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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，金属性和星形形成速率（SFR）是了解银河形成和演化的关键参数。然而，这些参数之间的关系（即基本关系）仍然是对于发光红外（IR）星系的辩论问题，它在类似于1的Z中携带宇宙的大部分SFR预算。我们已经调查了在Z时，日本红外卫星Akari检测到的日本红外卫星Akari检测到的中外红外星系中的恒星质量，气相氧气丰度和SFR之间的关系。我们观察到与Subaru / Fiber Multi物体光谱仪附近的350个Akari来源接近IR光谱仪，并检测到来自25个星系的确认的H alpha排放线，预计来自44个星系的HA排放线。 SFRH alpha，我们的样品的IR几乎是恒定的（ =与我们样品的恒星质量范围内的25米（圆点）YR（-1））。与类似红移范围（类似于0.78的Z类似的主序列（MS）星系相比，我们检测到的样品的平均SFR对于大规模星系（类似于10（10.58）M圆点），而相似对于较少的大规模星系（类似于10（10.05）m圆点）至0.6°。我们测量[N II] / H alpha排放线比的金属性。我们发现我们单独测量的源的质量金属性关系同意，对于Z的光学选择的星形星系，其Z类似于0.1，而堆叠光谱的金属与类似于0.78的Z的MS星系。考虑单独测量的源的高SFR，IR星系的基本金属关系（FMR）与类似于0.1的Z的不同之处不同。然而，在质量金属性平面上，它们与MS星系一致，突出了IR星系的更高的SFR。这表明我们的红外星系的进化路径与MS星系的进化路径不同。可能的物理解释包括通过星系的相互作用和/或相互作用和/或相似的Z处于类似于0.88的IR星系的星形成活动，但尚未诱导金属差气体的流入，保持金属性完整。

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