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Bulge Luminosity vs. Virial Methods in Determining BH Mass of Nearby QSOs

Study comparing methods for calculating supermassive black hole (BH) mass in nearby Quasars (QSOs). Analyzing the bulge luminosity method and the virial method, utilizing data from HST WFPC2 images and HST FOS spectra. Investigating BH mass correlations with host galaxy properties locally and extrapolated to z~0.4. Results show potential correlation and hints of disc-like BLR geometry. FWHM analysis and QSO inclination angles tested for compatibility using Kolmogorov-Smirnov test. Including data from high-z QSOs and ESO 3.6m + EFOSC2 spectra for broader insights.

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Bulge Luminosity vs. Virial Methods in Determining 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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