论文标题
使用HAWC伽马射线观测站对TEV光子能量的活动星系的调查
A survey of active galaxies at TeV photon energies with the HAWC gamma-ray observatory
论文作者
论文摘要
高空水Cherenkov伽马射线天文台（HAWC）连续检测到其大型视野内的TEV光子和颗粒，每天积累了更深层次的三分之二天空。我们分析了1523年的HAWC实时数据在四年半的时间内获取了{\ em fermi} 3fhl目录在Sierra Negra的Zenith $ 40^\ yegra的$ 40^\ circs of the sierra negra的{\ em fermi} 3 fermi} calmminog的后续分析（$ z <0.3 $）（$ z <0.3 $）。对持续的TEV发射的搜索使用了最大样品分析，假设固有的幂律光谱通过对伽马射线光子的成对产生与静脉外背景光的伽马射线光谱减弱。 HAWC清楚地检测到MKN〜421和MKN〜501的持续发射，TEV Sky中的两个最亮的盛宴分别为65 $σ$和17 $σ$级别。 {对于其他三个已知的高能量发射器的长期发射证据较弱：}放射性M87和Bl lac对象VER〜J0521+211和1ES〜1215+303，后来的两个，$ z \ sim \ sim 0.1 $。我们从先前报道的非常高能来源的集合中找到了集体排放的证据，这些资源不包括MKN〜421和MKN〜501，并具有随机概率$ \ sim 10^{ - 5} $。在幂律假设和预定义的（0.5-2.0），（2.0-8.0）和（8.0-32.0）TEV能量间隔下，对样品进行了上限。
The High Altitude Water Cherenkov Gamma-Ray Observatory (HAWC) continuously detects TeV photons and particles within its large field-of-view, accumulating every day a deeper exposure of two thirds of the sky. We analyzed 1523~days of HAWC live data acquired over four and a half years, in a follow-up analysis of {138} nearby ($z<0.3$) active galactic nuclei from the {\em Fermi} 3FHL catalog culminating within $40^\circ$ of the zenith at Sierra Negra, the HAWC site. This search for persistent TeV emission used a maximum-likelihood analysis assuming intrinsic power-law spectra attenuated by pair production of gamma-ray photons with the extragalactic background light. HAWC clearly detects persistent emission from Mkn~421 and Mkn~501, the two brightest blazars in the TeV sky, at 65$σ$ and 17$σ$ level, respectively. {Weaker evidence for long-term emission is found for three other known very-high energy emitters:} the radiogalaxy M87 and the BL Lac objects VER~J0521+211 and 1ES~1215+303, the later two at $z\sim 0.1$. We find evidence for collective emission from the set of 30 previously reported very high-energy sources that excludes Mkn~421 and Mkn~501 with a random probability $\sim 10^{-5}$. Upper limits are presented for the sample under the power-law assumption and in the predefined (0.5-2.0), (2.0-8.0) and (8.0-32.0) TeV energy intervals.
