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We perform an exhaustive follow-up analysis of a subsolar-mass (SSM)gravitational wave (GW) candidate reported by Phukon et al. from the secondobserving run of Advanced LIGO. This candidate has a reported signal-to-noiseratio (SNR) of $8.6$ and false alarm rate of $0.41$ yr which are too low toclaim a clear gravitational-wave origin. When improving on the search by usingmore accurate waveforms, extending the frequency range from 45 Hz down to 20Hz, and removing a prominent blip glitch, we find that the posteriordistribution of the network SNR lies mostly below the search value, with the$90\%$ confidence interval being $7.94^{+0.70}_{-1.05}$. Assuming that theorigin of the signal is a compact binary coalescence (CBC), the secondarycomponent is $m_2 = \text{$0.76^{+0.50}_{-0.14}$} M_\odot$, with $m_2 < 1M_\odot$ at $84\%$ confidence level, suggesting an unexpectedly light neutronstar or a black hole of primordial or exotic origin. The primary mass would be$m_1 = \text{$4.71^{+1.57}_{-2.18}$} M_\odot$, likely in the hypothesized lowermass gap and the luminosity distance is measured to be $D_{\rmL}=124^{+82}_{-48}$Mpc. We then probe the CBC origin hypothesis by performingthe signal coherence tests, obtaining a log Bayes factor of $4.96 \pm 0.13$ forthe coherent vs. incoherent hypothesis. We demonstrate the capability ofperforming a parameter estimation follow-up on real data for an SSM candidatewith moderate SNR. The improved sensitivity of O4 and subsequentLIGO-Virgo-KAGRA observing runs could make it possible to observe similarsignals, if present, with a higher SNR and a more precise measurement of theparameters of the binary.

Analysis of a subsolar-mass compact binary candidate from the second observing run of Advanced LIGO