We present observations of the SS 433 jets using the Chandra High Energy Transmission Grating Spectrometer with contemporaneous optical and Very Long Baseline Array 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 3 × 1014?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 2 × 1012?cm. The base jet density is in the range 1010-13?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 15 relative to the solar value, which may have resulted from an unusual supernova that formed the compact object.
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