论文标题
FRB 20180916b的60 pc环境
The 60 pc Environment of FRB 20180916B
论文作者
论文摘要
在其主机Galaxy SDSS J015800.28+654253.0中，快速无线电爆发FRB 20180916b以149 MPC为止是迄今为止最接近的FRB，拥有强大的主机银河系协会。该消息来源还表现出16.35天的爆发。在这里，我们在哈勃太空望远镜上使用WFC3摄像头介绍了FRB 20180916b的光学和红外成像以及FRB 20180916b的整体田间光谱观测值，以及10.4 m Gran Telescopio Canarias上的Megara光谱仪。 Hubble成像的60-90 MILLIARCSECOND（MAS）分辨率，以及先前的FRB 20180916b的2.3-MAS定位，使我们能够以30-60 PC的分辨率探测其环境。我们将FRB 20180916B位置的任何类似点的星形形态或HII区域限制为具有H $α$亮度$ L_ \ MATHRM {Hα} \ Lessim 10^{37} \，\ Mathrm {erg {erg {erg {erg {erg，s^{ - 1}} $，并相应地限制了，以相应地约束，以相应地限制$ \ sillssim10^{ - 4} \，\ mathrm {m_ \ odot \，yr^{ - 1}} $。对H $α$的限制表明，与O6V相比，FRB 20180916b的恒星伴侣应具有较酷，较大的光谱类型。 FRB 20180916b距离最近的年轻恒星团的最明亮像素（预计距离为250 pc），即$ \ sim380 $ \，大小（全宽度为一半）。由于二进制文件（60-750 km s $^{ - 1} $）的脉冲星，磁铁或中子星的典型速度，FRB 20180916b将需要800 kyr到7 Myr，以横穿观察到的距离距离其假定出生地的距离。这个时间尺度与磁铁的活跃年龄（$ \ lyssim10 $ kyr）不一致。相反，推断的年龄和观察到的分离与高质量X射线二进制和伽马射线二进制的年龄以及它们与最近的OB关联的分离。
Fast Radio Burst FRB 20180916B in its host galaxy SDSS J015800.28+654253.0 at 149 Mpc is by far the closest-known FRB with a robust host galaxy association. The source also exhibits a 16.35-day period in its bursting. Here we present optical and infrared imaging as well as integral field spectroscopy observations of FRB 20180916B with the WFC3 camera on the Hubble Space Telescope and the MEGARA spectrograph on the 10.4-m Gran Telescopio Canarias. The 60-90 milliarcsecond (mas) resolution of the Hubble imaging, along with the previous 2.3-mas localization of FRB 20180916B, allow us to probe its environment with a 30-60 pc resolution. We constrain any point-like star-formation or HII region at the location of FRB 20180916B to have an H$α$ luminosity $L_\mathrm{Hα} \lesssim 10^{37}\,\mathrm{erg\,s^{-1}}$ and, correspondingly, constrain the local star-formation rate to be $\lesssim10^{-4}\,\mathrm{M_\odot\,yr^{-1}}$. The constraint on H$α$ suggests that possible stellar companions to FRB 20180916B should be of a cooler, less massive spectral type than O6V. FRB 20180916B is 250 pc away (in projected distance) from the brightest pixel of the nearest young stellar clump, which is $\sim380$\,pc in size (full-width at half maximum). With the typical projected velocities of pulsars, magnetars, or neutron stars in binaries (60-750 km s$^{-1}$), FRB 20180916B would need 800 kyr to 7 Myr to traverse the observed distance from its presumed birth site. This timescale is inconsistent with the active ages of magnetars ($\lesssim10$ kyr). Rather, the inferred age and observed separation are compatible with the ages of high-mass X-ray binaries and gamma-ray binaries, and their separations from the nearest OB associations.
