ON THE SUPERSONIC TURBULENCE OF NGC-604

Two-dimensional high spatial resolution Fabry-Perot observations with TAURUS 2 at the William Herschel Telescope in La Palma, over the inner central regions of NGC 604 in M33, have been obtained. The data show a large variety of line profile shapes produced over the region. Some display clear splitting, or strong asymmetries, most likely caused by the action of strong winds and champagne flows produced by the many massive stars presently disrupting large sections of the parent cloud. On the other hand, emission lines arising from the multicore or highest intensity regions of NGC 604 show well-defined Gaussian profiles with a typical FWHM of 38.8 km s(-1) in H alpha, implying an intrinsic supersonic velocity dispersion of 16.5 km s(-1). This agrees, within the observational errors, with the global integrated line profile of NGC 604. Here we show that the contribution to the overall line profile from other zones of NGC 604 are negligible. They present a much lower intensity and thus, even if some are fitted with broader Gaussians, they do not contribute appreciably when compared to the higher intensity lines arising from the multicore region.