lines with wings of $\sim$ 1500kms$^{-1}$ larger in the blue and extending $\sim$5kpc out from the nucleus. These emission lines, as well as other Wolf-Rayet features observed, could be caused by supernova winds and turbulent motions associated with the merger [@Johansson1988]. The northern galaxy on the other hand, has narrower emission lines and weaker starburst activity.

In Figure \[ir23128\_spec\], we present the CVF spectra of each galaxy along with our flux measurements using the four broad-band filters. The integrated MIR SED of the whole system is displayed in Figure \[ir23128\_phot\], as well as the ISOPHOT-S spectrum which is in good agreement with our data. As in the case of IRAS19254-7245, no MIR emission is seen to be associated with the tidal tails down to our sensitivity limits (see Figure \[ir23128\_im\]).

We find that approximately 75$\%$ of the MIR flux in IRAS23128-5919 originates from the southern galaxy. The spectrum reveals that the thermal continuum (12–16$\mu$m) is higher in the southern galaxy than that of the north, making the southern galaxy the dominant origin of the MIR emission. Since the SED of both components displays a rising spectrum with prominent UIBs and a weak continuum at 5–6$\mu$m, we conclude that the MIR 