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The BH mass of nearby QSOs A comparison of the bulge luminosity and virial methods M. Labita, A. TrevesUniversità dell’Insubria, Como, Italy R. FalomoINAF,

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Presentation on theme: "The BH mass of nearby QSOs A comparison of the bulge luminosity and virial methods M. Labita, A. TrevesUniversità dell’Insubria, Como, Italy R. FalomoINAF,"— Presentation transcript:

1 The BH mass of nearby QSOs A comparison of the bulge luminosity and virial methods M. Labita, A. TrevesUniversità dell’Insubria, Como, Italy R. FalomoINAF, Osservatorio Astronomico di Padova, Italy M. UslenghiINAF-IASF, Milano, Italy

2 2 The virial method Elliptical galaxies SMBHs THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

3 3 The virial method (AGN) R BLR : reverberation mapping THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

4 4 The virial method (3) BRL radius Nuclear luminosity Pian E., Falomo R., Treves A. 2005, MNRAS, 361, 919 THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

5 5 M BH and global properties of the host galaxy Locally:  Velocity dispersion  ;  Galaxy Luminosity: Coevolution of host galaxies and SMBHs THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

6 6 M BH for close-by quasars  Virial method  Host galaxy luminosity method Sample:HST WFPC2 images HST FOS spectra THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

7 7 The sample 30 QSOs  18 RLQs  12 RQQs 0.1< z <0.6 THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

8 8 The spectra Continuum subtracted rest-frame spectra C IV emission lines: FWHM determination THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

9 9 BH mass comparison f=1.3f=√3/2 THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

10 10 Main results  M BH – L bulge correlation obtained locally can be extrapolated to z ~ 0.4  f ~ 1.3 i.e. disc-like BLR geometry with inclination angles 12° < i < 48° THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

11 11 FWHM distribution _____ observed FWHM cumulative distribution - - - - - expected cumulative distribution in a disc-like BLR geometry picture THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

12 12 QSOs inclination angles Kolmogorov – Smirnov test of compatibility: 12° < i < 48° THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

13 13 QSOs at high z From Falomo et al. 2004 THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi

14 14 ESO 3.6m + EFOSC2 THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi QSOs at high z: spectra

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