X-Rays from HH 80, HH 81, and the Central Region
X-Rays from HH 80, HH 81, and the Central Region
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DOI：
10.1086/382220
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发表时间：
2004-03
期刊：
影响因子：
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通讯作者：
S. Pravdo;Y. Tsuboi;Y. Maeda
中科院分区：
文献类型：
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作者：
S. Pravdo;Y. Tsuboi;Y. Maeda
我们报告了钱德拉 X 射线天文台上的 ACIS 仪器对 HH 80 和 HH 81 的 X 射线的探测。它们是光学领域最亮的赫比格-哈罗 (HH) 光源之一，也是目前已知的 X 射线中最亮的光源。这些X射线是由两极外流向南延伸撞击周围物质时发生的强烈冲击产生的。高X射线发射区域和高Hα发射区域之间存在一一对应的关系。 HH 80 和 HH 81 的 X 射线光度分别为 4.5 和 4.3 × 1031 ergs-1，假设测量到的低能量吸收不在源中。 HH 等离子体的测量温度并不像从光学发射线的延伸尾部中看到的最大速度所预期的那么大。相反，它与光线路“窄”核心的~106 K 温度一致。根据较低灵敏度的测量，没有观测到来自双极流向北延伸的 HH 80 North 的发射。我们对双极流的中心区域进行了成像，揭示了复杂的 X 射线源，其中包括一个接近但与无线电和红外推定电源不重合的 X 射线源。该光源，CXOPTM J181912.4-204733，在其他波长下没有对应物，并且在光度和光谱方面与 AV ~ 90 mag 的大质量恒星一致。它可能会对综合体的电力输入做出重大贡献。或者，这种发射可能是来自靠近电源的流出物的扩展 X 射线。我们在这个恒星形成区域总共检测到 94 个 X 射线源。
We report detections of X-rays from HH 80 and HH 81 with the ACIS instrument on the Chandra X-Ray Observatory. These are among the most luminous Herbig-Haro (HH) sources in the optical, and they are now the most luminous known in X-rays. These X-rays arise from the strong shocks that occur when the southern extension of this bipolar outflow slams into the ambient material. There is a one-to-one correspondence between regions of high X-ray emission and high Hα emission. The X-ray luminosities of HH 80 and HH 81 are 4.5 and 4.3 × 1031 ergs s-1, respectively, assuming that the measured low-energy absorption is not in the sources. The measured temperature of the HH plasma is not as large as that expected from the maximum velocities seen in the extended tails of the optical emission lines. Rather, it is consistent with the ~106 K temperature of the "narrow" core of the optical lines. There is no observed emission from HH 80 North, the northern extension of the bipolar flow, based on a measurement of lower sensitivity. We imaged the central region of the bipolar flow revealing a complex of X-ray sources, including one near but not coincident with the putative power source in the radio and infrared. This source, CXOPTM J181912.4-204733, has no counterparts at other wavelengths and is consistent in luminosity and spectrum with a massive star with AV ~ 90 mag. It may contribute significantly to the power input to the complex. Alternatively, this emission might be extended X-rays from outflows close to the power source. We detect 94 X-ray sources overall in this area of star formation.