  Most neutron stars are expected to be born in supernovae, but only about half
of supernova remnants (SNRs) are associated with a compact object. In many
cases, a supernova progenitor may have resulted in a black hole. However, there
are several possible reasons why true pulsar-SNR associations may have been
missed in previous surveys: The pulsar's radio beam may not be oriented towards
us; the pulsar may be too faint to be detectable; or there may be an offset in
the pulsar position caused by a kick. Our goal is to find new pulsars in SNRs
and explore their possible association with the remnant. The search and
selection of the remnants presented in this paper was inspired by the
non-detection of any X-ray bright compact objects in these remnants when
previously studied. Five SNRs were searched for radio pulsars with the Green
Bank Telescope at 820 MHz with multiple pointings to cover the full spatial
extent of the remnants. A periodicity search plus an acceleration search up to
500 m/s^2 and a single pulse search were performed for each pointing in order
to detect potential isolated binary pulsars and single pulses, respectively. No
new pulsars were detected in the survey. However, we were able to re-detect a
known pulsar, PSR J2047+5029, near SNR G89.0+4.7. We were unable to detect the
radio-quiet gamma-ray pulsar PSR J2021+4026, but we do find a flux density
limit of 0.08 mJy. Our flux density limits make our survey two to 16 times more
sensitive than previous surveys, while also covering the whole spatial extent
of the same remnants. We discuss potential explanations for the non-detection
of a pulsar in the studied SNRs and conclude that sensitivity is still the most
likely factor responsible for the lack of pulsars in some remnants.
