FRB Energetics and detectability from high redshifts

Bing Zhang

doi:10.3847/2041-8213/aae8e3

paper

FRB Energetics and detectability from high redshifts

arXiv:1808.05277 · doi:10.3847/2041-8213/aae8e3

Abstract

We estimate the upper limit redshifts of known FRBs using the dispersion measure (DM) - redshift ( $z$ ) relation and derive the upper limit peak luminosity $L_{p}$ and energy $E$ of FRBs within the observational band. The average $z$ upper limits range from 0.17 to 3.10, the average $L_{p}$ upper limits range from $1.24 \times 1 0^{42} erg s^{- 1}$ to $7.80 \times 1 0^{44} erg s^{- 1}$ , and the average $E$ upper limits range from $6.91 \times 1 0^{39}$ erg to $1.94 \times 1 0^{42}$ erg. FRB 160102 with DM $= 2596.1 \pm 0.3 pc c m^{- 3}$ likely has a redshift greater than 3. Assuming that its intrinsic DM contribution from the host and FRB source is $D M_{host} + D M_{scr} \sim 100 pc c m^{- 3}$ , such an FRB can be detected up to $z \sim 3.6$ by Parkes and by FAST under ideal conditions up to $z \sim 10.4$ . Assuming that there exist FRBs detectable at $z \sim 15$ by sensitive telescopes such as FAST, the upper limit DM for FRB searches may be set to $\sim 9000 pc c m^{- 3}$ . For single-dish telescopes, those with a larger aperture tend to detect more FRBs than those with a smaller aperture if the FRB luminosity function index $α_{L}$ is steeper than 2, and vice versa. In any case, large-aperture telescopes such as FAST are more capable of detecting high- $z$ FRBs, even though most of FRBs detected by them are still from relatively low redshifts.

8 pages, ApJL, in press

FRB Energetics and detectability from high redshifts

Abstract

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