Jose A. Acosta Pulido 1,2,3, U. Klaas 2, & R. Laureijs 1
1 ISO Science Operations Centre, Astrophysics Division of ESA, Villafranca, P.O. Box 50727, 28080 Madrid, SPAIN
2 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, GERMANY
3 Instituto de Astrofisica de Canarias E-38200 La Laguna, S/C Tenerife, SPAIN
NGC 6090 is a tightly interacting galaxy pair, likely in the process of merging. The two nuclei are separated by 6.4", which corresponds to a projected distance of 3.6 kpc. As the system is undergoing a very strong collision, different excitation conditions are expected in the various parts of the galaxies. Therefore the individual emission components may well have different sites of origin. We study the spatial distribution of the MIR emission in this compact system, based on multi-filter ISOCAM observations (from 4.5um to 15um). This includes maps of the continuum emission as well as maps in the main PAH features (6.2um, 7.7um and 11.3um) and the two forbidden lines [NeII]12.8um and [NeIII]15.5um. The data reduction was done using standard procedures in CIA, but a new transient correction was applied with a concise description of it given here. Our observations were perfomed in raster mode and the shift was a fraction of a pixel in order to improve the sampling of the PSF. The two galaxy nuclei are resolved in all filters. As their separation is close to the resolution limit of ISOCAM, deconvolution techniques are applied to restore the maximum
resolution. We also present cross calibration with already published ISOPHOT
data.