  The knowledge of the positions of the corotation resonance in spiral arms is
a key way to estimate their pattern speed, which is a fundamental parameter
determining the galaxy dynamics. Various methods for its estimation have been
developed, but they all demonstrate certain limitations and a lack of agreement
with each other. Here, we present a new method for estimating the corotation
radius. This method takes into account the shape of the profile across the arm
and its width and, thus, only photometric data is needed. The significance of
the method is that it can potentially be used for the farthest galaxies with
measurable spiral arms. We apply it to a sample of local galaxies from
Savchenko et al. and compare the obtained corotation radii with those
previously measured in the literature by other methods. Our results are in good
agreement with the literature. We also apply the new method to distant galaxies
from the COSMOS field. For the first time, corotation locations for galaxies
with photometric redshifts up to $z\sim0.9$ are measured.
