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• W3100760028 abstract "A $gamma$-ray transient, Swift J0644.5-5111, has been claimed to be associated with FRB 131104. The $gamma$-ray energy output is estimated as $E_gamma approx 5times 10^{51}$,erg at the nominal $zapprox 0.55$ redshift implied by the dispersion measure of FRB 131104. However, a long-term radio imaging follow-up observations only place an upper limit on the radio afterglow flux of Swift J0644.5-5111. Applying the external shock model, we make a detailed constraint on the afterglow parameters for the FRB 131104/Swift J0644.5-5111 system. We find that for the commonly used microphysics shock parameters (e.g., $epsilon_e=0.1$, $epsilon_B=0.01$ and $p=2.3$), if the redshift value inferred from the DM value is correct to order of magnitude (i.e., $z>0.1$), the ambient medium number density should be $leq 10^{-3}~rm{cm^{-3}}$, which is the typical value for a compact binary merger environment but disfavors a massive star origin. Assuming a typical ISM density, one would require that the redshift of the FRB much smaller than the value inferred from DM value ($zll0.1$), implying a non-cosmological origin of DM. The constraints are much looser if one adopts smaller $epsilon_B$ and $epsilon_e$ values, as observed in some GRB afterglows. The FRB 131104/Swift J0644.5-5111 association remains plausible. We critically discuss possible progenitor models for the system." @default.
• W3100760028 created "2020-11-23" @default.
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• W3100760028 date "2017-01-25" @default.
• W3100760028 modified "2023-09-26" @default.
• W3100760028 title "Implications from the Upper Limit of Radio Afterglow Emission of FRB 131104/Swift J0644.5-5111" @default.
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• W3100760028 doi "https://doi.org/10.3847/2041-8213/835/2/l21" @default.
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