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In this paper we apply to gravitational waves from non-spinning binarysystems a recently intro- duced frequentist methodology to calculateanalytically the error for a maximum likelihood estimate (MLE) of physicalparameters. While existing literature focuses on using the Cramer Rao Lowerbound (CRLB) and Monte Carlo simulations, we use a power expansion of the biasand covariance in inverse powers of the signal to noise ratio. The use ofhigher order derivatives of the likelihood function in the expansions makes theprediction also sensitive to the secondary lobes of the MLE probabilitydistribution. We discuss conditions for validity of the CRLB and predict newfeatures in regions of the parameter space currently not explored. For example,we see how the bias can become the most important contributor to theparameters' errors for high mass systems (200M and above).

Parameter estimation from Gravitational waves generated by non-spinning binary black holes with laser interferometers: beyond the Fisher information