Relations of stellar mass between electron temperature-based metallicity of star-forming galaxies in a wide mass range
2014
We select 947 star-forming galaxies from SDSS-DR7 with
[O~{\sc iii}]$\lambda$4363 emission lines
detected at a signal-to-noise {ratio }larger than 5$\sigma$.
Their electron temperatures and direct oxygen abundances are {then }determined. {W}e
compare the results from different methods. $t_2${, the} electron
temperature in {the }low ionization region{,} estimated from $t_3${, that} in {the }high ionization region{,} {is} compared {using} three analysis
relations between $t_2-t_3${. These} show obvious differences, which
result in some different ionic oxygen abundances. The results of
$t_3$, $t_2$, {$\rm O^{++}$/$\rm H^+$} and {$\rm O^{+}$/$\rm H^+$} derived by using
methods from IRAF and literature are also compared. The ionic
abundances $\rm O^{++}$/$\rm H^+$ {are} higher than $\rm O^{+}$/$\rm H^+$ for most
cases. The{ different} oxygen abundances derived from $T_{\rm e}$ and the strong-line ratios show {a }clear discrepancy, which is more obvious
following increasing stellar mass and strong-line ratio
$R_{23}$. The sample{ of} galaxies from SDSS {with}
detected [O~{\sc iii}]$\lambda$4363 have lower metallicites and
higher {star formation rates}, {so} they may not be typical representatives of the
whole{ population of} galaxies. Adopting data objects from
{Andrews \& Martini}, {Liang et al.} and {Lee et al.} data, we derive new relations of stellar mass and metallicity for star-forming
galaxies in a much wider stellar mass range: from $10^6\,M_\odot$
to $10^{11}\,M_\odot$.
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