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Properties and redshift evolution of star-forming galaxies with high [O? III]/[O? II] ratios with MUSE at 0.28?&? z?&?0.85

机译:高[O?]的恒星形成星系的性质和红移演化。 III ] / [O? II ]比率,MUSE为0.28?&lt ;? z ?<?0.85

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We present a study of the [O? III ]/[O? II ] ratios of star-forming galaxies drawn from Multi-Unit Spectroscopic Explorer (MUSE) data spanning a redshift range 0.28 < z < 0.85. Recently discovered Lyman continuum (LyC) emitters have extremely high oxygen line ratios: [O? III ] λ 5007/[O? II ] λλ 3726, 3729 > 4. Here we aim to understand the properties and the occurrences of galaxies with such high line ratios. Combining data from several MUSE Guaranteed Time Observing (GTO) programmes, we select a population of star-forming galaxies with bright emission lines, from which we draw 406 galaxies for our analysis based on their position in the z -dependent star formation rate (SFR)–stellar mass ( M _(?)) plane. Out of this sample 15 are identified as extreme oxygen emitters based on their [O? III ]/[O? II ] ratios (3.7%) and 104 galaxies have [O? III ]/[O? II ] > 1 (26%). Our analysis shows no significant correlation between M _(?), SFR, and the distance from the SFR? M _(?)relation with [O? III ]/[O? II ]. We find a decrease in the fraction of galaxies with [O? III ]/[O? II ] > 1 with increasing M _(?), however, this is most likely a result of the relationship between [O? III ]/[O? II ] and metallicity, rather than between [O? III ]/[O? II ] and M _(?). We draw a comparison sample of local analogues with ? z ? ≈ 0.03 from the Sloan Digital Sky Survey, and find similar incidence rates for this sample. In order to investigate the evolution in the fraction of high [O? III ]/[O? II ] emitters with redshift, we bin the sample into three redshift subsamples of equal number, but find no evidence for a dependence on redshift. Furthermore, we compare the observed line ratios with those predicted by nebular models with no LyC escape and find that most of the extreme oxygen emitters can be reproduced by low metallicity models. The remaining galaxies are likely LyC emitter candidates.
机译:我们对[O? III] / [O? II]从跨红移范围0.28 4。在这里,我们旨在了解具有如此高线比率的星系的性质和出现。结合多个MUSE保证时间观测(GTO)计划的数据,我们选择了具有明亮发射线的恒星形成星系,根据它们在z依赖恒星形成率(SFR)中的位置,从中得出406个星系进行分析。 )–星体质量(M _(?))平面。根据这些样品的[O2? III] / [O? II]比率(3.7%)和104个星系具有[O? III] / [O? II]> 1(26%)。我们的分析表明,M _(?),SFR和距SFR?的距离之间无显着相关性。 M _(?)与[O? III] / [O? II]。我们发现[O?]减少了星系的比例。 III] / [O? II]> 1随着M _(?)的增加,但是,这很可能是[O? III] / [O? II]和金属性,而不是[O? III] / [O? II]和M _(?)。我们绘制一个带有?的本地类似物的比较样本。 ? ≈Sloan Digital Sky Survey的0.03,发现该样本的发生率相似。为了研究高[O? III] / [O? II]发射器具有红移,我们将样本分为三个相等数量的红移子样本,但没有证据表明对红移有依赖性。此外,我们将观察到的线比率与没有LyC逸出的星云模型所预测的线比率进行比较,发现大多数极端的氧气排放源可以通过低金属性模型重现。其余的星系很可能是LyC发射体的候选者。

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