  A co-rotation radius is a key characteristic of disc galaxies that is
essential to determine the angular speed of the spiral structure $\Omega_{p}$,
and therefore understand its nature. In the literature, there are plenty of
methods to estimate this value, but do these measurements have any consistency?
In this work, we collected a dataset of corotation radius measurements for 547
galaxies, 300 of which had at least two values. An initial analysis reveals
that most objects have rather inconsistent corotation radius positions.
Moreover, a significant fraction of galactic discs is distinguished by a large
error coverage and almost uniform distribution of measurements. These findings
do not have any relation to spiral type, Hubble classification, or presence of
a bar. Among other reasons, obtained results could be explained by the
transient nature of spirals in a considerable part of galaxies. We have made
our collected data sample publicly available, and have demonstrated on one
example how it could be useful for future research by investigating a winding
time value for a sample of galaxies with possible multiple spiral arm patterns.
