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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >The mass-metallicity relation of AKARI-FMOS infrared galaxies at z similar to 0.88 in the AKARI North Ecliptic Pole Deep Survey Field
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The mass-metallicity relation of AKARI-FMOS infrared galaxies at z similar to 0.88 in the AKARI North Ecliptic Pole Deep Survey Field

机译：Akari-MMOS红外星系在Akari North Ecliptic Pole Deep Resource田中Akari-FMOS红外星系的质量金属关系与0.88相似

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摘要

The mass, metallicity, and star formation rate (SFR) of a galaxy are crucial parameters in understanding galaxy formation and evolution. However, the relation between these parameters, (i.e., the fundamental relation) is still a matter of debate for luminous infrared (IR) galaxies, which carry a bulk of the SFR budget of the universe at z similar to 1. We have investigated the relation among stellar mass, gas-phase oxygen abundance, and SFR of the Japanese infrared satellite AKARI-detected mid-IR galaxies at z similar to 0.88 in the AKARI north ecliptic pole deep field. We observed similar to 350 AKARI sources with Subaru/Fiber Multi Object Spectrograph near-IR spectrograph, and detected confirmed H alpha emission lines from 25 galaxies and expected Ha emission lines from 44 galaxies. The SFRH alpha, IR of our sample is almost constant (< SFRH alpha, IR > = similar to 25M(circle dot) yr(-1)) over the stellar mass range of our sample. Compared with main-sequence (MS) galaxies at a similar redshift range (z similar to 0.78), the average SFR of our detected sample is comparable for massive galaxies (similar to 10(10.58) M-circle dot), while higher by similar to 0.6 dex for less massive galaxies (similar to 10(10.05) M-circle dot). We measure metallicities from the [N II]/H alpha emission line ratio. We find that the mass-metallicity relation of our individually measured sources agrees with that for optically-selected star-forming galaxies at z similar to 0.1, while metallicities of stacked spectra agree with that of MS galaxies at z similar to 0.78. Considering the high SFR of individually measured sources, the fundamental metallicity relation (FMR) of the IR galaxies is different from that at z similar to 0.1. However, on the mass-metallicity plane, they are consistent with the MS galaxies, highlighting the higher SFR of the IR galaxies. This suggests that the evolutionary path of our infrared galaxies is different from that of MS galaxies. A possible physical interpretation includes that the star-formation activities of IR galaxies at z similar to 0.88 in our sample are enhanced by interactions and/or mergers of galaxies, but the inflow of metal-poor gas is not yet induced, keeping the metallicity intact.
机译：星系的质量、金属丰度和恒星形成率（SFR）是理解星系形成和演化的关键参数。然而，对于发光的红外（IR）星系来说，这些参数之间的关系（即基本关系）仍然是一个有争议的问题，它们在z处携带着宇宙的大部分SFR预算，类似于1。我们研究了日本红外卫星AKARI在AKARI北黄道极深场中探测到的z类似于0.88的中红外星系的恒星质量、气相氧丰度和SFR之间的关系。我们用Subaru/光纤多目标光谱仪近红外光谱仪观测了350个类似的AKARI源，并检测到来自25个星系的确认Hα发射线和来自44个星系的预期Ha发射线。在样品的恒星质量范围内，样品的SFRHα，IR几乎是恒定的（=类似于25M（圆点）yr（-1））。与红移范围相似（z类似于0.78）的主序列（MS）星系相比，我们检测到的样本的平均SFR对于大质量星系（类似于10（10.58）米圆点）是可比的，而对于质量较小的星系（类似于10（10.05）米圆点），其平均SFR更高，类似于0.6 dex。我们通过[N II]/Hα发射线比率测量金属丰度。我们发现，我们单独测量的源的质量金属丰度关系与光学选择的恒星形成星系在z处的质量金属丰度关系类似于0.1，而叠加光谱的金属丰度与MS星系在z处的质量金属丰度关系类似于0.78。考虑到单独测量源的高SFR，IR星系的基本金属丰度关系（FMR）与z处的基本金属丰度关系（FMR）不同，类似于0.1。然而，在质量金属丰度平面上，它们与MS星系一致，突出了IR星系更高的SFR。这表明我们红外星系的演化路径不同于MS星系。一种可能的物理解释是，在我们的样本中，z类似于0.88的红外星系的恒星形成活动因星系的相互作用和/或合并而增强，但贫金属气体的流入尚未被诱导，从而保持了金属丰度的完整性。

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