Hot halo gas in the Virgo cluster galaxy NGC 4569

We have observed the Virgo cluster spiral NGC 4569 in X-rays with ROSAT (0. 1-2.4 keV) and in the optical. From the PSPC image one can distinguish diff erent components, like the dominant source in the nuclear region, the galac tic disk, and a diffuse soft component extended to the west. This latter on e coincides with a giant H alpha structure. In both spectral ranges the str ucture reaches up to 9 kpc out of the disk. This coincidence, the soft X-ra y energy distribution, and the existence of a central starburst in NGC 4569 let us conclude that the X-ray gas traces a large scale out ow from accumu lating supernova explosions and stellar winds in the galactic center. The r esulting physical properties of this X-ray halo are comparable to those der ived from X-ray halos in edge-on galaxies, like e.g. NGC 253. We also discu ss the influence of the intracluster medium on the observed X-ray and H alp ha morphology. The spectral 0.1-2.4 keV distribution of the central source and the X-ray-to-H alpha luminosity ratio favour a supermassive star cluste r at the very compact core rather than an accretion-powered active nucleus in agreement with the absence of a hard compact X-ray source in the ASCA ba nd. The nearby Magellanic dwarf galaxy IC 3583 at a projected distance of o nly 30 kpc reveals an unresolved X-ray point source, several blue knots in the optical, and a narrow H alpha spur, pointing toward NGC 4569, detected also in the B band image. This is an indication for ongoing star formation also in IC 3583. Some interaction with NGC 4569 will be discussed although the relative radial velocity between both objects of about 1300 km s(-1) ma kes it rather unlikely.