The evolution of SMBH from Hard X-ray surveys Andrea Comastri (INAF – Osservatorio di Bologna – Italy) The XRB as a tracer of SMBH mass densit Hard X-ray surveys: observational resul Near-IR observations of hard X-ray sour Evidences of merging Conclusions and perspectives
The evolution of SMBH from Hard X-ray surveys. The XRB as a tracer of SMBH mass density Hard X-ray surveys: observational results Near-IR observations of hard X-ray sources Evidences of merging Conclusions and perspectives. Andrea Comastri (INAF – Osservatorio di Bologna – Italy). - PowerPoint PPT Presentation
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The evolution of SMBH from Hard X-ray surveys
Andrea Comastri (INAF – Osservatorio di Bologna – Italy)
•The XRB as a tracer of SMBH mass density•Hard X-ray surveys: observational results•Near-IR observations of hard X-ray sources•Evidences of merging•Conclusions and perspectives
Hard X-ray Surveys
Most direct probe of the super-massive black hole (SMBH) accretion activity recorded in the XRB spectral energy density
Chandra and XMM surveys: SMBH census is almost complete (integral) obscured AGN make the bulk of the XRB
The light-up and evolution of obscured accreting SMBH is still largely unknown
(differential) XLF evolution of obscured AGN
The deepest X-ray sky
HDFN (Brandt et al. 2001) CDFS (Giacconi et al. 2002)
Chandra Surveys, 1 Ms exposures
The origin of the cosmic XRBA truly diffuse component not exceeding 10% of
the observed flux (warm IGM, missing baryons …) may still be present in the soft (below 2 keV) X-ray band
the hard XRB (2-100 keV) is due to single sources (X-ray surveys, CMB argument)
OBSCUREDAGN
SMBH mass density from XRB (Fabian & Iwasawa 1999)
Where all the SMBH have gone ? N(L), N(z), efficiency, bolometric correction ?
DEEP FIELDS: Redshift Distributions
•CDFS, Gilli 2003•CDFN, Barger et al. 2002
Cosmic Sheets
Z=0.67
•CDFS •CDFN
X-ray source clusteringYang et al. 2003 (astro-ph/0302137)
•Hard X-raysources more clustered thansoft ones
•Gilli et al. 2003 (astro-ph/0304177)
The same LSS is traced by both X-ray and near IRsurveys
Luminosity function:
•Cowie et al. 2003astro-ph/0301231
•Hasinger 2003astro-ph/0302574
Space density:
•Cowie et al. 2003: rho_BH ~ 2x105
•Hasinger 2003
Deep Chandra surveys: limits
Small solid angle lack of high z high L objects
Soft X-ray response biased against highly obscured objects
Limited by faint optical counterparts and thus incomplete at high-z
The Hellas2XMM survey Wide and shallow: 3 deg2 (15 XMM public fields)
~30 sources/field, Fx>10-14
Bulk of the XRB Rare and peculiar sources, avoid cosmic variance