Periastron Observations of TeV Gamma-Ray Emission from a Binary System with a 50-year Period
Periastron Observations of TeV Gamma-Ray Emission from a Binary System with a 50-year Period
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DOI：
10.3847/2041-8213/aae70e
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发表时间：
2018-10
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通讯作者：
T. V. C. A. U. Abeysekara;W. Benbow;R. Bird;A. Brill;R. Brose;J. Buckley;A. Chromey;M. Daniel
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文献类型：
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作者：
T. V. C. A. U. Abeysekara;W. Benbow;R. Bird;A. Brill;R. Brose;J. Buckley;A. Chromey;M. Daniel
我们报告的观测脉冲星/Be星星二进制系统PSR J2032+4127/MT 91 213之间的能量范围内，并与甚高能辐射成像望远镜阵列和主要大气伽玛成像切伦科夫望远镜阵列。双星轨道的周期约为50年，最近的近星点发生在2017年11月13日。我们的观测跨度从近星点前的18个月到近星点后的一个月。在PSR J2032+4127/MT 91213的位置上探测到一个新的点状γ射线源。伽玛射线光变曲线和光谱的特点，以及在近星点通过。的通量是可变的，至少在一个数量级，峰值在近星点，从而提供了一个坚实的联系TeV源与脉冲星/Be星星系统。在近星点之前的观测表明，在能量大约为1000的时候，光谱会有一个截止。这一结果增加了一个新的成员，已知的TeV二进制的小人口，它确定了只有第二个来源的这个类中的性质和性质的紧凑对象是牢固确立的。我们比较伽马射线的结果与光变曲线测量的X射线望远镜上的尼尔Gehrels斯威夫特天文台和最近的理论模型的预测系统。我们的结论是，需要显着修订的模型，以解释我们所观察到的排放的细节，我们讨论的二元系统和重叠的稳定扩展源，TeV J2032+4130之间的关系。
We report on observations of the pulsar/Be star binary system PSR J2032+4127/MT91 213 in the energy range between and with the Very Energetic Radiation Imaging Telescope Array and Major Atmospheric Gamma Imaging Cherenkov telescope arrays. The binary orbit has a period of approximately 50 years, with the most recent periastron occurring on 2017 November 13. Our observations span from 18 months prior to periastron to one month after. A new point-like gamma-ray source is detected, coincident with the location of PSR J2032+4127/MT91 213. The gamma-ray light curve and spectrum are well characterized over the periastron passage. The flux is variable over at least an order of magnitude, peaking at periastron, thus providing a firm association of the TeV source with the pulsar/Be star system. Observations prior to periastron show a cutoff in the spectrum at an energy around . This result adds a new member to the small population of known TeV binaries, and it identifies only the second source of this class in which the nature and properties of the compact object are firmly established. We compare the gamma-ray results with the light curve measured with the X-ray Telescope on board the Neil Gehrels Swift Observatory and with the predictions of recent theoretical models of the system. We conclude that significant revision of the models is required to explain the details of the emission that we have observed, and we discuss the relationship between the binary system and the overlapping steady extended source, TeV J2032+4130.