Definition of the AXIS survey (Carrera et al 06) The XMS samples (Barcons et al. 07) The content of the XMS Redshift distribution Luminosities in addition to redshifts

Definition of the AXIS survey (Carrera et al 06) The XMS samples (Barcons et al. 07) The content of the XMS Redshift distribution Luminosities in addition to redshifts

Definition of the AXIS survey (Carrera et al 06) The XMS samples (Barcons et al. 07) The content of the XMS Redshift distribution Luminosities in addition to redshifts

Williams, Randy, Host has reference to this Academic Journal, PHwiki organized this Journal Obscured in addition to 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 Resolving the X-ray background: An XMM-Newton International Survey (AXIS) Definition of the AXIS survey (Carrera et al 06) 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 in addition to /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 in addition to products: Exposure in addition to background maps Source detection Spectra in addition to 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 b in addition to s (see below) Mrk 205

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X-ray source counts (XMM-Newton & Ch in addition to ra & ASCA) The contribution to the X-ray background Surveys Medium surveys resolve the brightest 50% of the X-ray background The XMM-Newton Medium Survey (XMS)

The XMS samples (Barcons et al. 07) Subset of AXIS: 25 fields chosen as long as follow-up: 3.3 deg2 Flux limited in Soft, Hard in addition to XID Optical identification of the XMS Optical imaging: g,r,i (SDSS), Z (Gunn), mostly at the INT/WFC to r~23-24mag Reliable & unique c in addition to idate counterpart in r/i as long as virtually all sources (< 5” or < 5) Optical spectroscopy 50% from AXIS programme (WHT, TNG, NOT): multi-fibre in addition to 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, in addition to others Preliminary results from 2 XMM-Newton fields (~30 sources) in Barcons et al (2002) The content of the XMS Deep Medium Shallow Breakdown of identified sources Redshift distribution Soft Peak of QSO distribution (z~1.5) well sampled. Obscured population out to z~1 in Hard sample Luminosities in addition to redshifts Soft Hard QSOs “Seyferts” Tips as long as statistical identification ~90% Obscured AGN 90% unobscured AGN Stars HR2 log(FHard/Fopt) Obscured in addition to Unobscured AGN X-ray to optical ratio: a marker as long as obscuration Soft 5% of sources with fX/fopt>10 30% of fX/fopt>10 obscured AGN Hard log(FHard/Fopt) 15% of sources with fX/fopt>10 ~70% of fX/fopt>10 obscured AGN log(FSoft/Fopt) FX(10-14cgs) FX(10-14cgs) Optical colours Hard Soft r-i g-r g-r Reddening Fainter X-ray sources are redder FHard(10-14cgs) r-i

Optical versus X-ray “colours”: Hard Hard Harder sources are >90% obscured AGN Softer sources: Optically blue: unabsorbed AGN Optically red: mix of abs & unabs AGN HR2 g-r 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 Mateos et al (2005) 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)

Stacking analysis Averaging X-ray spectra Corral et al., in preparation Procedure still being tested Selecting X-ray spectra with >80cts Unfolding with best fit Gal+Intrinsic abs. p.l. Correcting as long as Galactic NH De-redshifting Renormalizing using flux in 2-8 keV b in addition to 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 Conclusions

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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 in addition to 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 in addition to red optical counterparts. Most unIDed objects faint (r/i>21.5) in addition to extended: NELGs Preliminary results from average spectra show Fe lines in both BLAGN in addition to NELGs

Williams, Randy Host

Williams, Randy is from United States and they belong to WDXX-FM and they are from  Selma, United States got related to this Particular Journal. and Williams, Randy deal with the subjects like Country Music

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