D. E. Harris (SAO), C. C. Cheung (GSFC), L. Stawarz (KIPAC), and J. A. Biretta (STScI)
We have been monitoring the M87 jet with sub-arcsec resolution since 2002 in radio, optical, and X-rays. From an analysis of the first derivative of the X-ray lightcurve we find evidence for an unexpected oscillation in the brightening and fading of HST-1. This knot which lies 0.86" (60pc projected) from the nucleus, displayed a giant flare that peaked in 2005, coinciding with the maximum observed TeV intensity from M87. We evaluate various timescales to determine if differences in radio, optical, and X-rays can be attributed to loss mechanisms suffered by the relativistic electrons responsible for the observed emissions. The work at SAO was supported by NASA grants NAS GO6-7112X and GO7-8119X.