Computer Science
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205...50d&link_type=abstract
Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at
Computer Science
Scientific paper
A discrete thin rotating emission-line disk is ideal for determining the mass of a supermassive black hole in the nucleus of a galaxy. One can use high resolution imaging in combination with a matrix of spatially resolved velocity measurements to confirm the simple geometry and kinematics of the disk. If the disk remains bright and orderly beyond the sphere of influence of the black hole, with motion driven predominantly by gravitational force, one can also measure the density of the surrounding matter in the nucleus. Accordingly, I have used the Hubble Space Telescope to make one of the most direct and complete high-resolution measurements of a supermassive black hole and the density of its surrounding nuclear matter ever made. I first imaged the nucleus of the radio-bright Liner galaxy NGC 3998 in Hα+[NII] emission and in two adjacent continuum bands with the WFPC2 PC, finding a sub-arcsecond oval emission-line region. I then observed this apparent disk with STIS at Hα+[NII] and [SII], placing the 0.1 arcsec slit along the major axis and in 4 parallel positions to map the emission-line kinematics. Velocities could be measured at nearly 20 points along the major axis, at spacings of 6 pc. The major axis rotation curve shows a 108 solar mass black hole in its inner part, then rolls over at 25 parsecs to show a density of about 2000 solar masses per cubic parsec in its outer part. The minor axis velocities are approximately systemic, as expected for a simple rotating disk.
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