HST Workshop Bologna Jan 31, 2008 Heavily obscured Heavily obscured SMBH at high SMBH at high redshift redshift Andrea Comastri INAF - OABologna C. Vignali, R. Gilli, K. Iwasawa, F. Civano, M. Brusa, N. Cappelluti,, F. Fiore, G. Zamorani, W.N. Brandt, X. Barcons, F. Carrera, F. Nicastro, V. Mainieri, H. Brunner, A. Merloni, J. Silverman, P. Rosati, S. Puccetti, P. Tozzi, I.
Heavily obscured SMBH at high redshift. Andrea Comastri INAF - OABologna. C. Vignali, R. Gilli, K. Iwasawa, F. Civano, M. Brusa, N. Cappelluti,, F. Fiore, G. Zamorani , - PowerPoint PPT Presentation
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HST Workshop Bologna Jan 31, 2008
Heavily obscured Heavily obscured SMBH at high SMBH at high redshiftredshiftAndrea ComastriINAF - OABologna
C. Vignali, R. Gilli, K. Iwasawa, F. Civano, M.
Brusa, N. Cappelluti,, F. Fiore, G. Zamorani,
W.N. Brandt, X. Barcons, F. Carrera, F. Nicastro, V. Mainieri, H. Brunner,
A. Merloni, J. Silverman, P. Rosati, S. Puccetti,
P. Tozzi, I. Georgantopoulos
HST Workshop Bologna Jan 31, 2008
OutlineAccreting SMBH represents a key ingredient of AGN/galaxy formation and co-evolution.
AGN census and evolution (the search for the most obscured -Compton Thick- ones)
The Ultradeep XMM - CDFS survey add spectral sensitivity to multi data HST after SM4 (WFC3 - IR channel) Host galaxies morphologies - high z (> 6) obscured QSO
HST Workshop Bologna Jan 31, 2008
AGN and galaxy co-AGN and galaxy co-evolutionevolution
Early on Strong galaxy
interactions= violent star-bursts
Heavily obscured QSOs
When galaxies coalesce accretion peaks QSO becomes
optically visible as AGN winds blow out gas.
Later times SF & accretion
quenched red spheroid,
passive evolution
Most BH mass accreted during luminous AGN phases ! Most bulges passed a phase of activity
AGN hosts (mostly early type morphology) populate the red sequence and green valley
AGN activity persist after SF has ended Many hard sources in the red sequence At variance with model predictions
Mignoli+04HELLAS2XMM
Pozzi+07 See also Silverman+07AGN hosts in the green valley
HST Workshop Bologna Jan 31, 2008
Evidences for missing SMBH
Marconi+04/08
Gilli, AC, Hasinger 07
Compton Thick AGN are predicted to be as numerous as unobscured and less obscured AGN
HST Workshop Bologna Jan 31, 2008
Highly obscured AGN
highly obscured at optical and soft X-ray wavelengths shine in hard X-rays and in the MIR (thanks to the reprocessing of the nuclear radiation by dust)
More than 100 obscured AGN (a few tens CT) will be discovered by XMM & Chandra ultra-deep CDFS surveys
WFC3 - IR deep (AB ~ 28) high resolution observations
Obscured AGN host galaxy morphologiesPick up faint red nuclei Red passive galaxy hosting dying SMBH ?The role of environment (i.e. LSS @ z ~ 0.7) Is AGN feedback responsible of SF quenching ?