Ruffini, R.R.Ruffini0000-0003-3142-5020Bianco, C. L.C. L.BiancoDella Valle, M.M.Della ValleLi, LiangLiangLiMirtorabi, M. T.M. T.MirtorabiMoradi, R.R.MoradiRastegar Nia, F.F.Rastegar NiaRueda, J. A.J. A.RuedaWang, Y.Y.WangIcranet Team2024-12-092024-12-092024http://hdl.handle.net/20.500.12386/40423The T90 of GRB 240825A is only 4 seconds (GCN 37301), and it is located at a relatively close distance (z=0.659, GCN 37293). The fluence reaches a high level of 10^{-4} erg/cm^2. Through spectral analysis, we find that peak energy Ep is about 400 keV and isotropic energy Eiso is about 2x10^{53} erg, consistent with the Amati relation for long-duration gamma-ray bursts. Comparing its X-ray afterglow (see figure attached below, blue dots), its luminosity falls within the range of other long-duration bursts which are associated with supernovae, higher than those of short-duration bursts which have merge origins. Based on these findings, we conclude that GRB 240825A is a long-duration burst (BdHN I; see, e.g., Bianco, et al., 2024, ApJ, 966, 219) and is associated with a SN. The supernova may reach its optical peak in the observer's rest-frame approximately one month after the trigger. Its peak brightness should be within the detection limits of both ground- and space-based telescopes. Therefore, we encourage further observations in the coming weeks. Figure: https://www.icranet.org/documents/GRB_240825A.pngnewsletter2024GCN.37536....1R