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The detection of GW170817 in gravitational waves provides unprecedentedconstraints on the equation of state (EOS) of the ultra-dense matter within thecores of neutron stars (NSs). We extend the nonparametric analysis firstintroduced in Landry & Essick (2019), and confirm that GW170817 favors softEOSs. We infer macroscopic observables for a canonical 1.4 $M_{\odot}$ NS,including the tidal deformability $\Lambda_{1.4} = 211^{+312}_{-137}$($491^{+216}_{-181}$) and radius $R_{1.4}= 10.86^{+2.04}_{-1.42}$($12.51^{+1.00}_{-0.88}$) km, as well as the maximum mass for nonrotating NSs,$M_{max} = 2.064^{+0.260}_{-1.34}$ ($2.017^{0.238}_{-0.087}$) $M_\odot$, withnonparametric priors loosely (tightly) constrained to resemble candidate EOSsfrom the literature. Furthermore, we find weak evidence that GW170817 involvedat least one NS based on gravitational-wave data alone ($B^{NS}_{BBH}= 3.3 \pm1.4$), consistent with the observation of electromagnetic counterparts. We alsoinvestigate GW170817's implications for the maximum spin frequency ofmillisecond pulsars, and find that the fastest known pulsar is spinning at morethan 50% of its breakup frequency at 90% confidence. We additionally findmodest evidence in favor of quark matter within NSs, and GW170817 favors thepresence of at least one disconnected hybrid star branch in the mass--radiusrelation over a single stable branch by a factor of 2. Assuming there aremultiple stable branches, we find a suggestive posterior preference for a sharpsoftening around nuclear density followed by stiffening around twice nucleardensity, consistent with a strong first-order phase transition. While thestatistical evidence in favor of new physics within NS cores remains tenuouswith GW170817 alone, these tantalizing hints reemphasize the promise ofgravitational waves for constraining the supranuclear EOS.

Nonparametric Inference of Neutron Star Composition, Equation of State, and Maximum Mass with GW170817