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While 2% of active galactic nuclei (AGNs) exhibit narrow emission lines withline-of-sight velocities that are significantly offset from the velocity of thehost galaxy's stars, the nature of these velocity offsets is unknown. Weinvestigate this question with Chandra/ACIS and Hubble Space Telescope/WideField Camera 3 observations of seven velocity-offset AGNs at z<0.12, and allseven galaxies have a central AGN but a peak in emission that is spatiallyoffset by < kpc from the host galaxy's stellar centroid. These spatial offsetsare responsible for the observed velocity offsets and are due to shocks, eitherfrom AGN outflows (in four galaxies) or gas inflowing along a bar (in threegalaxies). We compare our results to a velocity-offset AGN whose velocityoffset originates from a spatially offset AGN in a galaxy merger. The opticalline flux ratios of the offset AGN are consistent with pure photoionization,while the optical line flux ratios of our sample are consistent withcontributions from photoionization and shocks. We conclude that these opticalline flux ratios could be efficient for separating velocity-offset AGNs intosubgroups of offset AGNs -- which are important for studies of AGN fueling ingalaxy mergers -- and central AGNs with shocks -- where the outflows are biasedtowards the most energetic outflows that are the strongest drivers of feedback.

Shocks and Spatially Offset Active Galactic Nuclei Produce Velocity Offsets in Emission Lines