Formation and Evolution of Massive Stars, and the Chemical Evolution of Galaxies

Details Formation and Evolution of Massive Stars, and the Chemical Evolution of Galaxies Formation and Evolution of Massive Stars, and the Chemical Evolution of Galaxies

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992hst..prop.3813r&link_type=abstract

HST Proposal ID #3813

Computer Science

Hst Proposal Id #3813

Scientific paper

FOS spectra at R = 560, completely covering the wavelength range 1150 A to 9260 A will be obtained of the cores of 4 giant H II regions in M 101. Taken through one and the same aperture, the UV, visual and far-red emission line spectra of the ionized gas will allow for the first time an accurate determina- tion of the C/O abundance ratio in an extragalactic object over a wide range of O/H abundances. Furthermore, the S/O abundance ratio will be obtained with much higher precision than possible from ground using the prominent [S III] 9036 A line, unaffected by strong H2O atmospheric absorption. Finally, the spatially integrated spectra of the ionizing star clusters will be analyzed using WFC evolutionary population synthesis models. Because the whole spectral range is observed through the same aperture, scaling errors between ground based and IUE UV data, which have been so far a major obstacle in such an analysis, will be absent. The nebular continuous emission, which is contributing typically 50 % of the total flux at 3000 A, can be very accurately estimated using the H BETA line flux obtained through the same aperture.The data will be discussed in the context of galactic chemical evolution, for which C/O and S/O gradients, which are indicative of contributions from different stellar mass ranges, are of particular interest. The stellar initial mass function and the evolutionary scenarios for massive stars will be studied over a range of metallicity from 1/5 to 2 times the solar neighborhood value.

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