High resolution observations of radio recombination lines from starburst galaxies

Details High resolution observations of radio recombination lines from starburst galaxies High resolution observations of radio recombination lines from starburst galaxies

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.4508r&link_type=abstract

American Astronomical Society, 200th AAS Meeting, #45.08; Bulletin of the American Astronomical Society, Vol. 34, p.715

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We present high-resolution ( ~ 1" ) observations of radio recombination lines (RRL) H92α (3.6 cm) and H53α (0.7 mm) from the starburst galaxies M82, NGC 253 and Arp 220 using the VLA of the NRAO. By using the H92α RRL observations we obtained the velocity field in the central regions of M82 and NGC 253. For M82 we fitted a rotation curve for the ionized gas. The inclination of the plane of rotation was found to be ~ 70o, a position angle of 65o, center of rotation at 200 km s-1 and observed solid body rotation for the central ~ 150 pc. In the superbubble region of M82, the peaks in the integrated emission of H92α line emission are coincident with the 12CO line emission, implying close interaction of the ionized and molecular gas and resembling the shell structure proposed by Wills et al. (1999). We modeled the H92α and H53α RRLs emission by using low-density and high-density HII regions and derived values for densities (103, 105 cm-3) temperatures ( ~ 5x 103 K), sizes (5, 0.05 pc) and number of HII regions ( ~ 500, 50) that fit the observations. The H53α line emission is detected from a few compact sources. From the models we found that the H53α line emission arises in a few high density HII regions. The National Radio Astronomy Observatory (NRAO) is a facility of the National Science Foundation operated under a cooperative agreement by Associated Universities, Inc.

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