The spectral variability of UV-optical continuum emission of Active Galactic Nuclei

Details The spectral variability of UV-optical continuum emission of Active Galactic Nuclei The spectral variability of UV-optical continuum emission of Active Galactic Nuclei

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010fym..confp..40m&link_type=abstract

"The First Year of MAXI: Monitoring Variable X-ray Sources", Poster Presentations, 4th International MAXI Workshop held November

Computer Science

Scientific paper

We examine whether the spectral shape of UV-optical continuum emission of AGNs changes during flux variation. The long-term optical monitoring observations of 11 nearby Seyfert galaxies and QSOs were carried out by the MAGNUM telescope. The multi-epoch flux data in any two different bands obtained on the same night showed a tight linear flux-to-flux relationship, and the non-variable component of the host galaxy plus narrow emission lines was located on the fainter extension of the best-fit linear regression. The UV spectral variation was examined based on the multi-epoch photometric data of 10 bright QSOs at z=1.0-2.4 observed by the SDSS Legacy Survey. The rest-frame UV flux data in two different bands showed a linear relationship, but in contrast to the optical, the host-galaxy color was systematically redder than the slope of the linear relationship. These results indicate that the spectral shape of continuum emission retains almost constant during flux variation in optical, but it becomes bluer as brighter in UV. Those spectral variability of UV-optical continuum emission can be interpreted by the standard accretion disk model changing the mass accretion rate with a constant black-hole mass, which strongly supports the standard accretion disk model for UV-optical continuum emission of AGNs.

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