Outflows from the Disk Fueling the Massive Black Hole in M87

Details Outflows from the Disk Fueling the Massive Black Hole in M87 Outflows from the Disk Fueling the Massive Black Hole in M87

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8666f&link_type=abstract

HST Proposal ID #8666

Physics

Hst Proposal Id #8666 Agn/Quasars

Scientific paper

The disk in M87 is a prototype for gas orbiting a massive central object. Although the disk is rotating, its morphology and kinematics are far from simple. A deep Halpha+N II HST image shows a trailing, three arm spiral superposed on the underlying disk, and an extended system of filaments. The NW filaments appear to connect directly to the disk. Ground- based and HST observations suggest that some of the filaments originate in a bi-directional wind emanating from the disk. Such a wind can carry away angular momentum, enabling gas to flow through the resolved disk into the accretion disk around the black hole. We propose high spatial resolution STIS spectroscopy aimed at achieving the following scientific goals: 1} Determine if winds are carrying angular momentum away from the disk, thereby enabling inflow and fueling of the massive black hole, 2} Estimation of the rate of mass loss and angular momentum loss from the disk, and 3} Use changes in the velocities and line strengths at the positions of the spiral- like features in the disk to determine if these are shocks where gas is flowing through a density wave. Because small, 100-parsec scale gaseous disks like the one in M87 are common in the centers of active galaxies, demonstration that a wind is removing angular momentum from the M87 disk will have far reaching consequences.

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