the additional errors arise by studying the consequences of eqn. (\[m1\]).

The Newtonian Waveform {#MCres}
======================

Monte Carlo Simulations {#MCres1}
-----------------------

In this section we shall restrict ourselves to the Newtonian waveform. We have the four parameters: $$\bbox{\mu} \equiv \mu^a \equiv \{\mu^0,\mu^1,\mu^2,\mu^3\} \equiv 
\{A, 2\pi f_st_s, \Phi, 2\pi
f_s\tau_0\}.$$ Simulations were carried out for a test case of $\check\tau_0 = 5.558$ s This corresponds to a binary comprised of a $10M_\odot$ black hole and a $1.4M_\odot$ neutron star. The waveform was cutoff at a frequency of $800$ Hz and the data train was sampled at $2000$Hz. As mentioned before the power spectral density was chosen to be consistent with the initial LIGO interferometer. The range of $\tau_0$ for the filters was $[5.358,5.758]$ with a spacing of $1$ msec. The simulations presented here were carried out for an SNR of $10$, [*i.e.*]{}, $\check A = 10$. We considered $12000$ realizations of noise.

The covariance matrix for the Newtonian case is given below: $$\label{cov1}
{\bf C}_{(\bbox{\mu})}\equiv 
\left[C^{ab}_{(\bbox{\mu})}\right] = \frac{1}{{\check A}^2}\left(\begin{tabular}{cccc}
${\check  A}^2$&0.0&0.0&0.0\\
0.0\ \ &222.50&322.26&-227.25\\
0.0&322.26&469.16&-328.65\\
0.0&-227.25&-328.65&232.26\\
\end{tabular}\right)$$ In the above the diagonal values denote the variances in the parameters and the nondiagonal components denote the covariances between the parameters. Since the 