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kinematics around the non-thermal superbubble in ic 10

1 We study the kinematics around a non-thermal superbubble found by Yang & Skill-man. Considering the H II and [S II] profiles, we find that between 3 and 6 supernovae are required to form this superbubble. IC 10 may well be the nearest example of a blue compact dwarf galaxy (BCD). Among the Local Group star-forming dwarf galaxies, IC 10 is conspicuous for having the highest surface density of WR stars (11.2 kpc −2 , Richer et al. 2000). The presence of so many WR stars and the high Hα luminosity emphasize that IC10 is currently undergoing a burst of star formation that began at least 10 Myr ago. Observations of 21-cm emission from neutral hydrogen reveal that IC 10 consists of an inner disk embedded in an extended, complex, counter-rotating envelope (Shostak & Skillman 1989). This leads Wilcots & Miller (1998) to conclude that IC 10 is still in its formative stage. These H I observations make clear the youth of the current star formation episode for there is a notable lack of interestellar medium structures attributable to supernovae (Wilcots & Miller 1998). The galaxy size in the light of Hα is 5 × 3 arcmin while in H I it is 18 × 15 arcmin. All optical studies of IC 10 are hampered by the large foreground reddening due to its position near the plane of our galaxy (l = 119 • , b = −3 •). Our observations of the non-thermal superbub-ble, discovered by Yang & Skillman (1993), were obtained in the light of Hα and [S II] with the scanning Fabry-Perot Interferometer, PUMA. We suppose that the energy in the ionized interstellar medium comes from the energy injected by stellar winds and supernovae. Considering both the Hα and [S II] profiles , we find a typical expansion velocity of 50 to 70 km s −1. Using a distance of 661 kpc (Sakai et al. 1999) and a diameter of 41.5 inferred from Yang & Skillman (1993), we calculate a radius of 66 pc for the superbubble. Adopting a density of 1.1 atoms cm −3 (Yang & Skillman 1993), the mass swept out by the superbubble is 4.87×10 37 g (2.45×10 4 solar masses). Fig. 1. A close-up of the region of the non-thermal su-perbubble in Hα with the Yang & Skillman, (1993) iso-contours of the 49-cm flux superposed. This image was formed by summing up the …