Features and prospects for kilonova remnant detection with current and future surveys

Open Access

Fig. 5.

Detection prospects for KNRs from their temporal evolution information. Top: $\frac{Δ F}{F Δ t}$ $\frac{\Delta F}{F\Delta t}$ for our fiducial cases with Δt = 5 yr. $\frac{dlog F_{3 GHz}}{d t}$ $\frac{\mathrm{dlog}F_{\mathrm{3 GHz}}}{\mathrm{d}t}$ approaches 3/t and ∼1/t in the blast wave and ST regimes, respectively. Bottom: $(\frac{Δ F}{F}) \times (\frac{t_{ST}}{Δ t})$ $(\frac{\Delta F}{F})\times (\frac{t_{\mathrm{ST}}}{\Delta t})$ for the three cases with Δt = 5 yr. We note that t_ST is not available to us directly and has to be extracted from the light-curve data. As $(\frac{Δ F}{F}) \times (\frac{t_{ST}}{Δ t})$ $(\frac{\Delta F}{F})\times (\frac{t_{\mathrm{ST}}}{\Delta t})$ is similar for all cases around the Sedov time, we can estimate t_ST from observed quantities, such as $\frac{Δ F}{F}$ $\frac{\Delta F}{F}$ and Δt (Eq. (37)). As an example, we show the case for an EKNR for which $\frac{Δ F}{F Δ t} \sim 0.02 {yr}^{- 1}$ $\frac{\Delta F}{F\Delta t}\sim 0.02\,\mathrm{yr^{-1}}$ at around the time when it starts to enter deep into the Sedov regime (upper panel).

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