  We present observations of the SS 433 jets using the Chandra High Energy
Transmission Grating Spectrometer with contemporaneous optical and VLBA
observations. The X-ray and optical emission line regions are found to be
related but not coincident as the optical line emission persists for days while
the X-ray emission lines fade in less than 5000 s. The line Doppler shifts from
the optical and X-ray lines match well, indicating that they are less than 3e14
cm apart. The jet Doppler shifts show aperiodic variations that could result
from shocks in interactions with the local environment. These perturbations are
consistent with a change in jet direction but not jet speed. The proper motions
of the radio knots match the kinematic model only if the distance to SS 433 is
4.5 +/- 0.2 kpc. Observations during eclipse show that the occulted emission is
very hard, seen only above 2 keV and rising to comprise >50% of the flux at 8
keV. The soft X-ray emission lines from the jet are not blocked, constraining
the jet length to >~ 2e12 cm. The base jet density is in the range
1e(10-13)/cm^3, in contrast to our previous estimate based on the Si XIII
triplet, which is likely to have been affected by UV de-excitation. There is a
clear overabundance of Ni by a factor of about 10 relative to the solar value,
which may have resulted from an unusual supernova that formed the compact
object.

High Energy Astrophysical Phenomena