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Roberto Decarli. The redshift dependence of the M BH - M host relation in quasars. Max-Planck Institut fuer Astronomie Università degli Studi dell’Insubria. A. Treves R. Falomo M. Labita. J.K. Kotilainen R. Scarpa M. Uslenghi. Decarli et al., 2010a-b, MNRAS 402, 2441 & 2453.
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Roberto Decarli The redshift dependenceof the MBH-Mhost relationin quasars Max-Planck Institut fuer AstronomieUniversità degli Studi dell’Insubria A. TrevesR. Falomo M. Labita J.K. KotilainenR. ScarpaM. Uslenghi Decarli et al., 2010a-b, MNRAS 402, 2441 & 2453 AGN9 Ferrara - May, 26, 2010
MBH – host galaxy relations Gultekin et al. (2009)
MBH – host galaxy relations Blackholes BLR Host galaxies Rinf = G MBH / s*2~ 0.001 Rhost Gultekin et al. (2009)
? ? ? MBH – host galaxy relations Blackholes BLR Host galaxies Rinf = G MBH / s*2~ 0.001 Rhost Gultekin et al. (2009)
Our study • 96 quasars (48 RQQs, 48 RLQs) with 0<z<3 (2x the sample by Peng et al., 2006 and 3x McLure et al., 2006) • Host galaxy luminosity from high res. images • Black hole masses from spectra
Our study • 96 quasars (48 RQQs, 48 RLQs) with 0<z<3 (2x the sample by Peng et al., 2006 and 3x McLure et al., 2006) • Host galaxy luminosity from high res. images • Black hole masses from spectra • For low-z quasars, images in the HST-WFPC2, spectra from the SDSS and HST-FOS and from on-purpose observations at the Asiago 1.82m Telescope. • For z>0.5 targets, images taken at the NOT and the ESO/VLT, spectra from the NOT and ESO/3.6m Telescope.
Virial estimate of MBH • MBH = G-1RBLRvBLR2 • RBLR~ lLla (Kaspi et al., 2000, 2005, 2007) • vBLR = f FWHM
Virial estimate of MBH • MBH = G-1RBLRvBLR2 • RBLR~ lLla (Kaspi et al., 2000, 2005, 2007) • vBLR = f FWHM
QSO PSF
QSO PSF
QSO PSF
QSO PSF
QSO PSF
The MBH–Mhost ratio as a function of z G ≡ MBH/Mhost increases of a factor ~7 from z=0 to z=3 log G = (0.28 ± 0.06) z + - (2.91 ± 0.08) Decarli et al (2010 a,b)
The MBH–Mhost ratio as a function of z G ≡ MBH/Mhost increases of a factor ~7 from z=0 to z=3 log G = (0.28 ± 0.06) z + - (2.91 ± 0.08) Decarli et al (2010 a,b)
The MBH–Mhost ratio as a function of z G ≡ MBH/Mhost increases of a factor ~7 from z=0 to z=3 log G = (0.28 ± 0.06) z + - (2.91 ± 0.08) Decarli et al (2009 a,b)
Unresolved hosts / disk contaminations Decarli et al (2010 a,b)
Unresolved hosts / disk contaminations Decarli et al (2010 a,b)
Different SFHs Decarli et al (2009 a,b)
Different SFHs G ≡ MBH/Mhost increases of a factor ~7 from z=0 to z=3 log G = (0.28 ± 0.06) z + - (2.91 ± 0.08) Decarli et al (2009 a,b)
The MBH–Mhost ratio as a function of z G ≡ MBH/Mhost increases of a factor ~7 from z=0 to z=3 log G = (0.28 ± 0.06) z + - (2.91 ± 0.08) Peng et al. (2006) McLure et al. (2006) Merloni et al. (2010) Decarli et al. (2010) Decarli et al (2010 a,b)
Conclusions • We probed the MBH-Mhost relation up to z=3, both for RLQs and RQQs • The MBH-Lhost is practically constant • Once we correct for the evolution of the M/L ratio, G increases of a factor ~7 from z=0 toz=3, similarly for RLQs and RQQs
What is the fate of z=3 galaxies withMBH/Mhost~0.01? What does it mean? The MBH-Mhost ratio at z=3 is 7 timeslarger than at z=0 They move onto the local MBH-Mhost Mhost increases with Cosmic Timethrough merger events Mhost increasesby gas consumption Evolution of the host galaxyfundamental plane Theydo not move onto thelocal MBH-Mhost Why don’t we see such highG in the local galaxies?
Only 1-2 major mergersare expected(e.g., Volonteri et al., 2003) Stellar populations are old.If strong SF occurs, the Gevolution is even stronger MBH-s* studies also finda similar trend in G The high-mass end of the MBH-host relations is poorlyconstrained, but… What does it mean? They move onto the local MBH-Mhost Mhost increases with Cosmic Timethrough merger events Mhost increasesby gas consumption Evolution of the host galaxyfundamental plane Theydo not move onto thelocal MBH-Mhost Why don’t we see such highG in the local galaxies?
Luminosity Function bias • The scatter in the MBH-Mhost (Lhost, s*, etc) relation introduces a bias (Lauer et al., 2007). • The steeper is the luminosity function, the larger is the bias. • log MBH = ((M2)-(M1)) / ∫M1M2(M)dM