Nuclear gasdynamics in Arp 220: Subkiloparsec-scale atomic hydrogen disks

We present new, high angular resolution (similar to0.22) MERLIN observations of neutral hydrogen (H I) absorption and lambda 21 cm radio continuum emission across the central similar to 900 pc of the ultraluminous infrared galaxy Arp 220. Spatially resolved H I absorption is detected against the morphologically complex and extended lambda 21 cm radio continuum emission, consistent with two counterrotating disks of neutral hydrogen, with a small bridge of gas connecting the two. Column densities across the two nuclei are high, lying in the range 8 x 10(19) T-s(K) less than or similar to N-H less than or similar to 2.4 x 10(20) T-s(K) cm(-2) (T-s is spin temperature) and corresponding to optical extinctions of 0.052T(s)(K) less than or similar to A(V) less than or similar to 0.155 T-s(K) mag,with the higher column densities in the eastern nucleus. Velocity gradients are clearly visible across each nucleus, reaching 1010 +/- 20 mk s(-1) kpc(-1) in P.A. similar to 55 degrees and 830 +/- 20 km s(-1) kpc(-1) in P.A. similar to 270 degrees for eastern and western nuclei, respectively. These gradients imply dynamical masses M-D = 1.1 x 10(9)(sin(-2) i) (E) and 1.7 x 10(8)(sin(-2) i) M-. (W), assuming that the neutral gas in distributed in two thin circularly rotating disks. We propose a merger model in which the two nuclei represent the galaxy cores that have survived the initial encounter and are now in the final stages of merging, similar to conclusions drawn from previous CO studies. However, we suggest that instead of being coplanar with the main CO disk (in which the eastern nucleus is embedded), the western nucleus lies above it and, as suggested by the bridge of H I connecting the two nuclei, will soon complete its final merger wit the main disk. We suggest that the collection of radio supernova (RSNe) detected in VLBA studies in the more compact western nucleus represents the second burst of star formation associated wit this final merger stage and that free-free absorption due to ionized gas in the bulgelike component can account for the observed RSN distribution.