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The BH mass of nearby QSOs

The BH mass of nearby QSOs. A comparison of the bulge luminosity and virial methods. M. Labita, A. Treves Università dell’Insubria, Como, Italy R. Falomo INAF, Osservatorio Astronomico di Padova, Italy M. Uslenghi INAF-IASF, Milano, Italy.

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The BH mass of nearby QSOs

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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