Introduction: Stellar evolution is predominantly governed by the mass of the star. Depending upon the mass, stars take different trajectories from their Main Sequence (MS) period to their death. In our work, we are particularly interested in the MS stars with masses ranging from 140M⊙ to 240M⊙ as they die in the process of Pair Instability Supernova (PISN) leaving no remnant post explosion. Thus, Standard Stellar theory forbids the formation of black holes within the mass range of 60M⊙ to 130M⊙ due to PISN, creating a gap in the black hole mass function. But in 2019, LIGO & Virgo detected a binary black hole merger (GW190521) of two black holes with masses of 85M⊙ and 66M⊙, merging into a single black hole of mass 150M⊙. The observational evidence of GW190521 does not comply with the existing theory. Hence, we propose a new insight for the existence of the black holes in the Pair-Instability mass gap region.

Method: Weakly Interacting Massive Particles (WIMPs) are hypothesized to be Dark Matter (DM) particles which the are thermal relics of the early universe and interact normally only via gravity. Cosmological models suggest the likelihood of first stars being the Massive Population III stars that may have exploded as PISN and Pulsational PISN. As the presence of DM particles were denser at the earlier epochs, it would be more likely for massive stars to accumulate DM particles. The presence of DM, even in a small fraction, admixed with baryonic matter can affect the stellar structure and evolution of the progenitor of PISN. Using the relation between the mass and parameters like temperature, lifetime, and luminosity we have analyzed how DM particles of different mass can affect the progenitor of PISN for different fractions.

Result: Higher the fraction of DM admixture, higher will be the temperature and luminosity in order to maintain the equilibrium. The increased temperature and luminosity will cause the lifetime of the PISN progenitor to drop to around half, even in the presence of relatively small fractions of DM. Even 10% of DM particles with a mass of 50 GeV is sufficient to rise the temperature by a factor of 10. Thereby, allowing the progenitor to escape the PISN stage by overcoming the explosive oxygen phase and collapsing into a black hole. The respective calculations and graphs leading to this conclusion have been mentioned in the paper elaborately.

Summary: We have looked upon the effects of DM in the progenitors of PISN in terms of luminosity, lifetime and temperature and show that with DM admixture, the progenitors can avoid the PISN stage, to collapse into a black hole.