Deep Simultaneous Limits on Optical Emission from FRB 20190520B by 24.4 fps Observations with Tomo-e Gozen
Deep Simultaneous Limits on Optical Emission from FRB 20190520B by 24.4 fps Observations with Tomo-e Gozen
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DOI：
10.3847/1538-4357/ac6be8
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发表时间：
2022-04
期刊：
影响因子：
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通讯作者：
Y. Niino;M. Doi;S. Sako;R. Ohsawa;Noriaki Arima;Jiachen Jiang;N. Tominaga;Masaomi Tanaka;
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文献类型：
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作者：
Y. Niino;M. Doi;S. Sako;R. Ohsawa;Noriaki Arima;Jiachen Jiang;N. Tominaga;Masaomi Tanaka;
我们使用安装在岐阜105厘米施密特望远镜上的高速CMOS相机Tomo - e Gozen，对重复快速射电暴（FRB）20190520B进行了每秒24.4帧的光学观测，同时使用五百米口径球面射电望远镜（FAST）进行射电观测。我们成功地对FAST探测到的11次射电暴进行了同时光学观测。然而，未发现相应的光学辐射。对银河系内尘埃消光进行校正后，得到单个射电暴的光通量极限低至0.068焦耳每毫秒（叠加数据为0.029焦耳每毫秒）。该通量极限比之前对持续时间≳0.1毫秒的光学辐射进行同时观测所得到的结果更低。尽管目前对快速射电暴的射电 - 光学谱能量分布（SED）的限制并不严格，但我们表明，一旦对射电通量≳5焦耳每毫秒的明亮快速射电暴获得与我们观测类似的通量极限，基于光学探测到的脉冲星等射电变源观测到的SED的SED模型，以及理论模型中部分参数空间（其中快速射电暴的光学辐射是由脉冲星磁层中的逆康普顿散射或磁星爆发波撞击热气泡产生的）都可以被排除。
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 ≳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 ≳5 Jy ms.