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Boston, November 2006 Extragalactic X-ray surveys. Spectral analysis of X-ray sources in the CDFS. Paolo Tozzi. 0.3-1 keV 1-3 keV 3-7 keV. Detailed spectral analysis of X-ray sources Tozzi, Gilli, Mainieri et al. 2006, A&A, 451, 457. Rosati et al. 2002 National Geographic, Dec 2002. - PowerPoint PPT Presentation
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Boston, November 2006Extragalactic X-ray surveys
Paolo Tozzi
Spectral analysis of X-ray sources
in the CDFS
0.3-1 keV
1-3 keV
3-7 keV
Rosati et al. 2002
National Geographic, Dec 2002
Detailed spectral analysis of X-ray sources
Tozzi, Gilli, Mainieri et al. 2006, A&A, 451, 457
Deep X-ray Surveys: some open issues
The distribution of intrinsic absorption among AGN
Detection of Compton-Thick AGN
The unresolved fraction of the XRB at high energies
Compton thick candidates
NH vs redshifts for the whole sample
Detected fraction as a function of NH and z
Sampling different luminosity and spectral population at different zSelection effects are relatively easy to model in the X-ray band
z < 0.7
0.7 < z <1.5
z > 1.5
NH histogram corrected for completeness
Corrected for completenessand sources outside the detectability region
<log(NH)> ~ 23.1
dispersion = 1.1
5% C-thick (14 reflection+4 sources N
H>1.5 1024 cm-2)
density ~ 200 +- 50 deg-2
in agr w XRB model byGilli, Comastri, Hasinger (2006)
NH distribution vs Optical Type
Whole sample (321)Cthick candidates (14)
Consistent with evolutionary sequence:pre-QSO phaseC-thin absorbed QSO (QSOII @ high z)unobscured QSO activityquiescent spheroidal galaxyAlexander et al. 2005; Stevens et al. 2005
Model: Granato et al. 2005
Part of the missing XRB is fromintermediate z strongly absorbedmoderate luminosity, possibly C-thick sources, in a secondary, relatively low-z phase of accretion(see “downsizing” or anti-hierarchical behaviour)
Whole sample (321)QSOII (44)
Missing XRB: NH=4.5 1023 cm-2 @ z=0.8
~50% not resolved yet for E> 5 keV(Worsley et al. 2004, 2005)
The unresolved fraction increases with the energy band
Compute the contribution of the absorbed sources to the XRB
NH > 1022 cm-2
NH > 1023 cm-2
Worsley et al. 2004This work
After computing the skycoverage according to the spectral shape of each source
CONCLUSIONSDetailed X-ray Spectral Analysis of faint X-ray sources:
Towards an universal distribution of intrinsic absorption (selection effects can be easily modelled in X-rays)
>~80% of the AGNs agree with simple unification models (TypeI/TypeII Unobscured/Obscured corr.)
Evidence for strongly absorbed, C-thick sources @ z~1, and a substantial QSOII population at z>~2
Part of the missing XRB is already observed in agreement with most recent XRB synthesis models
C-thick candidates in IRAC/MIPS colors
Use secure spectral identifications in CDFS and CDFN
Norman et al. 2004
29 galaxies with good spectra in the CDFS and emission line ratios consistent with starbursts or normal galaxies give the X-ray priors. A Bayesian approach allows us to identify 74 galaxies in the CDFS and 136 in the CDFN (2 Ms)
SFR densities
Compilation from Tresse et al. 2002:
Gallego et al. 1995 (H )
Gronwall 1999
Hopkins et al. 2000
Pascual et al. 2001
Tresse et al. 2002
Sullivan et al. 2000
Lilly et al. 1996
Lines from 60 m
Saunders et al. 1990, Takeuchi et al. 2003
Norman et al. 2004
XLF consistent with a PLE ~ (1+z)2.7
Consistent with an evolution of SFR (1+z)2.7 for 0<z<1.
XLF of Star Forming Galaxies is a goal for future X-ray missions (Con-X, XEUS)
Daddi et al. 2004
K20 survey
IR selected galaxies at z~2 with massive SF
Daddi et al. 2004
Stacked image of 23 BzK galaxies; HR< -0.5 @ 2sigma ; L2-10
~1042 erg/secSFR ~ 170 M⊙ yr-1 (4 higher than LBG). SFRD of 0.04 M⊙ /yr/Mpc3
We are witnessing the massive spheroid formation epoch(the peak of just the low-z tail?)
Soft Hard
The evolution of the obscured fraction with redshift
This work
Ueda et al. 2003
Average NH artificially increases towards high-z
Tozzi, Gili, Mainieri et al. 2006
NH ~ 1020cm-2
150 and 80 net counts
Ueda et al 2003Hasinger et al. 2005
Luminosity dependent density evolution:downsizing or anti-hierarchical behaviour
ExtendedCDFS
PI N. Brandt~1000 sources(Lehmer et al. 2005)
1Ms+
4 X 240 ks
AGN Contribution to the hard XRB
CDFS (1Ms): XRB(S> 4.5×10 -16) = (1.70±0.15)×10 -11 erg s -1cm -2deg -2
90% resolved in 0.5-2 keV93% resolved in 2-8 keVAGN contribution83% in 0.5-2 keV95% in 2-8 keV(Bauer et al. 2004)
CDFN (2Ms): XRB(S> 2 ×10 -16) = (2.07±0.15)×10 -11 erg s -1cm -2deg -2
Worsley et al. 2004; 2005Missing XRB: NH=4.5 1023 cm-2 @ z=0.8
~50% not resolved yet for E> 5 keV(Worsley et al. 2004, 2005)
The unresolved fraction increases with the energy band
Compute the contribution of the absorbed sources to the XRB
Worsley et al. 2004This work
After computing the skycoverage according to the spectral shape of each source