-
The relation between bulge and SMBH and its evolution
-
M-L and M-sigma relationIn local quiescent galaxies(Kormendy
1993a, Kormendy & Richstone 1995 Gebhardt et al., 2000)
-
AGN (McLure and Dunlop, 2002; Nelson et al., 2004).M-L (0304274)
0.2% (McLure and Dunlop, 2002)M-n (astro-ph/0607378)
-
Our aimsM-sigma and M-L M-sigma and M-L M-sigma and M-L
-
Quiescent HST
AGN2-d image modelling (GALFIT) Integrating field and AOI 3D
On-axis spectrum with MCS deconvolution method 2D The AGN-galaxy
spectral decomposition algorithm 1D
Advantages and disadvantages
-
HST , :a)b) Leonard & Merritt 1989
0.1pc + Plummer
John Kormendy & Karl Gebhardt 2004Genzel 2000
-
Why BH? Spitzer& Hart 1971Plummer potential Zapoosky
Salpeter 1969Eyal Maoz 1998
-
2-D modelling
M-L
-
F. Eisenhauer et al 2000
-
K. JAHNKE et al 2003PSF
-
On-axis spectrum with MCS deconvolution methodPSFAGN
Courbin et al 1998P.Magain et al 1997
-
1060---&--- AGN
XBDong et al 2004
-
::2D-modelling:AOIOn-axis spectrum: AOI
-
Mbh- : :
-
Silk & Rees (1998)
vs>
-
King, A. R. et al. (2003, 2005, 2006) ve>vm tC =tflow
Rcve>>vmRc vm=
-
Adams, et al. (2003) aeff
p
-
Begelman, & Nath (2005) 100 ()M4
-
Burkert & Silk (2001) rcr=GMbh/sph2 rcrtsf
-
Haehnelt & Kauffmann (2000) Mbhsph2
-
Ostriker (2000) self-interacting Mbh4-4.5
-
Miralda-Escude & Kollmeier (2005) Mbh30/7
-
BH mass distribution Vestergaard 2004, ApJ, 601, 676) Low
redshift(3.5): 150 quasars
-
M-LM-SIGMA 311.7-4.510-12Grys ago.1.0-1.7,8-10Gyrs
ago20MbhKormendy&Geb-hardt(2001)LRBettonietal.(2003)(Mbh )R
(MR)log(MBH/M)= .0.50(0.06)MR.2.70(1.35)Peng Chien Y, Impey Chris D
, Ho Luis C, et al. The A strophysical Journal, 2006, 640(1): 114
125.
-
:M-LM-SIGMA
- 1.7
-
:M-LM-SIGMA M-L
-
& P. L.Biermann AAS VOL.41 NO.4
-
,(nearby,normal early-type galaxies,excluding lenticular
galaxies),(Mbh) ,.
-
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