Synchrotron Afterglow Model for AT 2022cmc: Jetted Tidal Disruption Event or Engine-Powered Supernova?

Abstract

AT 2022cmc is a luminous optical transient ($νL_ν \gtrsim 10^{45}$ erg s$^{-1}$) accompanied by decaying non-thermal X-rays (peak duration $t_{\rm X} \lesssim$ days and isotropic energy $E_{\rm X,iso} \gtrsim 10^{53}$ erg) and a long-lived radio/mm synchrotron afterglow, which has been interpreted as a jetted tidal disruption event (TDE). Both an equipartition analysis and a detailed afterglow model reveals the radio/mm emitting plasma to be expanding mildly relativistically (Lorentz factor $Γ\gtrsim\,few$) with an opening angle $θ_{\rm j}\simeq0.1$ and roughly fixed energy $E_{\rm j,iso} \gtrsim few \times 10^{53}$ erg into an external medium of density profile $n \propto R^{-k}$ with $k \simeq 1.5-2$, broadly similar to that of the first jetted TDE candidate Swift J1644+57 and consistent with Bondi accretion at a rate $\sim 10^{-3}\dot{M}_{\rm Edd}$ onto a $10^{6}M_{\odot}$ black hole before the outburst. The rapidly decaying optical emission over the first days is consistent with fast-cooling synchrotron radiation from the same forward shock as the radio/mm emission, while the bluer slowly decaying phase to follow likely represents a separate thermal emission component. Emission from the reverse shock may have peaked during the first days, but whose non-detection in the optical band places an upper bound $Γ_{\rm j} \lesssim 100$ on the Lorentz factor of the unshocked jet. Although a TDE origin for AT 2022cmc is indeed supported by some observations, the vast difference between the short-lived jet activity phase $t_{\rm X} \lesssim$ days relative to the months-long thermal optical emission, also challenges this scenario. A stellar core-collapse event giving birth to a magnetar or black hole engine of peak duration $\sim 1$ day offers an alternative model also consistent with the circumburst environment, if interpreted as a massive-star wind.