Evidence for X-ray Emission in Excess to the Jet Afterglow Decay 3.5 yrs After the Binary Neutron Star Merger GW 170817: A New Emission Component

For the first \(\sim3\) years after the binary neutron star merger event GW 170817 the radio and X-ray radiation has been dominated by emission from a structured relativistic off-axis jet propagating into a low-density medium with n \(< 0.01\,\rm{cm^{-3}}\). We report on observational evidence for an excess of X-ray emission at \(\delta t>900\) days after the merger. With \(L_x\approx5\times 10^{38}\,\rm{erg\,s^{-1}}\) at 1234 days, the recently detected X-ray emission represents a \(\ge 3.2\,\sigma\) (Gaussian equivalent) deviation from the universal post jet-break model that best fits the multi-wavelength afterglow at earlier times. In the context of JetFit afterglow models, current data represent a departure with statistical significance \(\ge 3.1\,\sigma\), depending on the fireball collimation, with the most realistic models showing excesses at the level of \(\ge 3.7\,\sigma\). A lack of detectable 3 GHz radio emission suggests a harder broad-band spectrum than the jet afterglow. These properties are consistent with the emergence of a new emission component such as synchrotron radiation from a mildly relativistic shock generated by the expanding merger ejecta, i.e. a kilonova afterglow. In this context, we present a set of ab-initio numerical-relativity BNS merger simulations that show that an X-ray excess supports the presence of a high-velocity tail in the merger ejecta, and argues against the prompt collapse of the merger remnant into a black hole. Radiation from accretion processes on the compact-object remnant represents a viable alternative. Neither a kilonova afterglow nor accretion-powered emission have been observed before, as detections of BNS mergers at this phase of evolution are unprecedented.