Abstract

We present the first HST long-slit spectrum of a gaseous disk around a candidate super-massive black-hole. The results of this study on the kinematics of the gaseous disk in M87 are a considerable improvement in both spatial resolution and accuracy over previous observations and requires a projected mass of MBH(sin i)2 = (2.0 ± 0.5)×109M⊙ (MBH = 3.2×109M⊙ for a disk inclination i = 52◦) concentrated within a sphere whose radius is less than 0.′′05 (3.5 pc) to explain the observed rotation curve. The kinematics of the ionized gas is well described by a thin disk in keplerian motion. A lower limit to the mass-to-light ratio of this region is M/LV ≃110, significantly strengthening the claim that this mass is due to the presence of a central black-hole in M87. (Refer to PDF file for exact formulas).

Publication Date

1997

Comments

Also archived in: arXiv:astro-ph/9706246 v1 24 Jun 1997 Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555 and by STScI grant GO-3594.01-91A.ISSN:1365-2966 Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type

Article

Department, Program, or Center

School of Physics and Astronomy (COS)

Campus

RIT – Main Campus

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