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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 ...

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Obscured AGN in the COSMOS field: the multiwavelength challenge

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  1. 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) CXC Extragalactic Surveys workshop

  2. 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 Massive Redshift campaigns High resolution optical data Large, contiguous area • 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 CXC Extragalactic Surveys workshop

  3. 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 Survey 2deg2 (PI: N. Scoville) XMM-Newton PI: G. Hasinger soft 0.5-2.0 keV medium 2.0-4.5 keV hard 4.5-10.0 keV Hasinger et al. 2007 C-COSMOS 1.8 Ms (PI M. Elvis) 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 + MAMBO, CFHT, Bolocam and (future) others CXC Extragalactic Surveys workshop http://www.astro.caltech.edu/cosmos/

  4. XMM-COSMOS in a context CDFN-CDFS 0.1deg2 Barger et al. 2003; Szokoly et al. 2004 -16 E-CDFS 0.3deg2 Lehmer et al. 2005 EGS/AEGIS 0.5deg2 Nandra et al. 2006 C-COSMOS 0.9 deg2 -15 ELAIS-S1 0.5deg2 Puccetti et al. 2006 Flux 2-10 keV (cgs) XMM-COSMOS 2 deg2 HELLAS2XMM 1.4 deg2 Cocchia et al. 2006 Champ 1.5deg2 Silverman et al. 2005 -14 SEXSI 2 deg2 Eckart et al. 2006 -13 XBOOTES 9 deg2 Murray et al. 2005, Brand et al. 2005 CXC Extragalactic Surveys workshop Area (see Brandt & Hasinger 2005 review (ARA&A 43, 827)

  5. 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 CXC Extragalactic Surveys workshop

  6. 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 CXC Extragalactic Surveys workshop

  7. 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 CXC Extragalactic Surveys workshop Brandt & Hasinger 2005

  8. From optical bands to IRAC/MIPS IRAC 3.6 IRAC 4.5 IRAC 3.6 IRAC 4.5 IRAC 8.0 ACS IRAC 8.0 ACS Courtesy: Salvato, Ilbert + S-COSMOS • ~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 IRAC 3.6 IRAC 4.5 IRAC 8.0 ACS • Importance of MIPS data for identification of optically faint AGN (see Fabrizio’s talk) CXC Extragalactic Surveys workshop

  9. Examples of XMM/IRAC coincidenceson bright/ambiguous sources • ~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 4.5 IRAC 3.6 IRAC 4.5 IRAC 3.6 IRAC 8.0 IRAC 8.0 ACS ACS Courtesy: Salvato, Ilbert + S-COSMOS • Both can be counterparts • Try to put BOTH in slits In spectroscopic programs CXC Extragalactic Surveys workshop

  10. Redshift distribution 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] Brusa et al. 2007 ApJS CXC Extragalactic Surveys workshop

  11. 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 Stern et al. 2005 locus (Updated) Brusa et al. 2007, ApJS See also results in Heng Hao poster CXC Extragalactic Surveys workshop

  12. Optical/IR Colors of X-ray sources (2) 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. 2007 ApJS Lacy et al. 2004 locus (“dichotomy” confirmed by spectral analysis, Mainieri et al. 2006) CXC Extragalactic Surveys workshop

  13. Summary • 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 CXC Extragalactic Surveys workshop

  14. XMM-COSMOS on-going projects • 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. CXC Extragalactic Surveys workshop

  15. FAQ on XMM-COSMOS 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 CXC Extragalactic Surveys workshop

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

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