Abstract

We obtained equations for determining the star-formation rate in local compact star-forming galaxies from the SDSS Data Release 16 using luminosities of the forbidden emission lines [O II] λ 372.7 nm, [Ne III] λ 386.8 nm, [O III] λ 495.9 nm, and [O III] λ 500.7 nm and their combinations. The equations are based on the assumption that the star-formation rates, determined from the luminosity of the forbidden lines and H_β emission lines, are equal. This approach is especially useful because the observation of H_β emission is not always possible. For example, in galaxies with redshift z > 1, this line goes beyond the optical range, and the [O II] λ 372.7 nm line, the [Ne III] λ 386.8 nm line, or their combination can be used instead. On the other hand, in many studies of faint objects using low-resolution spectra, the H_β line merges with the stronger [O III] λ 495.9 nm and [O III] λ 500.7 nm lines. In these cases, [O III] lines and their combination can be used to determine the rate of star formation. The resulting equations can be applied to compact star-forming galaxies in a wide range of redshifts.

中文翻译：

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SDSS 数据第 16 版中具有活跃恒星形成的致密星系：基于光学范围内禁止发射线光度的恒星形成率

摘要

我们使用禁止发射线 [O II] λ 372.7 nm、[Ne III] λ 386.8 nm、[O III] 的光度从 SDSS 数据发布 16 中获得了确定局域致密恒星形成星系中恒星形成速率的方程式λ 495.9 nm 和 [O III] λ 500.7 nm 及其组合。_{这些方程基于这样的假设，即由禁线和 H β}发射线的光度确定的恒星形成率是相等的。_{这种方法特别有用，因为 H β}发射的观察并不总是可能的。例如，在红移z的星系中> 1，此谱线超出光学范围，可用[O II] λ 372.7 nm谱线、[Ne III] λ 386.8 nm谱线或它们的组合代替。另一方面，在许多使用低分辨率光谱的微弱物体研究中，H _β线与更强的 [O III] λ 495.9 nm 和 [O III] λ 500.7 nm 线合并。在这些情况下，[O III] 线及其组合可用于确定恒星形成的速率。由此产生的方程式可以应用于大红移范围内的致密恒星形成星系。