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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. - PowerPoint PPT Presentation
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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, ItalyR. Falomo INAF, Osservatorio Astronomico di Padova, ItalyM. Uslenghi INAF-IASF, Milano, Italy
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The virial method
Elliptical galaxies
SMBHs
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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The virial method (AGN)
RBLR: reverberation mapping
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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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
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MBH and global propertiesof 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
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MBH for close-by quasars
Virial method Host galaxy luminosity method
Sample: HST WFPC2 imagesHST FOS spectra
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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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
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The spectra
Continuum subtractedrest-frame spectra
C IV emission lines:FWHM determination
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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BH mass comparisonf=1.3f=√3/2
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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Main results
MBH – Lbulge correlation obtained locallycan be extrapolated to z ~ 0.4
f ~ 1.3 i.e. disc-like BLR geometrywith inclination angles 12° < i < 48°
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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FWHM distribution_____observed FWHM
cumulative distribution
- - - - -expected cumulativedistribution in a disc-likeBLR geometrypicture
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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QSOs inclination angles
Kolmogorov –Smirnov test ofcompatibility:
12° < i < 48°
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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QSOs at high z
FromFalomo et al. 2004
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
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ESO 3.6m + EFOSC2
THE BH MASS OF NEARBY QSOs – M. Labita, A. Treves, R. Falomo, M. Uslenghi
QSOs at high z:spectra
