论文标题
从FRB 20190520b乘出24.4 fps观测的高度同时限制了tomo-e gozen的24.4 fps观测
Deep simultaneous limits on optical emission from FRB 20190520B by 24.4 fps observations with Tomo-e Gozen
论文作者
论文摘要
我们使用Tomo-e Gozen进行了24.4〜FPS的光学观察（FRB）20190520b，使用Tomo-e Gozen，这是一种高速CMOS摄像机，安装在KISO 105-CM Schmidt Telescope上，同时使用五架hundred Metrenred Meter perture sphericer spherical Xpheric poaderialic xbererial Xpherial spherial Xberical Prioader telescope（快速）进行了无线电观察。我们在快速检测到的11次无线电爆发的同时光学观察中取得了成功。但是，未发现相应的光学发射。对于在银河系中校正了尘埃灭绝的单个爆发（堆叠数据上的0.029 JY MS），获得了高达0.068 JY MS的光通量极限。与以前的同时观察值获得的光发射持续时间为$ \ gtrsim 0.1 $ ms的光发射限制更深。 Although the current limits on radio--optical spectral energy distribution (SED) of FRBs are not constraining, we show that SED models based on observed SEDs of radio variable objects such as optically detected pulsars, and a part of parameter spaces of theoretical models in which FRB optical emission is produced by inverse-Compton scattering in a pulsar magnetosphere or a strike of a magnetar blastwave into a hot wind bubble, can be ruled out once与我们的观察值一样，对于带有无线电通量$ \ gtrsim 5 $ jy ms的明亮FRB的观察值类似。
We conduct 24.4~fps optical observations of repeating Fast Radio Burst (FRB) 20190520B using Tomo-e Gozen, a high-speed CMOS camera mounted on the Kiso 105-cm Schmidt telescope, simultaneously with radio observations carried out using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). We succeeded in the simultaneous optical observations of 11 radio bursts that FAST detected. However, no corresponding optical emission was found. The optical fluence limits as deep as 0.068 Jy ms are obtained for the individual bursts (0.029 Jy ms on the stacked data) corrected for the dust extinction in the Milky Way. The fluence limit is deeper than those obtained in the previous simultaneous observations for an optical emission with a duration $\gtrsim 0.1$ ms. Although the current limits on radio--optical spectral energy distribution (SED) of FRBs are not constraining, we show that SED models based on observed SEDs of radio variable objects such as optically detected pulsars, and a part of parameter spaces of theoretical models in which FRB optical emission is produced by inverse-Compton scattering in a pulsar magnetosphere or a strike of a magnetar blastwave into a hot wind bubble, can be ruled out once a similar fluence limit as in our observation is obtained for a bright FRB with a radio fluence $\gtrsim 5$ Jy ms.
