  We present the results from an analysis of deep Herschel far-infrared
observations of the edge-on disk galaxy NGC 3079. The PSF-cleaned PACS images
at 100 and 160 um display a 25 kpc x 25 kpc X-shape structure centered on the
nucleus that is similar in extent and orientation to that seen in Halpha,
X-rays, and the far-ultraviolet. One of the dusty filaments making up this
structure is detected in the SPIRE 250 um map out to ~25 kpc from the nucleus.
The match between the far-infrared filaments and those detected at other
wavelengths suggests that the dusty material has been lifted out of the disk by
the same large-scale galactic wind that has produced the other structures in
this object. A closer look at the central 10 kpc x 10 kpc region provides
additional support for this scenario. The dust temperatures traced by the
100-to-160 um flux ratios in this region are enhanced within a biconical region
centered on the active galactic nucleus, aligned along the minor axis of the
galaxy, and coincident with the well-known double-lobed cm-wave radio structure
and Halpha-X-ray nuclear superbubbles. PACS imaging spectroscopy of the inner
6-kpc region reveals broad [C II] 158 um emission line profiles and OH 79 um
absorption features along the minor axis of the galaxy with widths well in
excess of those expected from beam smearing of the disk rotational motion. This
provides compelling evidence that the cool material traced by the [C II] and OH
features directly interacts with the nuclear ionized and relativistic outflows
traced by the Halpha, X-ray, and radio emission.
