CHIME/FRB Discovery of Eight New Repeating Fast Radio Burst Sources
CHIME/FRB Discovery of Eight New Repeating Fast Radio Burst Sources
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DOI：
10.3847/2041-8213/ab4a80
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发表时间：
2019-08
期刊：
影响因子：
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通讯作者：
B. Andersen;K. Bandura;M. Bhardwaj;P. Boubel;M. Boyce;P. Boyle;C. Brar;T. Cassanelli;P. Chawla-P
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作者：
B. Andersen;K. Bandura;M. Bhardwaj;P. Boubel;M. Boyce;P. Boyle;C. Brar;T. Cassanelli;P. Chawla-P
我们报道了利用加拿大氢强度测绘实验(CHME)望远镜发现的八个重复的快速射电爆发(FRB)源。这些震源的弥散测量(DM)范围为103.5-1281pC cm−3。它们表现出不同程度的活性：6个震源被检测到两次，另一个被检测到3次，1个被检测到10次。这8个重复的FRB很可能代表了不频繁重复的源分布的明亮和/或高速率端。对于所有源，我们确定天空坐标，不确定度为∼10‘。FRB180916.J0158+65的爆发平均Dm=349.2±0.3rad cm−3，比模拟的银河系极大值低(低至∼20pc cm−3)；这个源的法拉第旋转量(Rm)也是−114.6±0.6rad m−2，远低于FRB 180916.J0158+65测得的Rm。FRB 181030.J1054+73的中继器DM最低，为103.5±0.3pC cm−3，DM超过∼70 pC cm−3。这两个来源都是有趣的多波长跟踪目标，因为它们明显接近。我们的中继器样本的DM分布与前12个尚未重复的CHAME/FRB源的DM分布在统计上无法区分。我们发现，在4σ意义下，中继器爆发一般比未重复的CHAME/FRB爆发宽，这表明不同的发射机制。我们的许多重复事件显示了复杂的形态，这让人想起最初发现的两个重复的FRB。这些源的重复行为将使干涉定位和随后的宿主星系识别成为可能。
We report on the discovery of eight repeating fast radio burst (FRB) sources found using the Canadian Hydrogen Intensity Mapping Experiment (CHIME) telescope. These sources span a dispersion measure (DM) range of 103.5–1281 pc cm−3. They display varying degrees of activity: six sources were detected twice, another three times, and one 10 times. These eight repeating FRBs likely represent the bright and/or high-rate end of a distribution of infrequently repeating sources. For all sources, we determine sky coordinates with uncertainties of ∼10′. FRB 180916.J0158+65 has a burst-averaged DM = 349.2 ± 0.3 pc cm−3 and a low DM excess over the modeled Galactic maximum (as low as ∼20 pc cm−3); this source also has a Faraday rotation measure (RM) of −114.6 ± 0.6 rad m−2, which is much lower than the RM measured for FRB 121102. FRB 181030.J1054+73 has the lowest DM for a repeater, 103.5 ± 0.3 pc cm−3, with a DM excess of ∼70 pc cm−3. Both sources are interesting targets for multi-wavelength follow-up due to their apparent proximity. The DM distribution of our repeater sample is statistically indistinguishable from that of the first 12 CHIME/FRB sources that have not yet repeated. We find, with 4σ significance, that repeater bursts are generally wider than those of CHIME/FRB bursts that have not repeated, suggesting different emission mechanisms. Many of our repeater events show complex morphologies that are reminiscent of the first two discovered repeating FRBs. The repetitive behavior of these sources will enable interferometric localizations and subsequent host galaxy identifications.