our images (Figure \[ir19254\_im\]), and there is no evidence for emission extending toward the direction of the tails. Even the northern nucleus is marginally above the sensitivity limit $\sim$1mJy at 3$\sigma$ (see Table \[phot\]).

Using optical spectroscopy, the southern galaxy has been classified as a Seyfert 2 with an observed FWHM of $\sim$1700kms$^{-1}$ in both permitted and forbidden lines [@Mirabel1990; @Duc1997a]. The presence of an active nucleus is further suggested by the IRAS criteria for selecting Seyferts, since the ratio of its 25$\mu$m to the 60$\mu$m IRAS flux density is greater than 0.2 [see @deGrijp1985], while its optical and near-infrared colors indicate a strong contribution from a non-thermal component, likely originating from an AGN, as well as emission from very hot dust ($\sim$1000K) [@Vanzi2002]. Evidence of massive star formation is also seen in the nuclear regions as emission line splitting which has been attributed to a biconical outflow [@Colina1991]. The kinetic energy necessary for this to occur can only be produced by supernova explosions or stellar winds further suggesting high star formation rates [150M$_{\sun}$yr$^{-1}$, @Colina1991]. Ground-based MIR observations at 10$\mu$m show that more than 80$\%$ of the total flux originates from the Seyfert 2 (the southern galaxy). The spectrum of 