ZFIRE：星系团动力学、H $α$恒星形成速率和XMM-LSS J02182-05102在z=1.6233时的气相金属丰度
ZFIRE: Galaxy Cluster Kinematics, H$α$ Star Formation Rates, and Gas-Phase Metallicities of XMM-LSS J02182-05102 at z=1.6233
摘要：
作为ZFIRE巡天的一部分，我们使用凯克一号卫星上的LRIS（光学）和MOSFIRE（近红外）对星系团XMM-LSS J 02182 -05102（以下简称IRC 0218）进行了光谱巡天。IRC 0218有一个窄的红移范围$1.612<z_{\rm spec}<1.635$，由33个成员定义，其中20个在R $_{\rm proj}<1$ Mpc。星系团的红移和速度色散分别为$z_{\rm cl}=1.6233\pm0.0003$和$σ_{\rm cl}=254\pm50$ km s $^{-1}$。我们达到近红外线灵敏度的$\sim0.3\times10^{-17}$ erg的$^{-1}$厘米$^{-2}$，结合多波长光度，提供修正的H $α$恒星形成率（SFR），气相金属丰度从[NII]/H $α$，和恒星质量。我们测量了$\sim325{\rm M}_{\odot}$ yr $^{-1}$（26个成员; R $_{\rm proj}<2$ Mpc）的综合H $α$ SFR，并表明在星团核心（R $_{\rm proj}<0.25$ Mpc）中的恒星形成是由恒星形成成员的浓度驱动的，但每个H $α$检测到的星系的平均SFR是R $_{\rm proj}\sim1$ Mpc成员的一半。然而，我们没有检测到任何环境的印记时，比较衰减和气相金属丰度：团星系表现出类似的趋势与M $_{\star}$的字段，例如，更大的质量星系有更大的恒星衰减。IRC 0218的气相金属度-M $_{\star}$关系（MZR）相对于$z\sim0$偏移到较低的金属度，斜率为$0.13\pm0.10$。将IRC 0218中的MZR与$z=2.1$的COSMOS星系团进行比较，显示没有演化（$Δt\sim1$ Gyr）：两个星系团的MZR彼此非常一致，并且与$z\sim2$的几次实地调查几乎相同。
英文摘要：
We spectroscopically survey the galaxy cluster XMM-LSS J02182-05102 (hereafter IRC 0218) using LRIS (optical) and MOSFIRE (near-infrared) on Keck I as part of the ZFIRE survey. IRC 0218 has a narrow redshift range of $1.612<z_{\rm spec}<1.635$ defined by 33 members of which 20 are at R$_{\rm proj}<1$ Mpc. The cluster redshift and velocity dispersion are $z_{\rm cl}=1.6233\pm0.0003$ and $σ_{\rm cl}=254\pm50$ km s$^{-1}$. We reach NIR line sensitivities of $\sim0.3\times10^{-17}$ erg s$^{-1}$ cm$^{-2}$ that, combined with multi-wavelength photometry, provide extinction-corrected H$α$ star formation rates (SFR), gas phase metallicities from [NII]/H$α$, and stellar masses. We measure an integrated H$α$ SFR of $\sim325{\rm M}_{\odot}$ yr$^{-1}$ (26 members; R$_{\rm proj}<2$ Mpc) and show that the elevated star formation in the cluster core (R$_{\rm proj}<0.25$ Mpc) is driven by the concentration of star-forming members, but the average SFR per H$α$-detected galaxy is half that of members at R$_{\rm proj}\sim1$ Mpc. However, we do not detect any environmental imprint when comparing attenuation and gas phase metallicities: the cluster galaxies show similar trends with M$_{\star}$ as to the field, e.g. more massive galaxies have larger stellar attenuation. IRC 0218's gas phase metallicity-M$_{\star}$ relation (MZR) is offset to lower metallicities relative to $z\sim0$ and has a slope of $0.13\pm0.10$. Comparing the MZR in IRC 0218 to the COSMOS cluster at $z=2.1$ shows no evolution ($Δt\sim1$ Gyr): the MZR for both galaxy clusters are remarkably consistent with each other and virtually identical to several field surveys at $z\sim2$.
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