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HST Workshop Bologna Jan 31, 2008HST Workshop Bologna Jan 31, 2008
Heavily obscured Heavily obscured SMBH at high SMBH at high
redshiftredshift
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, 2008HST Workshop Bologna Jan 31, 2008
OutlineOutlineAccreting 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, 2008HST Workshop Bologna Jan 31, 2008
AGN and galaxy co-AGN and galaxy co-evolutionevolution
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
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, 2008HST Workshop Bologna Jan 31, 2008
Evidences for missing SMBH
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, 2008HST Workshop Bologna Jan 31, 2008
Highly obscured AGNHighly 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)
HST Workshop Bologna Jan 31, 2008HST Workshop Bologna Jan 31, 2008
135 sources (out of 1729 with F24 > 40 Jy) 22 detected by Chandra <LX>=43.4+/-0.3, <NH>=22.9+/-0.8, <z>~2.1 LogF(1.5-4keV) stacked sources= -- 17 @z~2 logLobs(2-8keV) stacked sources ~41.8 log<L (6 m) > ~ 44.6 ==> logL(2-8keV) unabs.~43 Difference implies logNH > 24
135 sources (out of 1729 with F24 > 40 Jy) 22 detected by Chandra <LX>=43.4+/-0.3, <NH>=22.9+/-0.8, <z>~2.1 LogF(1.5-4keV) stacked sources= -- 17 @z~2 logLobs(2-8keV) stacked sources ~41.8 log<L (6 m) > ~ 44.6 ==> logL(2-8keV) unabs.~43 Difference implies logNH > 24
Fiore+08
“Mildly” CT AGN Absorption by CT gasmay be key ingredientof feedback mechanism
Daddi+07
IR-optical IR-optical
HST Workshop Bologna Jan 31, 2008HST Workshop Bologna Jan 31, 2008
CT AGN onlybarely sampledby deep Chandra and XMM surveys
Relative fraction steeply increasing
Hard (> 10 keV) surveys more efficient
Redshift distribution <z> ~ 0 @ 10-11
<z> ~ 1 @ 10-15
X-ray X-ray
HST Workshop Bologna Jan 31, 2008HST Workshop Bologna Jan 31, 2008
XMM Ultradeep field XMM Ultradeep field
XMM simulation
~ 370 ks already available
~ 1.3 Ms in 2008
Aim at 3 Ms
Chandra 2 Ms just completed (PI W.N. Brandt)
Aim at 4-5 Ms
HST Workshop Bologna Jan 31, 2008HST Workshop Bologna Jan 31, 2008
Optically faint/Undetected
Optically faint/Undetected
Rodighiero+07
Brusa, Fiore+08Koekemoer+04EXOsCandidate z > 6More likely z~2-3
HST Workshop Bologna Jan 31, 2008HST Workshop Bologna Jan 31, 2008
Host galaxy morphologies Host galaxy morphologies
ACS cutoutsof two Type 2AGN in the z ~ 0.7CDFS LSSType 2 AGN at higher redshiftBrusa,Fiore+08
•Koekemoer+02
•Grogin+03
•Schreier+01
HST Workshop Bologna Jan 31, 2008HST Workshop Bologna Jan 31, 2008
K
K-band (ISAAC@VLT) residuals after deconvolution without and with the central component
Z ~ 0.1 - 0.2 !!!
Galaxy:J=16.52±0.01K=15.25±0.01AGN:J=20.30±0.35K=18.09±0.10
Galaxy:J=16.92±0.05K=15.21±0.01AGN:J=20.75±0.29K=18.39±0.24
K
Host galaxy morphologies Host galaxy morphologies
Civano+07
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 ?
Very faint or undetected --> very high-z AGN ?
Summary Summary