  Understanding astrophysical phenomena involving compact objects requires an
insight about the engine behind core-collapse supernovae (SNe) and the fate of
the stellar collapse of massive stars. In particular, this insight is crucial
in developing an understanding of the origin and formation channels of detected
population of BH-BH, BH-NS and NS-NS mergers. To gain this understanding, we
must tie our current knowledge of pre-SN stars properties and their potential
explosions to the final NS or BH mass distribution. The timescale of convection
growth may have a large effect on the strength of SN explosion and therefore
also on the mass distribution of stellar remnants. In this study we adopt the
new formulas for the relation between the pre-SN star properties and its
remnant from Fryer et al. 2022 into StarTrack population synthesis code and
check how they impact double compact object (DCO) mergers formed via isolated
binary evolution. The new formulas give one ability to test a wide spectrum of
assumptions on the convection growth time. In particular, different variants
allow for a smooth transition between having a deep lower mass gap and a
remnant mass distribution filled by massive NSs and low mass BHs. In this paper
we present distribution of masses, mass ratios and the local merger rate
densities of DCO mergers for different variants of new remnant mass formulas.
We test them together with different approaches to other highly uncertain
processes. We find that mass distribution of DCO mergers up to m_1+m_2 < 35
Msun is sensitive to adopted assumption on SN convection growth timescale.
Between the two extreme tested variants the probability of compact object
formation within the lower mass gap may differ up to 2 orders of magnitude. The
mass ratio distribution of DCO mergers is significantly influenced by SN model
only for our standard mass transfer stability criteria.
