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Over the past half century, gas outflows and winds have been observed asasymmetric emission lines in a wide range of astrophysical contexts, includinggalaxies and early-type stars. While P Cygni lines are modeled and understoodwith physically-motivated profiles under the Sobolev approximation, asymmetricnebular lines are not. Previous studies of galactic outflows using nebularemission lines have made physically unjustified assumptions about the shape ofthe line profile. These approaches limit assessment of outflow properties anddo not connect observations to the underlying physics. The physical complexityof galactic outflows requires a more robust approach. In response to this need,we present a novel profile for modeling nebular emission lines which isgeneralized yet physically motivated and provides insight into the underlyingmechanisms of galactic outflows. To demonstrate the usefulness of this profile,we fit it to the asymmetric nebular lines observed in the nuclear region of Mrk462, a starburst-AGN composite galaxy. From analysis of the best-fit profile,we conclude that the observed profile arises from a dustyradiation-pressure-driven outflow with a terminal velocity of 750 km s-1. Thisoutflow, while weak by some standards, is still sufficiently strong to regulatestar formation and black hole growth in the host galaxy by removing gas fromthe inner few kiloparsecs. Outflows like the one we observe and characterize inMrk 462 are crucial to our understanding of episodic gas-fueled activity ingalactic nuclei, which undoubtedly plays a pivotal role in galaxy evolution.

Galactic Outflow Emission Line Profiles: Evidence for Dusty, Radiatively-Driven Ionized Winds in Mrk 462