Measuring the M-σ Relation with Quasars from 0.2 < z < 1

Details Measuring the M-σ Relation with Quasars from 0.2 < z < 1 Measuring the M-σ Relation with Quasars from 0.2 < z < 1

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21930701h&link_type=abstract

American Astronomical Society, AAS Meeting #219, #307.01

Astronomy and Astrophysics

Astronomy

Scientific paper

It is now known that the masses of black holes, M, at the centers of galaxies correlate with host galaxy properties, including the stellar velocity dispersion, σ, of the central bulge region. The relation implies supermassive black holes and their hosts have a shared evolution, but it is only well studied in the local universe. The precise mechanism of black hole and host galaxy growth regulation is still unknown, but various models predict evolution in the relation with redshift.
We are studying the nature of the M-σ relation using two samples of quasars. 1) Our first sample consists of 29 post-starburst quasars that range in redshift from 0.2We conduct spectral fitting that measures the host galaxy stellar velocity dispersion by broadening a host galaxy template with a Gaussian. We test various templates to minimize template - host galaxy mismatch. We measure the black hole masses using the virial method, which employs the broad line width and continuum luminosity as observables. We are also comparing the velocity dispersions as measured from different spectral regions in a sample of quiescent E+A galaxies.
Our preliminary results show that black holes in both post-starburst and red quasars are over-massive with respect to their hosts when compared to the M-σ relation for local AGN. Our results are generally consistent with previous work that shows an offset for high-z low-luminosity active galaxies.

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