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Obscured and unobscured growth of Super-massive Black Holes from the XMM-Newton Medium Survey

Obscured and unobscured growth of Super-massive Black Holes from the XMM-Newton Medium Survey. Francisco J. Carrera, X. Barcons, J. Bussons, J. Ebrero, M. Ceballos, A. Corral (IFCA, CSIC-UC, Spain) and many SSC colleagues. SSC#20, Potsdam, Nov. 13, 2006. NGC4291.

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Obscured and unobscured growth of Super-massive Black Holes from the XMM-Newton Medium Survey

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  1. Obscured and unobscured growth of Super-massive Black Holesfrom the XMM-Newton Medium Survey Francisco J. Carrera, X. Barcons, J. Bussons, J. Ebrero, M. Ceballos, A. Corral (IFCA, CSIC-UC, Spain) and many SSC colleagues SSC#20, Potsdam, Nov. 13, 2006

  2. NGC4291 Definition of the AXIS survey Carrera et al 06 Mrk 205 • 36 XMM-Newton target fields: • Galactic latitude |b|>20 deg • X-ray observations with EPIC-pn detector in FULL-FRAME-MODE • ~Avoided fields with bright and/or extended targets • Good time intervals > 10 ksec • Available early on in the mission • Areas around target + OOT+ near the pn CCD gaps excluded • Solid angle ~4.8 deg2 • Using SAS v6.1.1 to produce final source list and products: • Exposure and background maps • Source detection • Spectra and calibration matrices • Own empirical sentitivity maps from detected source parameters • Very detailed source screening • Total of 1433 distinctX-ray sources with detection likelihood >15 in any of 4 bands (see below)

  3. Soft 0.5-2 keV XID 0.5-4.5 keV Hard 2-10 keV Ultrahard 4.5-7.5 keV X-ray source counts (BSS/HBS Della Ceca et al. 2004 & CDF Bauer et al. 2004 & AMSS Ueda et al. 2005)

  4. Deep Medium Shallow The contribution to the X-ray background Surveys Medium surveys resolve the brightest 50% of the X-ray background XID Hard Soft Ultra-hard

  5. Angular clustering • Detected significant (>99%) clustering in soft/XID: • In whole sky • No clustering in hard/ultrahard: because not enough sources? • No clustering in hard-spectrum sources

  6. The XMS samples Barcons et al. 07 • Subset of AXIS: • 25 fields chosen for follow-up: 3.3 deg2 • Flux limited in Soft, Hard and XID: total of 318 sources

  7. Optical identification of the XMS • Optical imaging: g,r,i (SDSS), Z (Gunn), mostly at the INT/WFC to r~23-24mag • Reliable & unique candidate counterpart in r/i for virtually all sources (< 5” or < 5): only 5 “empties” • Optical spectroscopy • 50% from AXIS programme (WHT, TNG, NOT): multi-fibre and long-slit spectroscopy • 20% from Calar Alto/3.5m long-slit spectroscopy • 15% from VLT/FORS2 long-slit spectroscopy • A few from AAT/2dF, SUBARU/FOCAS, SAO and others

  8. 10m spec lim 4m spec lim Deep Medium Shallow Full sample

  9. Breakdown of identified sources

  10. Redshift distribution Soft Peak of QSO distribution (z~1.5) well sampled. # z Hard Obscured population out to z~1 in Hard sample # z

  11. QSO-2 @ z=2.2 All galaxies consistent with hosting AGN LX>1042 erg/s: obscured AGN Luminosities and redshifts log(LSoft cgs) Soft QSOs z log(LHard cgs) “Seyferts” Hard z

  12. (Preliminary) X-ray spectral analysis NH Full sample z • Extracted X-ray spectra (pn+MOS) for all 318 sources • Fitted Gal. abs. * power law • Fitted Gal. abs. * Intrinsic abs. * power law • F-test 95%: X-ray absorbed 72 Filled symbols • 12 BLAGN • 17 NELG • 5 Gal

  13. (Preliminary) X-ray spectral analysis 16/35 unidentified sources X-ray absorbed (obscured AGN?) Full sample

  14. AXIS+XMM-2dF NELGs AXIS+XMM-2dF BLAGN Averaging X-ray spectraCorral et al., in preparation • Procedure still being tested • Selecting X-ray spectra with >80cts • Unfolding with best fit Galactic+Intrinsic absorption power law • De-absorbing (correcting for Galactic NH) • De-redshifting • Renormalizing using flux in 2-8 keV band • Averaging in final bins (≥500 cts) • Averaging AXIS: • BLAGN (200 sources) • NELG (43) • Much improved averaging AXIS+XMM-2dF: • BLAGN (549): =1.95±0.02 Fe line @6.5±0.2 keV EW=130±60 eV: ~3 • NELG (113): =1.53±0.02 Fe line @6.6±0.4 keV EW=130±100 eV: <~2

  15. AXIS+XMM-2dF NELGs AXIS+XMM-2dF BLAGN Averaging X-ray spectraCorral et al., in preparation • Procedure still being tested • Selecting X-ray spectra with >80cts • Unfolding with best fit Galactic+Intrinsic absorption power law • De-absorbing (correcting for Galactic NH) • De-redshifting • Renormalizing using flux in 2-8 keV band • Averaging in final bins (≥500 cts) • Averaging AXIS: • BLAGN (200 sources) • NELG (43) • Much improved averaging AXIS+XMM-2dF: • BLAGN (549): =1.95±0.02 Fe line @6.5±0.2 keV EW=130±60 eV: ~3 • NELG (113): =1.53±0.02 Fe line @6.6±0.4 keV EW=130±100 eV: <~2

  16. Tips for statistical identification 90% unobscured AGN log(FHard/Fopt) ~90% Obscured AGN (most Xabs) Stars Full sample HR2

  17. FX/Fopt >10 X-ray to optical ratio: a marker for obscuration? log(FSoft/Fopt) • 5% of sources with FX/Fopt>10 • ≥40% of FX/Fopt>10 obscured AGN Soft FX(10-14cgs) log(FHard/Fopt) Hard • 15% of sources with FX/Fopt>10 • ~70% of FX/Fopt>10 obscured AGN FX(10-14cgs)

  18. E+S0 E+S0 QSOs S+Irr QSOs S+Irr 10% of QSOs are red Optical colours r-i g-r g-r Soft Hard #

  19. Softer Redder Optical versus X-ray “colours”: Hard Harder sources are >90% obscured AGN Softer sources: Optically blue: unabsorbed AGN Optically red: mix of abs & unabs AGN g-r Hard HR2

  20. On-going work • Brightest 50% of the X-ray background dominated by AGN. • Unobscured accretion dominates, but increasingly important contribution from obscured objects. • X-ray absorption and optical obscuration not equivalent: • 10% of type 1 AGN are X-ray absorbed • 15% of type 2 AGN are not X-ray absorbed • 25% of FX/Fopt>10 hard X-ray sources are type 1 AGN • 10% of X-ray selected type 1 AGN have red colours • Even at medium fluxes, an important fraction of the X-ray sources have optically faint and red optical counterparts: • Need 10m class observing time • Most unIDed objects faint (r/i>21.5) and Xabs: NELGs? • Results from average spectra show Fe lines in both BLAGN and NELGs

  21. Publications • Carrera et al. 2006 (submitted): X-ray catalogue of AXIS sources • logN-logS • angular correlation • Answer from the referee ~OK: expected re-submission by end of year • Corral et al. 2007 (in prep.): spectral stacking analysis of AXIS and XMS sources (+2dF?) • Barcons et al. ~2007: XMS IDs and col-col plots • Ebrero et al. ~2007: luminosity function • Bussons et al. ~2007: SEDs • ?? et al. ~2007: statistical IDs with 2dF?

  22. Observing proposals • Submitted: • SAO/6m 6 nights March: XMS/UH mag>21.5 • CAHA/3.5m Omega2000: wide-field IR im. • XMM: deep look (200ks) at 4 Compton-thick candidates • Planned: • CAHA/3.5m Omega2000: wide-field/QSO2 IR im. • VLT/VIMOS LBQS2212?: MOS spectroscopy

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