Chemical Abundances of a Sample of Oxygen-dominated Galaxies

TL;DR

This study spectroscopically analyzed 85 oxygen-dominated galaxies from SDSS, revealing their chemical compositions, physical properties, and similarities to low-metallicity galaxies like the SMC, with new calibrations for temperature diagnostics.

Contribution

It introduces a new calibration for T([S III]) and provides detailed chemical abundance measurements for a large sample of extreme emission-line galaxies.

Findings

Most galaxies have metallicities similar to the SMC.

Only 12% are extremely metal-poor with 12+log(O/H)<7.7.

Detected high-ionization lines and Wolf-Rayet features in nearly all galaxies.

Abstract

We spectroscopically analyzed a sample of 85 Sloan Digital Sky Survey compact, oxygen-dominated galaxies located at redshift $z\sim0.001-0.350$, selected because of their large equivalent width of [O III]$\lambda$5007 (larger than 200\AA). These galaxies might be considered as extreme emission-line galaxies due to their strong [O III]$\lambda$5007 emission line. We detected high-ionization lines, even those related to the presence of Wolf-Rayet stars, in almost all the galaxies studied. We obtained physical properties (electron density and temperature) as well as chemical abundances by using the direct method based on the electron temperature. In this analysis, we obtained three different measurements of T(high): the usual one, T([O III]), but also that of T([S III]) and T([Ar III]) for five and three of the galaxies, respectively. Further, we established a new calibration for T([S III]). We determined oxygen, nitrogen, sulfur, neon, argon, iron, and chlorine abundances when possible, and we compared to the results of other late-type, low-metallicity galaxies, such as blue compact dwarfs, Ims, and green peas. From such a detailed study, we can conclude that the majority of the galaxies in this sample have similar metallicities to the SMC (about $12+\log(O/H)\approx8$dex), and that only 12% of the galaxies are extremely metal-poor, with abundances lower than $7.7$dex. Also, a comparison with some chemical evolution models as well as a brief discussion on the chemical evolution with time is considered.