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We compare GW150914 directly to simulations of coalescing binary black holesin full general relativity, accounting for all the spin-weighted quadrupolarmodes, and separately accounting for all the quadrupolar and octopolar modes.Consistent with the posterior distributions reported in LVC_PE[1] (at 90%confidence), we find the data are compatible with a wide range of nonprecessingand precessing simulations. Followup simulations performed usingpreviously-estimated binary parameters most resemble the data. Comparisonsincluding only the quadrupolar modes constrain the total redshifted mass Mz \in[64 - 82M_\odot], mass ratio q = m2/m1 \in [0.6,1], and effective aligned spin\chi_eff \in [-0.3, 0.2], where \chi_{eff} = (S1/m1 + S2/m2) \cdot\hat{L} /M.Including both quadrupolar and octopolar modes, we find the mass ratio is evenmore tightly constrained. Simulations with extreme mass ratios and effectivespins are highly inconsistent with the data, at any mass. Several nonprecessingand precessing simulations with similar mass ratio and \chi_{eff} areconsistent with the data. Though correlated, the components' spins (both inmagnitude and directions) are not significantly constrained by the data. Fornonprecessing binaries, interpolating between simulations, we reconstruct aposterior distribution consistent with previous results. The final black hole'sredshifted mass is consistent with Mf,z between 64.0 - 73.5M_\odot and thefinal black hole's dimensionless spin parameter is consistent with af = 0.62 -0.73. As our approach invokes no intermediate approximations to generalrelativity and can strongly reject binaries whose radiation is inconsistentwith the data, our analysis provides a valuable complement to LVC_PE[1].

Directly comparing GW150914 with numerical solutions of Einstein's equations for binary black hole coalescence