ASCA Observations of the NGC 2264 Molecular Cloud
ASCA Observations of the NGC 2264 Molecular Cloud
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ASCA 对 NGC 2264 分子云的观测
DOI：
10.1093/pasj/52.3.437
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发表时间：
2000
期刊：
影响因子：
--
通讯作者：
K. Ogura
中科院分区：
文献类型：
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作者：
M. Nakano;S. Yamauchi;K. Sugitani;K. Ogura
我们对NGC 2264相关的分子云进行了ASCA观测，并在软X射线带图像和硬X射线带图像中分别检测到了9个和5个源。其中大多数被认为是已知的前主序星或原恒星天体。两个具有中等亮度的 I 类源和一个与分子流出相关的 II 类源是 X 射线发射器的有希望的候选者。具有两个组件的光学薄热等离子体模型可以再现 GIS X 射线光谱，包括两个 I 类源。硬X射线可能来自这些I类源，并且本质上非常明亮，在0.7-10.0 keV能带中>1032erg s−1，并且它们的光度位于低质量I类源和W 3大质量核心区域的光度之间。由于近红外巡天数据显示 I 类源被嵌入的年轻星团包围，因此软 X 射线成分可以用低质量前主序星的聚集来解释。
We have made ASCA observations of the molecular cloud associated with NGC 2264, and detected nine and five sources in the soft and hard X-ray band images, respectively. Most of them are identified with known pre-main-sequence stars or protostellar objects. Two Class I sources with intermediate luminosities and one Class II source associated with molecular outflow are promising candidates for X-ray emitters. An optically thin hot-plasma model with two components can reproduce the GIS X-ray spectra, including both of the Class I sources. The hard X-rays probably arise from these Class I sources, and are intrinsically very luminous, >1032erg s−1in the 0.7–10.0 keV energy band, and their luminosities lie between low-mass Class I sources and that of the W 3 massive core region. Since near-infrared survey data reveal that Class I sources are surrounded by embedded young clusters, the soft X-ray components could be explained by aggregates of low-mass pre-main-sequence stars.