Stellar kinematics are hard to derive for Seyfert nuclei

Stellar kinematics are hard to derive for Seyfert nuclei -...

Info iconThis preview shows page 1. Sign up to view the full content.

View Full Document Right Arrow Icon
Stellar kinematics are hard to derive for Seyfert nuclei, much less quasars, because the starlight is swamped by the nonstellar light from the nucleus. It's easier for radio galaxies (like, for example, M87). On the theory that the compact radio source Sagittarius A * is some kind of weak AGN, studies of kinematics near the Milky Way's nuclear become relevant. A real breathrough has been the newly acquired ability to measure proper motions of stars within the central parsec over a few years. Ghez et al. (2000 Nature 407, 349) show arcs for these motions which suggest a central mass of 2.6 × 10 6 solar masses. The great thing about proper-motion studies is that the results only improve with time. Current data show substantial parts of stellar orbits here, making it clear thet they are Keplerian about a mass smaller than about 10 AU in radius, and making this by far the best-attested massive black hole. ( Link to animated GIF of stellar orbits ) Gravitational redshift of X-ray spectral features. Over the years there have been limits or
Background image of page 1
This is the end of the preview. Sign up to access the rest of the document.

This note was uploaded on 11/10/2011 for the course AST AST1002 taught by Professor Emilyhoward during the Fall '10 term at Broward College.

Ask a homework question - tutors are online