Jet‐ and Wind‐driven Ionized Outflows in the Superbubble and Star‐forming Disk of NGC 3079

HST WFPC2 images are presented that span the inner 19 kpc diameter of theedge-on spiral galaxy NGC 3079; they are combined with ground-based Halpha+[NII] Fabry-Perot spectra and VLA images of radio polarization vectors androtation measures. Ionized gas filaments within 9 kpc diameter project ~3 kpcabove the disk, with the brightest forming the 1 kpc diameter superbubble. Theyare often resolved into strands ~0."3 (25 pc) wide which emerge from thenuclear CO ring as five distinct gas streams with velocity gradients anddispersions of hundreds of km/s. One stream flows for 250 pc and aligns withthe VLBI-scale radio jet, the other four are not connected to the jet, insteadcurving to the vertical 0.6 kpc above the galaxy disk, then dispersing in aspray of droplets each with ionized mass ~1000 sqrt(f) Msun (volume fillingfactor f > 0.003 from our data). Shredded clumps of disk gas form a similarstructure in hydro models of a galaxy-scale wind. The pattern of magneticfields and the gas kinematics also suggest a wind of mechanical luminosity10^43 erg/s that has stagnated in the galaxy disk at radius ~800 pc, flared tolarger radii with increasing height as the balancing ISM pressure reduces abovethe disk, and entrained dense clouds into a vortex. Total KE and momentum ofthe filaments are (0.4-5)x10^55 sqrt(f) ergs and (1.6-6)x10^47 sqrt(f) dyne s.A star-forming complex elsewhere in the galaxy shows a striking spray of linearfilaments that extend for hundreds of parsecs.