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Using new ultraviolet (UV) spectra of five background quasars from the CosmicOrigins Spectrograph on the Hubble Space Telescope, we analyze the low-latitude(|b|=20-30 degree) regions of the Fermi Bubbles, the giant gamma-ray emittinglobes at the Galactic Center. We combine these data with previous UV and atomichydrogen (HI) datasets to build a comprehensive picture of the kinematics andmetal column densities of the cool outflowing clouds entrained in the FermiBubbles. We find that the number of UV absorption components per sightlinedecreases as a function of increasing latitude, suggesting that the outflowingclouds become less common with increasing latitude. The Fermi Bubble HI cloudsare accelerated up to b~7 degree, whereas when we model the UV Fermi Bubblesclouds deprojected flow velocities, we find that they are flat or evenaccelerating with distance from the Galactic center. This trend, which holds inboth the northern and southern hemispheres, indicates that the nuclear outflowaccelerates clouds throughout the Fermi Bubbles or has an acceleration phasefollowed by a coasting phase. Finally, we note the existence of severalblueshifted high-velocity clouds at latitudes exceeding ~30 degree, whosevelocities cannot be explained by gas clouds confined to the inside of thegamma-ray defined Fermi Bubbles. These anomalous velocity clouds are likely infront of the Fermi Bubbles and could be remnants from past nuclear outflows.Overall, these observations form a valuable set of empirical data on theproperties of cool gas in nuclear winds from star-forming galaxies.

Mapping Outflowing Gas in the Fermi Bubbles: a UV Absorption Survey of the Galactic Nuclear Wind