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To date, close to fifty presumed black hole binary mergers were observed bythe LIGO and Virgo detectors. The analyses have been done with an assumptionthat these objects are black holes by limiting the spin prior to the Kerrbound. However, the above assumption is not valid for superspinars, which havethe Kerr geometry but rotate beyond the Kerr bound. In this study, weinvestigate whether and how the limited spin prior range causes a bias inparameter estimation for superspinars if they are detected. To this end, weestimate binary parameters of the simulated inspiral signals of thegravitational waves of compact binaries by assuming that at least one componentof them is a superspinar. We have found that when the primary is a superspinar,both mass and spin parameters are biased in parameter estimation due to thelimited spin prior range. In this case, the extended prior range is stronglyfavored compared to the limited one. On the other hand, when the primary is ablack hole, we do not see much bias in parameter estimation due to the limitedspin prior range, even though the secondary is a superspinar. We also apply theanalysis to black hole binary merger events GW170608 and GW190814, which have along and loud inspiral signal. We do not see any preference of superspinarsfrom the model selection for both events. We conclude that the extension of thespin prior range is necessary for accurate parameter estimation if highlyspinning primary objects are found, while it is difficult to identifysuperspinars if they are only the secondary objects. Nevertheless, the bias inparameter estimation of spin for the limited spin prior range can be a clue ofthe existence of superspinars.

Prospects for estimating parameters from gravitational waves of superspinar binaries