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On August 14, 2019, the LIGO and Virgo detectors observed GW190814, agravitational-wave signal originating from the merger of a $\simeq 23 M_\odot$black hole with a $\simeq 2.6 M_\odot$ compact object. GW190814'scompact-binary source is atypical both in its highly asymmetric masses and inits lower-mass component lying between the heaviest known neutron star andlightest known black hole in a compact-object binary. If formed throughisolated binary evolution, the mass of the secondary is indicative of its massat birth. We examine the formation of such systems through isolated binaryevolution across a suite of assumptions encapsulating many physicaluncertainties in massive-star binary evolution. We update how mass loss isimplemented for the neutronization process during the collapse of theproto-compact object to eliminate artificial gaps in the mass spectrum at thetransition between neutron stars and black holes. We find it challenging forpopulation modeling to match the empirical rate of GW190814-like systems whilstsimultaneously being consistent with the rates of other compact binarypopulations inferred by gravitational-wave observations. Nonetheless, theformation of GW190814-like systems at any measurable rate requires a supernovaengine model that acts on longer timescales such that the proto-compact objectcan undergo substantial accretion immediately prior to explosion, hinting thatif GW190814 is the result of massive-star binary evolution, the mass gapbetween neutron stars and black holes may be narrower or nonexistent.

Exploring the Lower Mass Gap and Unequal Mass Regime in Compact Binary Evolution