RADIO VARIABILITY OF A FERMI LARGE AREA TELESCOPE BRIGHT SOURCE 0FGL J1847.8+3223
RADIO VARIABILITY OF A FERMI LARGE AREA TELESCOPE BRIGHT SOURCE 0FGL J1847.8+3223
复制标题
费米大面积望远镜亮源0FGL J1847.8 3223的射电变率
DOI：
10.1088/2041-8205/714/1/l36
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发表时间：
2010
期刊：
影响因子：
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通讯作者：
N. Matsumura
中科院分区：
文献类型：
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作者：
S. Kida;T. Daishido;T. Tanaka;T. Aoki;K. Tekefuji;K. Niinuma;K. Asuma;S. Nakagawa;H. Uehara;H. Akamatsu;A. Imai;H. Miyata;J. Ikouga;A. Otsubo;K. Odai;R. Kodama;Y. Takanashi;N. Nakamizo;Y. Yamada;R. Hiruma;N. Furukawa;N. Matsumura
在费米大面望远镜 (LAT) 亮源 0FGL J1847.8+3223 (B2 1846+32A) 所在区域的中心区域检测到 1.42 GHz 的射电变异性。使用早稻田那须天文台的二元干涉仪装置检测通量； 2004年的通量至少为1200 mJy，2005年的通量至少为1600 mJy。格林班克300望远镜观测到的B2 1846+32A的通量在1980年代为532 mJy，而通过甚大阵列观测到的1990年代为516 mJy。因此，从 20 世纪 90 年代中期到 2000 年代中期，1.4 GHz 频段的通量增加了两倍。 20世纪80年代和1990年代，对B2 1846+32A进行了几次观测；然而，没有检测到通量的变化。 2008年，LAT从B2 1846+32A探测到了8.800e-08光子(100 MeV–1 GeV) cm−2 s−1和6.400e-09光子(1 GeV–100 GeV) cm−2 s−1伽马射线。 1991 年至 2000 年，EGRET 尚未从该源探测到伽马射线。伽马射线通量在大约 10 年内至少增强了两倍。 EGRET 围绕该源的上限约为 4.9e-08 光子(>100 MeV) cm−2 s−1。无线电和伽马射线测量表明，B2 1846+32A 的通量在 2000 年代增强。这些结果表明无线电辐射和伽马射线发射之间存在很强的相关性。在这封信中，我们介绍了包括 B2 1846+32A 在内的区域中强条纹的分析结果。
Radio variability was detected at 1.42 GHz from an area at the center of which a Fermi Large Area Telescope (LAT) bright source 0FGL J1847.8+3223 (B2 1846+32A) was located. The flux was detected using a two-element interferometer setup at the Waseda Nasu Observatory; the flux was at least 1200 mJy in 2004 and at least 1600 mJy in 2005. The flux of B2 1846+32A was 532 mJy in the 1980s, as observed by the Greenbank 300 telescope, and 516 mJy in the 1990s, as observed by the Very Large Array. Thus, the flux tripled from the mid-1990s to the mid-2000s in the 1.4 GHz band. In the 1980s and 1990s, a few observations of B2 1846+32A were carried out; however, variability in flux was not detected. In 2008, 8.800e-08 photon(100 MeV–1 GeV) cm−2 s−1 and 6.400e-09 photon(1 GeV–100 GeV) cm−2 s−1 gamma rays were detected from B2 1846+32A by the LAT. Gamma rays had not been detected from this source by EGRET in 1991–2000. The gamma-ray flux strengthened at least twice in about 10 years. The upper limit around this source by EGRET is approximately 4.9e-08 photon(>100 MeV) cm−2 s−1. The flux of B2 1846+32A strengthened in the 2000s, as indicated by both radio and gamma-ray measurements. These results suggest that there exists a strong correlation between the radio radiation and the gamma-ray emission. In this Letter, we present the analytical results of a strong fringe in the area including B2 1846+32A.