CHANDRA X-RAY OBSERVATIONS OF THE REDSHIFT 1.53 RADIO-LOUD QUASAR 3C 270.1
CHANDRA X-RAY OBSERVATIONS OF THE REDSHIFT 1.53 RADIO-LOUD QUASAR 3C 270.1
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DOI：
10.1088/0004-637x/745/1/84
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发表时间：
2011-09
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通讯作者：
B. Wilkes;D. Lal;D. M. Worrall;M. Birkinshaw;M. Haas;S. Willner;R. Antonucci;M. Ashby;M. Avara;P. Barthel;R. Chini;R. Chini;Giovanni Fazio;M. Hardcastle;C. R. Lawrence;C. Leipski;P. Ogle;B. Schulz
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作者：
B. Wilkes;D. Lal;D. M. Worrall;M. Birkinshaw;M. Haas;S. Willner;R. Antonucci;M. Ashby;M. Avara;P. Barthel;R. Chini;R. Chini;Giovanni Fazio;M. Hardcastle;C. R. Lawrence;C. Leipski;P. Ogle;B. Schulz
2008年2月，钱德拉X射线对高红移（z = 1.532）射电噪类星体3C 270.1的观测显示，其核有一个幂律谱，r = 1.66 ± 0.08，是典型的射电噪类星体，以及一条微弱的Fe Kα发射线。这些数据还揭示了扩展的X射线发射，其中大约一半与该源的无线电发射有关。南方发射与射电瓣同空间，峰值位于双射电热点的位置。模拟这个热点，包括斯皮策上限，排除了来自单个幂律电子群体的同步辐射，有利于逆康普顿辐射，其场为1011 nT，大约是均分值的三分之一。北方发射集中在40°弯曲的位置附近，假设射电喷流遇到外部介质。它可以用涉及场为1.3nT的宇宙微波背景光子的逆康普顿发射来解释，场为1.3nT，比均分值低7-10倍。剩下的，更弥散的X射线发射更硬（HR = −0.09 ± 0.22）。由于只有22.8 ± 5.6个计数，谱形式不能被约束。假设热辐射的温度为4 keV，得到的光度估计为1.8× 1044 erg s−1，与低红移星系团的光度-温度关系一致。然而，需要更深入的钱德拉X射线观测来描绘空间分布，并更好地限制漫发射的光谱，以验证我们已经检测到来自高红移星系团的X射线发射。
Chandra X-ray observations of the high redshift (z = 1.532) radio-loud quasar 3C 270.1 in 2008 February show the nucleus to have a power-law spectrum, Γ = 1.66 ± 0.08, typical of a radio-loud quasar, and a marginally detected Fe Kα emission line. The data also reveal extended X-ray emission, about half of which is associated with the radio emission from this source. The southern emission is co-spatial with the radio lobe and peaks at the position of the double radio hot spot. Modeling this hot spot, including Spitzer upper limits, rules out synchrotron emission from a single power-law population of electrons, favoring inverse Compton emission with a field of ∼11 nT, roughly a third of the equipartition value. The northern emission is concentrated close to the location of a 40° bend where the radio jet is presumed to encounter an external medium. It can be explained by inverse Compton emission involving cosmic microwave background photons with a field of ∼3 nT, a factor of 7–10 below the equipartition value. The remaining, more diffuse X-ray emission is harder (HR = −0.09 ± 0.22). With only 22.8 ± 5.6 counts, the spectral form cannot be constrained. Assuming thermal emission with a temperature of 4 keV yields an estimate for the luminosity of 1.8× 1044 erg s−1, consistent with the luminosity–temperature relation of lower-redshift clusters. However, deeper Chandra X-ray observations are required to delineate the spatial distribution and better constrain the spectrum of the diffuse emission to verify that we have detected X-ray emission from a high-redshift cluster.