Liang Li, Yu Wang, Bing Zhang, Ye Li, Shu-Rui Zhang, Jochen Greiner, Zhi-Ping Jin, Jin-Jun Geng, Hou-Jun Lv, Asaf Peer, Maria Dainotti, Tong Liu, Yi-Zhong Fan, Yong-Feng Huang, Zi-Gao Dai, Melin Kole, Wei-Hua Lei, Ye-Fei Yuan, Shuang-Nan Zhang, Felix Ryde, She-Sheng Xue, Rong-Gen Cai

Gamma-ray bursts (GRBs), among the most energetic transients in the Universe, are traditionally classified into long-duration GRBs (lasting more than two seconds) and short-duration GRBs (lasting less than two seconds)\cite{Kouveliotou1993}. Long-duration GRBs are typically associated with the core collapse of massive stars (Type II), whereas short-duration GRBs originate from the merger of compact binary systems (Type I)\cite{Woosley2006, Zhang2006Natur, Zhang2009b, Berger2014}. Owing to their distinct physical origins, the two classes exhibit markedly different observational properties, which serve as key diagnostic criteria for GRB classification\cite{Norris2000, Zhang2009b, Lv2010, Lv2014, Qin2013, Li2016, Minaev2020}. Here we report a peculiar gamma-ray burst, GRB 160425A, comprising a short-sharp duration burst ($G_1$) followed by a long-broad duration burst ($G_2$), separated by only four minutes. Strikingly, nearly all standard prompt-emission observational diagnostics, including pulse morphology\cite{Norris2005}, duration\cite{Kouveliotou1993}, hardness ratio \cite{Horvath2010, Goldstein2017}, minimum variability timescale\cite{Golkhou2014, Golkhou2015}, spectral properties \cite{Dezalay1992}, spectral lag\cite{Norris2000,Norris2006, Yi2006, Bernardini2015}, and established empirical correlations (the Amati and Norris relations \cite{Amati2002, Norris2000}), consistently categorize $G_1$ as a short-like (Type-I, merger-origin) GRB and $G_2$ as a long-like (Type-II, collapsar-origin) GRB. The coexistence of merger and collapsar signatures within a single event challenges existing progenitor frameworks, calling for a fundamental re-evaluation of GRB classification schemes and progenitor scenarios.