An XMM–Newton and Chandra study of the starburst galaxy IC 10
An XMM–Newton and Chandra study of the starburst galaxy IC 10
复制标题
XMM-牛顿和钱德拉对星暴星系 IC 10 的研究
DOI：
--
复制
发表时间：
2005
期刊：
影响因子：
--
通讯作者：
R. Williams
中科院分区：
文献类型：
--
作者：
Q. Wang;K. Whitaker;R. Williams
基于XMM-牛顿和钱德拉的观测，我们给出了最近的恒星爆发星系IC10的X射线研究。列出了73个XMM-牛顿和28个钱德拉探测到的场内点状X射线源；由于IC10所在的银河系纬度较低，其中很大一部分可能是银河系中的恒星物体。IC10场中最亮的源X-1的平均光度为∼1.2×1038erg S-1，在XMM-牛顿观测期间，在∼104 S的时间尺度上，X-1的平均光度变化高达∼6。源的X射线光谱表明存在一个多色黑体吸积盘，其内部盘温度T为1.1keV。这些结果与恒星质量黑洞(BH)的解释是一致的，BH可能是从Wolf-Rayet(W-R)伴星中吸积而来的。我们推测这个BH的质量为∼4M0.如果它没有旋转，或者如果有显著的旋转，则系数高达∼6。我们还探测到了IC10的一个明显的扩散软X射线发射分量。我们设计了一种有效的方法来消除XMM-牛顿和钱德拉观测中强烈影响扩散分量研究的X-1的X射线CCD读出条纹。我们发现漫射X射线的形态是沿着星系的光学体定向的，并且主要与恒星暴发区有关。漫射分量可以由平均温度为∼4 x 10 6K、光度为∼8 x 10 37 erg S-1的光学薄热等离子体来表征，这只是银河系中大质量恒星预期机械能输入的一小部分。有证据表明，热气体正在推动星暴区域的外流；因此，大部分能量输入可能是在银河系风中释放的。
We present an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. A list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field is provided; a substantial fraction of them are likely stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ∼1.2 × 10 38 erg s -1 and shows a large variation by a factor of up to ∼6 on time-scales of ∼10 4 s during the XMM-Newton observation. The X-ray spectra of the source indicate the presence of a multicolour blackbody accretion disc with an inner disc temperature T in 1.1 keV. These results are consistent with the interpretation of the source as a stellar mass black hole (BH), probably accreting from a Wolf-Rayet (W-R) star companion. We infer the mass of this BH to be ∼4 M ○. if it is not spinning, or a factor of up to ∼6 higher if there is significant spinning. We also detect an apparent diffuse soft X-ray emission component of IC 10. An effective method is devised to remove the X-ray CCD-readout streaks of X-1 that strongly affect the study of the diffuse component in the XMM-Newton and Chandra observations. We find that the diffuse X-ray morphology is oriented along the optical body of the galaxy and is chiefly associated with starburst regions. The diffuse component can be characterized by an optically thin thermal plasma with a mean temperature of ∼4 x 10 6 K and a 0.5-2 keV luminosity of ∼8 x 10 37 erg s -1 , representing only a small fraction of the expected mechanical energy inputs from massive stars in the galaxy. There is evidence that the hot gas is driving outflows from the starburst regions; therefore, the bulk of the energy inputs may be released in a galactic wind.