to young stars [@Mirabel1998] or AGN [@Laurent2000]. On the contrary, the northern galaxy has strong UIBs (f$_{6.7\mu m}$/f$_{6\mu m}$$\sim$2.5) and faint thermal emission at 15$\mu$m (f$_{15\mu m}$/f$_{6.7\mu m}$$\sim$1.2), which is typical of MIR emission from normal spiral galaxies with cool IRAS colors [@Dale2001; @Roussel2001]. Comparison of in its broad-band SED with the template SED of a quiescent star forming region within the disk of M82 [@Laurent2000] illustrates that they are in a fairly good agreement (Figure \[ir19254n\_spec\]).

The absolute luminosities presented in Table \[global\] shows that the MIR emission originating from the southern Seyfert 2 galaxy is by far the strongest in our sample although the most luminous FIR source is IRAS14348-1447 (see Table \[info\]). One may also note that the flux density near 5$\mu$m does not reach zero level but is $\sim$100mJy, suggesting the presence of a hot dust component, which as discussed in the previous section is a clear sign of a hot dusty torus of an AGN [@Laurent2000]. Similarly, one can draw the same conclusion by observing the combination of the f$_{15\mu
m}$/f$_{6.7\mu m}$ and f$_{6.7\mu m}$/f$_{6\mu m}$ flux ratios. In IRAS19254-7245S, the low f$_{6.7\mu m}$/f$_{6\mu m}$ indicates weak UIB emission while f$_{15\mu m}$/f$_{6.7\mu m}$$\sim$2.7, a value 