  Recent gravitational-wave observations have begun to constrain the internal
physics of neutron stars. However, current detection searches for neutron star
systems assume that potential neutron stars are low-mass black holes, ignoring
any affect on the gravitational-wave signal due to the internal neutron-star
physics. We wish to create a template bank of binary neutron star waveforms
including the effect of tidal deformability. However, we find that the Fisher
matrix, which is commonly used to approximate match calculations when placing
template banks, is unsuitable to predict the match between two binary neutron
star waveforms. We find that the Fisher matrix can predict errors on the
mismatch that are larger than $100\%$ when attempting to identify waveforms
with a match of $0.97$. We explore the regime in which the Fisher matrix cannot
be trusted and examine why it breaks down. We demonstrate that including
higher-order terms in the Taylor series expansion of the match can reliably
compute matches for these examples, but that it is prohibitively
computationally expensive to do so. Finally, we demonstrate that stochastic
placement can still be used to construct a template bank of tidally deformed
neutron-star waveforms.
