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GRB 111005A, one long duration gamma-ray burst (GRB) occurred within ametal-rich environment that lacks massive stars with $M_{\rm ZAMS}\geq15M_\odot$, is not coincident with supernova emission down to stringent limitand thus should be classified as a "long-short" GRB (lsGRB; also known asSN-less long GRB or hybrid GRB), like GRB 060505 and GRB 060614. In this workwe show that in the neutron star merger model, the non-detection of theoptical/infrared emission of GRB 111005A requires a sub-relativisticneutron-rich ejecta with the mass of $\leq 0.01~M_\odot$, (significantly) lessmassive than that of GRB 130603B, GRB 060614 and GRB 050709. The lsGRBs arefound to have a high rate density and the neutron star merger origin model canbe unambiguously tested by the joint observations of the second generationgravitational wave (GW) detectors and the full-sky gamma-ray monitors such asFermi-GBM and the proposing GECAM. If no lsGRB/GW association is observed in2020s, alternative scenarios have to be systematically investigated. With thedetailed environmental information achievable for the very-nearby events, anovel kind of merger or explosion origin may be identified.

GRB 111005A at Z = 0.0133 and the Prospect of Establishing Long-short GRB/GW Association