% of the IDs have stellar (or almost stellar; FWHM<3 pixels) profile on ACS data blue points = pointlike red points = extended Very soft (HR=-1) sources are mostly point-like (dashed histogram) Very hard (HR=1) sources are preferentially associated with extended objects (solid histogram) ACS morphological information Brusa et al. 2006

November, CXC Extragalactic Surveys workshop U-B vs. B-V diagram The majority (80%) of stellar-like objects from ACS occupy the locus of quasars in the U-B vs. B-V diagram Conversely, >70% of UBV selected objects recovered in the X-rays (90-100% expected with the completion of XMM-COSMOS) Additional 50% (not shown) classified as extended  missed in color selected diagrams Colors of X-ray sources (1) Brusa et al. 2006

November, CXC Extragalactic Surveys workshop R-K vs. K Very soft (HR=-1) sources are mostly associated with “blue” sources (dashed histogram) Hard sources (HR>-0.3) are preferentially associated with red objects (solid histogram) Extended sources are significantively “redder” than point-like and associated with NOT BL AGN (“dichotomy” confirmed by spectral analysis Mainieri et al. 2006) See Francesca’s talk! Brusa et al Colors of X-ray sources (2) (AB mag)