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We present the results of recent Chandra, XMM-Newton, and Hubble SpaceTelescope observations of the radio-loud (RL), broad absorption line (BAL)quasar PG 1004+130. We compare our new observations to archival X-ray and UVdata, creating the most comprehensive, high signal-to-noise, multi-epoch,spectral monitoring campaign of a RL BAL quasar to date. We probe forvariability of the X-ray absorption, the UV BAL, and the X-ray jet, onmonth-year timescales. The X-ray absorber has a low column density of$N_{H}=8\times10^{20}-4\times10^{21}$ cm$^{-2}$ when it is assumed to be fullycovering the X-ray emitting region, and its properties do not varysignificantly between the 4 observations. This suggests the observed absorptionis not related to the typical "shielding gas" commonly invoked in BAL quasarmodels, but is likely due to material further from the central black hole. Incontrast, the CIV BAL shows strong variability. The equivalent width (EW) in2014 is EW=11.24$\pm$0.56 \AA, showing a fractional increase of $\Delta EW /\langle EW \rangle$=1.16$\pm$0.11 from the 2003 observation, 3183 days earlierin the rest-frame. This places PG 1004+130 among the most highly variable BALquasars. By combining Chandra observations we create an exposure 2.5 timesdeeper than studied previously, with which to investigate the nature of theX-ray jet and extended diffuse X-ray emission. An X-ray knot, likely with asynchrotron origin, is detected in the radio jet ~8 arcsec (30 kpc) from thecentral X-ray source with a spatial extent of ~4 arcsec (15 kpc). No similarX-ray counterpart to the counterjet is detected. Asymmetric, non-thermaldiffuse X-ray emission, likely due to inverse Compton scattering of CosmicMicrowave Background photons, is also detected.

Ultraviolet/X-ray variability and the extended X-ray emission of the radio-loud broad absorption line quasar PG 1004+130