where P pr ( EOS ) represents the set of the priors on the EOS , which we describe above . Because of the high accuracy in the measurement of the chirp mass , we fix it to the observed value , and use that to set m 2 for any given m 1 . Then , equation ( 13 ) can be written as   ( 9 ) . We find excellent agreement between our Λ − R prediction and the full Bayesian inference . Middle : Same as left panel , but showing , in addition , the marginalized posteriors over the neutron star radii for a fixed grid of masses . These marginalized likelihoods are shown in blue . By marginalizing the posteriors in this way , the results are skewed to higher radii and away from the maximum likelihood solution . Right : Marginalized likelihoods for an inference with only the priors and no data . These marginalized posteriors are nearly identical to the marginalized posteriors from the inference that incorporated data from a Λ = 400 centered Gaussian . This method of marginalization over - weights the prior on the EOS pressures imposed by the observation of a 1.97 M neutron star . The results of the marginalization are less sensitive to the input data and are not reliable .