negligible initial number density in the early universe and is produced from out of equilibrium decay or scattering of visible sector particles. The production mechanism for non-thermal DM is known as freeze-in and the candidates of non-thermal DM produced via freeze-in are often classified into a group called Freeze-in (Feebly interacting) massive particle (FIMP). For a recent review of this DM paradigm, please see [@Bernal:2017kxu]. The tiny couplings between DM and visible sector can be naturally realised either by higher dimensional operators [@Hall:2009bx; @Elahi:2014fsa; @McDonald:2015ljz] or through some UV complete renormalisable theories [@Biswas:2018aib]. While typical FIMP does not have much direct detection prospects and WIMP direct detection has so far failed, there exists a scenario which is a combination of both and have interesting detection prospects in terms of secondary particles. This is known as super-WIMP scenario [@Feng:2003uy] where a metastable WIMP decays into a super-weakly interacting dark matter at late epochs. Although DM still has feeble interactions with the visible sector, the metastable WIMP has sizeable interactions and can be detected as, for example, long lived BSM particle at collider experiments [@Lee:2018pag]. This scenario was also adopted in the context of neutrino mass models in several works including [@Borah:2017dfn; 