Shocked Gas in IRAS F17207-0014: ISM Collisions and Outflows
  We combine optical and near-infrared AO-assisted integral field observations
of the merging ULIRG IRAS F17207-0014 from the Wide-Field Spectrograph (WiFeS)
and Keck/OSIRIS. The optical emission line ratios [N II]/H$\alpha$, [S
II]/H$\alpha$, and [O I]/H$\alpha$ reveal a mixing sequence of shocks present
throughout the galaxy, with the strongest contributions coming from large radii
(up to 100% at $\sim$5 kpc in some directions), suggesting galactic-scale
winds. The near-infrared observations, which have approximately 30 times higher
spatial resolution, show that two sorts of shocks are present in the vicinity
of the merging nuclei: low-level shocks distributed throughout our
field-of-view evidenced by an H$_{2}$/Br$\gamma$ line ratio of $\sim$0.6-4, and
strong collimated shocks with a high H$_{2}$/Br$\gamma$ line ratio of
$\sim$4-8, extending south from the two nuclear disks approximately 400 pc
($\sim$0.5 arcsec). Our data suggest that the diffuse shocks are caused by the
collision of the interstellar media associated with the two progenitor galaxies
and the strong shocks trace the base of a collimated outflow coming from the
nucleus of one of the two disks.
