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KINEMATICS OF SUPERBUBBLES AND SUPERSHELLS IN THE IRREGULAR GALAXY, NGC 1569

We present observations in the optical lines of Hα and [S ii] (λλ6717, 6731 Å) and in X-rays of the irregular galaxy, NGC 1569. The observations in Hα and [S ii] were made with the UNAM scanning Fabry–Perot interferometer (PUMA) and the X-ray data were obtained from the Chandra data archive. We detected several superbubbles, filaments, and supershells in NGC 1569 for which we determined size as well as their kinematic properties. We present a catalog of expansion velocities of 12 superbubbles, listing their positions, diameters, and physical parameters. Likewise, we present a catalog of 15 filaments and 4 supershells. In order to identify possible X-ray emission from the superbubbles in this galaxy, we analyzed the X-ray emission of NGC 1569 in two energy bands: 0.2–2.0 keV (soft X-rays) and 2.0–8.0 keV (hard X-rays). Based on X-ray images, we detected X-ray emission that could possibly be related to some of the superbubbles. The spectrum of the X-ray superbubbles can be described by an optically thin thermal plasma model. In order to identify the possible coexistence of galactic super winds and superbubbles we have performed adiabatic three-dimensional N-body/smoothed particle hydrodynamics simulations to follow the evolution of the most important stellar clusters in this galaxy, SSC A and SSC B, using the GADGET-2 code. Those simulations demonstrate that depending on the specific initial conditions, the formation of superbubbles or a galactic superwind can result in NGC 1569.