The X-ray structure and spectrum of NGC 6251
The X-ray structure and spectrum of NGC 6251
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NGC 6251的X射线结构和能谱
DOI：
10.1086/172944
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发表时间：
1993
期刊：
影响因子：
--
通讯作者：
D. Worrall
中科院分区：
文献类型：
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作者：
M. Birkinshaw;D. Worrall
用ROSAT卫星上的位置敏感正比计数器在低能X射线中观测到NGC 6251。4.没有看到X射线发射。'5长的射电喷流，这表明电子光谱被切断的电子能量大于Emax 10 12 eV，但明亮的X射线源与星系的中心重合。这个源中的大多数计数都是在一个小角尺寸的分量中，FWHM<4“，对应于一个小于3 kpc的线性尺寸，尽管有证据表明存在一个FWHM <3”的低表面亮度晕。如果这个晕是NGC6251附近气体的热韧致辐射，那么这种气体就不能通过简单的（静态）气体压力来限制弧分尺度的射电喷流
NGC 6251 has been observed in low-energy X-rays with the Position Sensitive Proportional Counter on board ROSAT. No X-ray emission is seen from the 4.'5 long radio jet of this galaxy, suggesting that the electron spectrum is cut off for electron energies greater than E max ≃10 12 eV, but a bright X-ray source is coincident with the center of the galaxy. Most of the counts in this source are in a component of small angular size, FWHM<4″, corresponding to a linear size less than 3 kpc, although there is evidence for the presence of a low surface brightness halo with FWHM∼3'. If this halo is thermal bremsstrahlung of gas near NGC 6251, this gas cannot confine the arcminute-scale radio jet by simple (static) gas pressure