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Obscured and unobscured growth of Super-massive Black Holes

Obscured and unobscured growth of Super-massive Black Holes. Francisco J. Carrera, X. Barcons, J. Bussons, J. Ebrero, M. Ceballos, A. Corral (IFCA, CSIC-UC, Spain) & XMM-Newton Survey Science Centre (S. Mateos, M. J. Page, M.G. Watson, J. Tedds, R. Della Ceca ...).

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Obscured and unobscured growth of Super-massive Black Holes

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  1. Obscured and unobscured growth of Super-massive Black Holes Francisco J. Carrera, X. Barcons, J. Bussons, J. Ebrero, M. Ceballos, A. Corral (IFCA, CSIC-UC, Spain) & XMM-Newton Survey Science Centre (S. Mateos, M. J. Page, M.G. Watson, J. Tedds, R. Della Ceca ...) Extragalactic X-ray Surveys, Boston, November 6, 2006

  2. Resolving the X-ray background:An XMM-Newton International Survey (AXIS)

  3. 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 • 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 • Areas around target + OOT+ near the pn CCD gaps excluded • Own empirical sentitivity maps from detected source parameters • Very detailed source screening • Total of 1433 distinct X-ray sources with detection likelihood >15 in any of 4 bands (see below)

  4. 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 (XMM-Newton & Chandra & ASCA)

  5. Deep Medium Shallow The contribution to the X-ray background Surveys Medium surveys resolve the brightest 50% of the X-ray background

  6. The XMM-Newton Medium Survey(XMS)

  7. 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

  8. 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) • 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, and others • Preliminary results from 2 XMM-Newton fields (~30 sources) in Barcons et al (2002)

  9. The content of the XMS

  10. 10m spec lim 4m spec lim Deep Medium Shallow

  11. Breakdown of identified sources

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

  13. QSO-2 @ z=2.2 All galaxies consistent with hosting AGN LX>1042 erg/s Luminosities and redshifts Soft QSOs Hard “Seyferts”

  14. Tips for statistical identification 90% unobscured AGN log(FHard/Fopt) ~90% Obscured AGN Stars HR2

  15. Obscured and Unobscured AGN

  16. FX/Fopt >10 X-ray to optical ratio: a marker for obscuration? log(FSoft/Fopt) • 5% of sources with fX/fopt>10 • 30% of fX/fopt>10 obscured AGN Soft FX(10-14cgs) log(FHard/Fopt) • 15% of sources with fX/fopt>10 • ~70% of fX/fopt>10 obscured AGN Hard FX(10-14cgs)

  17. 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 #

  18. Reddening Fainter X-ray sources are redder? r-i FHard(10-14cgs)

  19. Softer 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. X-ray absorption vs obscuration: not equivalent • The XMS survey • 10% of type 1 AGN are absorbed • (with NH<1022 cm-2) • >40% of type 2 AGN are absorbed • The Lockman Hole survey • 15% (<30% at 3) of type 1 AGN • are absorbed (with NH<1022 cm-2) • 80% (>50% at 3) of type 2 AGN • are absorbed. But 5/28 are unabsorbed Mateos et al (2006) Mateos et al (2005)

  21. Stacking analysis

  22. 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 Gal+Intrinsic abs. p.l. • 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 (see Xu, Mateos): • BLAGN (549): =1.95±0.02 Fe line @6.5±0.2 keV EW=130±60 eV • NELG (113): =1.53±0.02 Fe line @6.6±0.4 keV EW=130±100 eV

  23. Conclusions

  24. 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. • Most unIDed objects faint (r/i>21.5) and extended: NELGs • Preliminary results from average spectra show Fe lines in both BLAGN and NELGs

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