Previous | Session 110 | Next
L. D. Bradley, H. C. Ford, A. R. Martel (JHU), H. D. Tran (Keck Obs.), Z. I. Tsvetanov (JHU/NASA HQ), W. B. Sparks, M. Livio (STScI), D. J. Axon (RIT)
The morphology and kinematics of the disk at the center of M87 are complex. HST/WFPC2 narrow-band images show the presence of a system of filaments extending to the north and northwest that appear to connect directly to the disk. These filaments may originate in a bi-directional wind emanating from the disk. To examine the detailed kinematics of the disk and extended filaments, we have obtained high spatial resolution HST/STIS spectra at several slit positions. Relative to M87's systemic velocity, we observe large redshifted and blueshifted velocities on opposite sides of the disk with a peak-to-peak difference of nearly 1200 km/s. We model this velocity field as gas in simple Keplerian rotation about a massive black hole. We also find large non-circular velocity components superimposed on the underlying rotation of the disk, some of which are spatially coincident with the ionized filaments. We also detect dust associated with many of the filaments, indicating that they are in the foreground and thus tipped toward the line of sight. The morphological and kinematic observations suggest that some of this filamentary gas is outflowing from the disk. This research is supported by STScI grant HST-GO-08666.01-A.
Previous | Session 110 | Next
Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.