Evidence for an Accretion Disk in MRK 335

Details Evidence for an Accretion Disk in MRK 335 Evidence for an Accretion Disk in MRK 335

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.5204z&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #52.04; Bulletin of the American Astronomical Society, Vol. 24, p.1209

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We observe the far-ultraviolet spectrum of the Seyfert galaxy Markarian 335 (z=0.026) using the Hopkins Ultraviolet Telescope on 1990 December 10. A prominent blended emission feature of O vi lambda lambda 1032, 1038 and Lybeta is nearly as strong as the C iv lambda 1549. The broad C iv component is blueshifted by ~ 450\ km\ s(-1) with respect to the narrow line. The continuum flux extends beyond the Lyman limit without noticeable discontinuity, but the flux declines gradually by 40% from the O vi/Lybeta blend to lambda_ {rest} = 890 Angstroms, where the spectrum is cut off by interstellar absorption in the Galaxy. We suggest that this decline in flux may be the signature of an accretion disk seen at a small inclination angle. Using a disk model, we fit the data with a central mass of 3.5 times 10(7\) M_sun, an accretion rate of 0.06\ M_sun/yr, and an optical depth at the Lyman edge of about 0.5. To account for the strong O vi emission as well as the soft X-ray excess, we consider the effects of Comptonization on the disk spectrum, which produces a high-energy tail for the UV bump and smooths the Lyman edge. This work is supported by NASA contract NAS 5-27000.

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