tokens: broadly consistent with the predictions of Fairhurst ( 2011a ). While the inclusion of LIGO-India was not examined in Fairhurst ( 2011a ), we recover a median localization of 9.3 deg 2 for the HIKLV network. 4.3. Comparison with Previous Studies We can compare our result to several studies of advanced network sky localization that have already been performed. We compared our results to those from analytic expectations of Wen Chen ( 2010 ) and Fairhurst ( 2011a ) throughout Sections 4.1 and 4.2 , respectively. The expression used to calculate the expected error regions from Wen Chen ( 2010 ) produces values that are consistent with both Fairhurst ( 2011a ) and our studies. In addition, our study remains broadly consistent with the analytic results of Vitale Zanolin ( 2011 ), recovering similar scalings in localization improvement for successive detector networks for a canonical BNS to our results in Table 2 . Studies such as Singer et al. ( 2014 ) have examined the sky localization capabilities of two- and three-interferometer networks of LIGO and LIGO–Virgo, using more realistic assumptions. In particular, they carried out an end-to-end study of the localizations from the outputs of one compact binary search pipeline used in the first two observing runs (Messick et al. 2017 ). They use a stream of data with colored, but Gaussian, noise and apply a minimum network S/N cut of 12 for each event. Singer et al. ( 2014 ) projected that Virgo would join the LIGO instruments during the second observation run at the sensitivity indicated in Abbott et al. ( 2016b ). They examine a population of BNSs in the HLV configuration, obtaining a median sky localization of 235 deg 2 at the 90% credible level. For our study of NSBH localization, we obtain a median sky localization of 193 deg 2 , seemingly contrary to the expectation that BNS sources are better localized than NSBHs. However, the fiducial networks in our study are have better sensitivities over a given frequency range compared to Singer et al. ( 2014 ), leading to improvements in the effective bandwidth measured by a given instrument. So, our improved localization from that predicted by Singer et al. ( 2014 ) can be attributed to our use of 2018-era instruments as opposed to the less-sensitive 2016 configuration used in Singer et al. ( 2014 ). Rodriguez et al. ( 2014 ) resolve sky localization for a BNS population in which each event realizes a network S/N of 20. On the contrary, our NSBH study samples a wide distribution of network S/Ns, meeting a minimum S/N threshold. 6 6 We require an S/N of at least 5.5 in the second-loudest detector. Therefore, our study probes the S/N regime at which detections are most likely to occur, while Rodriguez et al. ( 2014 ) ignores this low network S/N range. Nevertheless, our Figure 1 is qualitatively comparable to Figures 6 and 7 in Rodriguez et al. ( 2014 ). In particular, the increased isotropy of a three- to four-instrument network and the subsequent,
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