SIMBAD references

There is growing evidence that a stable magnetar could be formed from the coalescence of double neutron stars. In previous papers, we investigated the signature of formation of stable millisecond magnetars in radio and optical/ultraviolet bands by assuming that the central rapidly rotating magnetar deposits its rotational energy in the form of a relativistic leptonized wind. We found that the optical transient PTF11agg could be the first evidence for the formation of post-merger millisecond magnetars. To enhance the probability of finding more evidence for the post-merger magnetar formation, it is better to extend the observational channel to other photon energy bands. In this paper, we propose to search the signature of post-merger magnetar formation in X-ray and especially gamma-ray bands. We calculate the synchrotron self-Compton (SSC) emission of the reverse shock powered by post-merger millisecond magnetars. We find that the SSC component peaks at 1 GeV in the spectral energy distribution and extends to \gtrsim 10 TeV for typical parameters. These energy bands are quite suitable for Fermi Large Area Telescope and Cherenkov Telescope Array (CTA), which, with their current observational sensitivities, can detect the SSC emission powered by post-merger magnetars up to 1 Gpc . NuSTAR, which is sensitive in X-ray bands, can detect the formation of post-merger millisecond magnetars at redshift z∼1 . Future improvements in the sensitivity of CTA can also allow us to probe the birth of post-merger millisecond magnetars at redshift z∼1 . However, because of the γ-γ collisions, strong high-energy emission is clearly predicted only for ejecta masses lower than {10}^{-3} {M}_☉ .