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In 2018, we reported our discovery of a dozen quiescent X-ray binaries in thecentral parsec (pc) of the Galaxy (Hailey et al. 2018). In a recent follow-uppaper (Mori et al. 2021), we published an extended analysis of these sourcesand other X-ray binaries (XRBs) in the central pc and beyond, showing that mostif not all of the 12 non-thermal sources are likely black hole low-mass X-raybinary (BH-LMXB) candidates. In response, Maccarone et al. 2022 (TM22hereafter) argued, primarily on the claim that neutron star low-mass X-raybinaries (NS-LMXBs) often do not have short outburst recurrence times (<~ 10yr), that they cannot be excluded as a designation for the 12 quiescent X-raybinary sources. TM22 cites three main factors in their study: (1) X-rayoutburst data of NS transients detected by RXTE and MAXI, (2) the Galacticpopulation of NS-LMXBs, and (3) (persistently) quiescent NS-LMXBs in globularclusters. We address these arguments of TM22 and correct theirmisunderstandings of our work and the literature, even though most of thesepoints have already been thoroughly addressed by Mori et al. 2021. We alsocorrect TM22's assertion that our arguments are based solely on NS transients'recurrence times.

Comment on "On the recurrence times of neutron star X-ray binary transients and the nature of the Galactic Center quiescent X-ray binaries"