Near-Infrared [Fe ii] and PA beta Imaging and Spectroscopy of ARP 220

We have imaged the ultraluminous infrared galaxy Arp 220 in light of the near-infrared [Fe II] 1.257 micron and Paβ lines, and have obtained spectra in the J- and H-band atmospheric windows. Arp 220 is a strong source of [Fe II] and Paβemission, with luminosities of 1.3 x 10^41^ and 9.2 x 10^40^ ergs s^-1^, respectively. The [Fe II] and Paβ emission are both extended over the central 2"-3", but with different morphologies. The Paβ line is strongly peaked at the position of the western nucleus seen at 2.2 microns (Graham et al. 1990) with a fainter spur in the direction of the eastern nucleus. The [Fe II] emission line shows a weak peak at the western nucleus along with diffuse emission extending to the east, but with no indication of a secondary maximum. The [Fe II] is more extended in the north-south direction than the Paβ line. Nearly 75% of the detected [Fe II] emission is spatially resolved. The overall [Fe II]-to-Paβ line flux ratio in Arp 220 is consistent with that seen over similar spatial scales in Seyfert 2 galaxies, yet larger than what is measured in galaxies with nuclear starbursts. The [Fe II]-to-Paβ line flux ratio is spatially variable being approximately 0.8 at the position of the western nucleus and approximately 2.0 at radii of up to 500 pc. We suggest that the extended [Fe II] emission is produced through the interaction of fast shocks with ambient gas in the ISM at the base of the outflowing, supernovae-driven superwind mapped by Heckman et al. (1987). The bolometric luminosity of the starburst required to power this wind is estimated to be at least 2 x 10^11^ L_sun_. If the spatially unresolved [Fe II] emission is produced via a large number of supernova remnants, the implied rate is ~0.6 yr^-1^. The overall luminosity of such a starburst could account for a large fraction (1/2-1/3) of the Arp 220 energy budget, but the large deficit of ionizing photons (as counted by the Paβ luminosity) requires that the starburst be rapidly declining and/or have a low upper mass cutoff. Alternatively, dust may effectively compete with the gas for ionizing photons, or much of the ionizing radiation may escape through "holes" in the ISM. It is also possible that a buried AGN produces a large fraction of the unresolved [Fe II] and Paβ emission. We briefly discuss these possibilities in light of these new imaging and spectroscopic data.