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首页> 外文期刊>The Astrophysical journal >THE OXYGEN ABUNDANCES OF LUMINOUS AND ULTRALUMINOUS INFRARED GALAXIES
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THE OXYGEN ABUNDANCES OF LUMINOUS AND ULTRALUMINOUS INFRARED GALAXIES

机译：夜光和超光红外星系的氧丰度

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摘要

Luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) dominate the star formation rate budget of the universe at z ＞ 1, yet no local measurements of their heavy-element abundances exist. We measure nuclear or near nuclear oxygen abundances in a sample of 100 star-forming LIRGs and ULIRGs using new, previously published, and archival spectroscopy of strong emission lines (including [O II] λλ3726, 3729) in galaxies with redshifts (z) ～ 0.1. When compared to local emission-line galaxies of similar luminosity and mass (using the near-infrared luminosity metallicity and mass-metallicity relations), we find that LIRGs and ULIRGs are underabundant by a factor of 2 on average. As a corollary, LIRGs and ULIRGs also have smaller effective yields. We conclude that the observed under abundance results from the combination of a decrease of abundance with increasing radius in the progenitor galaxies and strong, interaction- or merger-induced gas inflow into the galaxy nucleus. This conclusion demonstrates that local abundance scaling relations are not universal, a fact that must be accounted for when interpreting abundances earlier in the universe's history, when merger-induced star formation was the dominant mode. We use our local sample to compare to high-redshift samples and assess abundance evolution in LIRGs and ULIRGs. We find that abundances in these systems increased by ～0.2 dex from z ～ 0.6 to z～ 0.1. Evolution from z ～ 2 submillimeter galaxies to z ～ 0.1 ULIRGs also appears to be present, although uncertainty due to spectroscopic limitations is large.
机译：发光和超发光的红外星系（LIRG和ULIRG）在z＞ 1时支配着宇宙的恒星形成速率预算，但尚无局部测量其重元素丰度的信息。我们使用新的，先前发表的，以及具有红移（z）〜的星系中强发射线（包括[O II] λλ3726、3729）的新的档案和归档光谱学，对100个恒星形成的LIRG和ULIRG的样本中的核或近核氧丰度进行了测量〜 0.1。当与具有相似亮度和质量的局部发射星系（使用近红外发光度金属性和质量-金属性关系）进行比较时，我们发现LIRGs和ULIRGs的平均数量不足2倍。因此，LIRG和ULIRG的有效产量也较小。我们得出的结论是，观测到的丰度来自祖细胞星系中丰度的降低与半径的增加以及强烈，相互作用或合并诱导的气体流入星系核的结合。该结论表明，局部丰度缩放关系不是普遍的，当合并历史中的恒星形成为主导模式时，在解释宇宙历史早期的丰度时必须考虑这一事实。我们使用本地样本与高红移样本进行比较，并评估LIRG和ULIRG中的丰度演变。我们发现这些系统中的丰度从z〜0.6增加到z〜0.1，增加了〜0.2 dex。从z〜2亚毫米星系到z〜0.1 ULIRG的演化似乎也存在，尽管由于光谱限制而不确定性很大。

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