英仙座星系团中CN（2-1），HCO $^{+}$（3-2）和C $_{2}$ H（3-2）发射线的首次观测：星系团气体加热机制的限制
First observations of CN(2-1), HCO$^{+}$(3-2) and C$_{2}$H(3-2) emission lines in the Perseus cluster: constraints on heating mechanisms in the cluster gas
摘要：
我们首次在英仙座星系团中观测到CN（2-1），HCO $^{+}$（3-2）和C $_{2}$ H（3-2）的发射谱线。我们观察了两个位置：直接在中央星系NGC 1275，也在大约20 $''$以东的位置，那里的相关的行星结构已被证明有强烈的CO排放。CN和HCO $^{+}$跃迁在NGC 1275中得到了清晰的检测，而C $_{2}$ H跃迁的检测很弱，而CN和HCO $^{+}$的检测很弱。柱密度和丰度分数（主要是上限）作为一个未知的旋转温度的函数的粗估计，这两个来源。这些观测数据与\citet{Baye10c}以前发表的热/化学模型的输出进行了比较，试图限制团簇气体的加热机制。我们发现，加热是由宇宙射线占主导地位的模型可以解释的分子观测。这一结论与\citet{Ferl09}在研究光学和红外辐射示踪气体时的结论一致。在分子辐射探测的区域，宇宙射线加热率至少要比银河系大两个数量级。
英文摘要：
We present the first observations of emission lines of CN(2-1), HCO$^{+}$(3-2) and C$_{2}$H(3-2) in the Perseus cluster. We observed at two positions: directly at the central galaxy, NGC 1275 and also at a position about 20$''$ to the east where associated filamentary structure has been shown to have strong CO emission. Clear detections in CN and HCO$^{+}$ transitions and a weak detection of the C$_{2}$H transition were made towards NGC 1275, while weak detections of CN and HCO$^{+}$ were made towards the eastern filamentary structure. Crude estimates of the column densities and fractional abundances (mostly upper limits) as functions of an unknown rotational temperature were made to both sources. These observational data were compared with the outputs of thermal/chemical models previously published by \citet{Baye10c} in an attempt to constrain the heating mechanisms in cluster gas. We find that models in which heating is dominated by cosmic rays can account for the molecular observations. This conclusion is consistent with that of \citet{Ferl09} in their study of gas traced by optical and infrared radiation. The cosmic ray heating rate in the regions probed by molecular emissions is required to be at least two orders of magnitude larger than that in the Milky Way.
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