Relations of stellar mass between electron temperature-based metallicity   of star-forming galaxies in a wide mass range
  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 $10^{11}\,M_\odot$. 
WeiBin Shi, YanChun Liang, Xu Shao, XiaoWei Liu, Gang Zhao, Francois   Hammer, Yong Zhang, Hector Flores, GuiPing Ruan, Li Zhou
astro-ph.GA