标题： H-ATLAS：室女座星系团内和周围的星系的远红外特性 显示英文标题

标题： H-ATLAS: The Far-Infrared properties of galaxies in and around the Coma Cluster

摘要： We describe a far infrared survey of the Coma cluster and the galaxy filament it resides within. Our survey covers an area of $\sim$150 deg$^2$ observed by $Herschel$ H-ATLAS in five bands at 100, 160, 250, 350 and 500$\mu$m. The SDSS spectroscopic survey ($m_{r} \le 17.8)$ is used to define an area (within the Virial radius) and redshift selected ($4268 < v < 9700$ km s$^{-1}$) sample of 744 Coma cluster galaxies - the Coma Cluster Catalogue (CCC). For comparison we also define a sample of 951 galaxies in the connecting filament - the Coma Filament Catalogue (CFC). The optical positions and parameters are used to define appropriate apertures to measure each galaxy's far infrared emission. 我们检测到SPIRE 250$\mu$m波段中99/744（13%）和422/951（44%）的星系团和丝状结构星系。 我们认为不同形态类型的星系的相对检测率，发现只有S0/Sa星系在星系团和丝状结构之间显示出明显的差异。 除早型星系尘埃温度外，星系团和丝状结构星系的尘埃质量和温度没有差异，星系团中的早型星系尘埃温度明显高于丝状结构（X射线加热？）。 从化学演化模型中，我们没有发现星系团和丝状结构中的星系之间存在不同的演化过程（气体损失或吸积）的证据。 显示英文摘要

摘要： We describe a far infrared survey of the Coma cluster and the galaxy filament it resides within. Our survey covers an area of $\sim$150 deg$^2$ observed by $Herschel$ H-ATLAS in five bands at 100, 160, 250, 350 and 500$\mu$m. The SDSS spectroscopic survey ($m_{r} \le 17.8)$ is used to define an area (within the Virial radius) and redshift selected ($4268 < v < 9700$ km s$^{-1}$) sample of 744 Coma cluster galaxies - the Coma Cluster Catalogue (CCC). For comparison we also define a sample of 951 galaxies in the connecting filament - the Coma Filament Catalogue (CFC). The optical positions and parameters are used to define appropriate apertures to measure each galaxy's far infrared emission. We have detected 99 of 744 (13\%) and 422 of 951 (44\%) of the cluster and filament galaxies in the SPIRE 250$\mu$m band. We consider the relative detection rates of galaxies of different morphological types finding that it is only the S0/Sa population that shows clear differences between the cluster and filament. We find no differences between the dust masses and temperatures of cluster and filament galaxies with the exception of early type galaxy dust temperatures, which are significantly hotter in the cluster than in the filament (X-ray heating?). From a chemical evolution model we find no evidence for different evolutionary processes (gas loss or infall) between galaxies in the cluster and filament.