SPATIALLY EXTENDED NAID RESONANT EMISSION AND ABSORPTION IN THE GALACTIC WIND OF THE NEARBY INFRARED-LUMINOUS QUASAR F05189-2524

Emission from metal resonant lines has recently emerged as a potentially powerful probe of the structure of galactic winds at low and high redshift. In this work, we present only the second example of spatially resolved observations of Na (I) D emission from a galactic wind in a nearby galaxy (and the first 3D observations at any redshift). F05189-2524, a nearby (z = 0.0428) ultraluminous infrared galaxy powered by a quasar, was observed with the integral field unit on the Gemini Multi-Object Spectrograph at Gemini South. Na (I) D absorption in the system traces dusty filaments on the near side of an extended, active galactic nucleus-driven galactic wind (with projected velocities up to 2000 km s(-1)). These filaments (A(v) less than or similar to 4 and N (H) less than or similar to 1022 cm(-2)) simultaneously obscure the stellar continuum and Na (I) D emission lines. The Na (I) D emission lines serve as a complementary probe of the wind: they are strongest in regions of low foreground obscuration and extend up to the limits of the field of view (galactocentric radii of 3 kpc). An azimuthally symmetric Sersic model extincted by the same foreground screen as the stellar continuum reproduces the Na (I) D emission line surface brightness distribution except in the inner regions of the wind, where some emission-line filling of absorption lines may occur. The presence of detectable Na (I) D emission in F05189-2524 may be due to its high continuum surface brightness at the rest wavelength of Na (I) D. These data uniquely constrain current models of cool gas in galactic winds and serve as a benchmark for future observations and models.