Standard stellar evolution models predict that black holes in the range of approximately 50−140⁢𝑀⊙ should not exist directly from stellar evolution. This gap appears because stars with masses between 100 and 240⁢𝑀⊙ are expected to undergo a pair instability supernova and leave behind no remnant, or a pulsational pair instability supernova and leave behind a remnant much smaller than their initial stellar mass. However, black holes have been discovered by the LIGO/Virgo collaboration within this mass range. In previous work [J. Ziegler and K. Freese, Filling the black hole mass gap: Avoiding pair instability in massive stars through addition of nonnuclear energy, Phys. Rev. D 104, 043015 (2021).], we used the stellar evolution code MESA to show that the addition of non-nuclear energy (such as from annihilation of dark matter) could alter the evolution of a 180⁢𝑀⊙ star so that the observed black holes could be produced from isolated stars. In this paper, we extend this analysis to stars of other masses, and find that sufficient amounts of non-nuclear energy can allow any star to avoid pair instability, and could produce a black hole of mass comparable to the initial stellar mass. In addition, we produce examples of the type of black hole initial mass function that can be produced from this mechanism. These illustrative examples suggest that adding non-nuclear energy to stars offers a way to fully close the mass gap.