The nature of the compact objects within the supposed “lower mass gap” remains uncertain. Observations of GW190814 and GW230529 highlight the challenges gravitational waves face in distinguishing neutron stars from black holes. Interpreting these systems is especially difficult because classifications depend simultaneously on measurement noise, compact binary population models, and equation of state (EOS) constraints on the maximum neutron star mass. We analyze 66 confident events from the third Gravitational-Wave Transient Catalog to quantify how the probability of a component being a neutron star, $P(\mathrm{NS})$, varies across the population. The effects are substantial; the dominant drivers of classification are the pairing preferences of neutron stars with other compact objects and the neutron star spin distributions. The data reveals that $P(\mathrm{NS})$ varies between 1%–67% for GW230529’s primary and between 51%–100% for GW190425’s primary. By contrast, $P(\mathrm{NS})$ for GW190814’s secondary varies by $\le 10\%$, demonstrating robustness from its high signal-to-noise ratio and small mass ratio. Analysis using EOS information tends to affect $P(\mathrm{NS})$ through the inferred maximum neutron star mass rather than the maximum spin. As it stands, $P(\mathrm{NS})$ remains sensitive to numerous population parameters, limiting its reliability and potentially leading to ambiguous classifications of future gravitational wave events.

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• Gravitational wave detection
• Gravitational wave sources
• Gravitational waves
• Neutron stars & pulsars