arXiv 2201.013072022-01-04astro-ph.GA

$z\sim1.4$恒星形成星系团中的重要分子气体亏损

Significant Molecular Gas Deficiencies in Star-forming Cluster Galaxies at $z\sim1.4$

Stacey Alberts, Jéa Adams, Benjamin Gregg, Alexandra Pope, Christina C. Williams, Peter R. M. Eisenhardt

备注：: Accepted for publication in ApJ
DOI：: 10.3847/1538-4357/ac48f6

摘要：

我们提出的平均气体性质来自ALMA带6尘埃连续成像的126个大规模（日志$M_{\star} / M_{\odot} \gtrsim 10.5$），恒星形成的星系团星系在11个星系团在$z=1-1.75$。使用叠加分析的ALMA图像，结合紫外远红外数据，我们量化的平均红外SED和气体性质（分子气体质量，$M_{\rm mol}$ ;气体耗尽时标，$τ_{\rm depl}$ ;和气体分数，f $_{\rm gas}$）作为一个函数的集群中心半径和属性，包括恒星质量和距离主序星。我们发现，相对于$-$场的预期值，ALMA通量显着缺乏，$M_{\rm mol}$和f $_{\rm gas}$相应较低，而$τ_{\rm depl}$ $-$较短，对团簇中心半径的依赖性较弱或不依赖，达到维里半径的两倍。Herschel+ALMA SEDs表明尘埃温度（$\sim36-38$ K）比同时代的场星系（$\sim30$ K）更高。我们执行一个彻底的比较团星系的气体属性场星系，发现赤字的2- 3倍，3- 4倍，2- 4倍的$M_{\rm mol}$，$τ_{\rm depl}$，和f $_{\rm gas}$相比，同时代的字段堆栈和更大的赤字相比，主要是建立在检测的字段缩放关系。这里推导出的集群气体性质与堆叠分析（原）集群在文献中，并在不一致的调查结果的领域一样的$τ_{\rm depl}$和增强f $_{\rm gas}$报告使用CO和尘埃连续检测。我们的分析表明，环境有相当大的影响，气体性质的大半径，在良好的协议与宇宙学模拟项目气体耗尽开始超越维里半径，并在很大程度上完成了第一次通过的集群核心。

英文摘要：

We present the average gas properties derived from ALMA Band 6 dust continuum imaging of 126 massive (log $M_{\star} / M_{\odot} \gtrsim 10.5$), star-forming cluster galaxies across 11 galaxy clusters at $z=1-1.75$. Using stacking analysis on the ALMA images, combined with UV-far-infrared data, we quantify the average infrared SEDs and gas properties (molecular gas masses, $M_{\rm mol}$; gas depletion timescales, $τ_{\rm depl}$; and gas fractions, f$_{\rm gas}$) as a function of cluster-centric radius and properties including stellar mass and distance from the Main Sequence. We find a significant dearth in the ALMA fluxes relative to that expected in the field $-$ with correspondingly low $M_{\rm mol}$ and f$_{\rm gas}$ and short $τ_{\rm depl}$ $-$ with weak or no dependence on cluster-centric radius out to twice the virial radius. The Herschel+ALMA SEDs indicate warmer dust temperatures ($\sim36-38$ K) than coeval field galaxies ($\sim30$ K). We perform a thorough comparison of the cluster galaxy gas properties to field galaxies, finding deficits of 2-3x, 3-4x, and 2-4x in $M_{\rm mol}$, $τ_{\rm depl}$, and f$_{\rm gas}$ compared to coeval field stacks and larger deficits compared to field scaling relations built primarily on detections. The cluster gas properties derived here are comparable with stacking analyses in (proto-)clusters in the literature and at odds with findings of field-like $τ_{\rm depl}$ and enhanced f$_{\rm gas}$ reported using CO and dust continuum detections. Our analysis suggests that environment has considerable impact on gas properties out to large radii, in good agreement with cosmological simulations which project gas depletion begins beyond the virial radius and largely completes by first passage of the cluster core.

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