NGC 3576 and NGC 3603: Two Luminous Southern HII Regions Observed at High Resolution with the Australia Telescope Compact Array

Details NGC 3576 and NGC 3603: Two Luminous Southern HII Regions Observed at High Resolution with the Australia Telescope Compact Array NGC 3576 and NGC 3603: Two Luminous Southern HII Regions Observed at High Resolution with the Australia Telescope Compact Array

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.1601d&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #16.01; Bulletin of the American Astronomical Society, Vol. 30, p.1276

Astronomy and Astrophysics

Astronomy

Scientific paper

NGC 3576 (l = 291.3(o) , b = -0.7(o) ) and NGC 3603 (l = 291.6(o) , b = -0.5(o) ) are optically visible, luminous HII regions located at distances of 3.0 kpc and 7.7 kpc, respectively. We present 3.4 cm Australian Telescope Compact Array (ATCA) observations of these two sources in the continuum and the H90alpha , He90alpha , C90alpha and H113beta recombination lines with an angular resolution of 7('') and a velocity resolution of 2.6 km s(-1) . All four recombination lines are detected in the integrated spectra of the two sources. Broad radio recombination lines are detected in both NGC 3576 (Delta VFWHM >= 50 km s(-1) ) and NGC 3603 (Delta VFWHM >= 70 km s(-1) ). In NGC 3576 a prominent N-S velocity gradient ( ~ 30 km s(-1) pc(-1) ) is observed, and a clear temperature gradient (6000 K to 8000 K) is found from east to west, consistent with a known IR color gradient in the source. In NGC 3603, the H90alpha , He90alpha and the H113beta lines are detected from 13 individual sources. The Y+ (He/H) ratios in the two sources range from 0.07+/-0.01 to 0.21+/-0.05. The H113beta /H90alpha ratio in NGC 3576 is close to the theoretical value, suggesting that local thermodynamic equilibrium (LTE) exists. This ratio is enhanced for most regions in NGC 3603, which may be the result of high optical depth or stimulated emission. We compare the morphology and kinematics of the ionized gas at 3.4 cm with the distribution of stars, 10micron emission and H_2O and CH_3OH maser emission. These comparisons suggest that both NGC 3576 and NGC 3603 have undergone sequential star formation.

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