How metal-rich are metal-rich H II regions

Details How metal-rich are metal-rich H II regions How metal-rich are metal-rich H II regions

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...282l..37k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 282, no. 3, p. L37-L40

Astronomy and Astrophysics

Astrophysics

40

Abundance, Astronomical Models, H Ii Regions, Line Spectra, Metallicity, Photoionization, Spectrophotometry, Calibrating, Mathematical Models, Visible Spectrum

Scientific paper

We have obtained deep spectrophotometry of the metal-rich H II region Searle 5 in M 101. This objects plays an important role in the calibration of the high-metallicity branch of the empirical bright-line methods for chemical abundance determinations. For the first time, the temperature sensitive auroral lines (NII) 5755 A, (SIII) 6312 A and (OIII) 7320/7330 A are clearly detected. A photoionization model fit to the observed line spectrum including the auroral line intensities gives value of 12+log (O/H)=8.9. This is in contrast to the high value of 9.1 frequently used to calibrate the high-metallicity branch of extra-galactic H II region abundances. The downward re-calibration by 0.2 dex establishes more solar-like O/H values for the great majority of H II regions studied by narrow band techniques in the recent literature.

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