Oxygen abundance in giant H II galaxies |
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Authors: | L S Pilyugin I A Zinchenko T X Thuan |
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Institution: | (1) NARO, National Radio Astronomy Observatory Tucson, 949 North Cherry Avenue, Tucson, AZ 857521-0655, USA;(2) Russian Academy of Sciences, P.N. Lebedev Physical Institute, Laninsky Prospect 53, Moskva, 119991, Russia |
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Abstract: | A sample of 93 emission-line high luminosity galaxies from the Sloan Digital Sky Survey (SDSS) has been investigated. Line
intensities have been measured in 116 SDSS spectra. Oxygen abundance has been determined in the studied galaxies. Since the
auroral line of twice ionized oxygen O III] λ 436.3 nm cannot be detected in the spectra of the sample, the intensity ratio
of nebular to auroral lines needed to determine the electron temperature is calculated using the ff-relation. The oxygen abundances obtained in SDSS high luminosity galaxies are 0.2–0.5 dex lower than the maximum attainable
value. This is caused by the fact that the sample includes only the gas-rich galaxies in which intense bursts of star formation
occur. The equivalent number of O7 V stars which are responsible for excitation of luminescent H II regions in the studied
sample is two or three orders of magnitude more than the number of stars which cause the luminescence of the brightest H II
regions in nearby galaxies, and it exceeds by one order of magnitude the number of stars which cause gas in SBS 0335-052 E
to glow. |
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