cadence, this strategy not only yields detections of multiply imaged supernovae, but it also enables the measurement of basic lensing properties such as time delays and flux ratios between the images. In this respect, this is an ideal observational strategy for large and self-contained surveys such as the LSST. Initial information on lensing configurations can be also used to pin down the best candidates for follow-up observations.

Magnification
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Strongly lensed supernovae can be detected as transients which appear significantly brighter than the brightest supernovae at the redshift of the apparent host galaxy (lens galaxy for lensed supernovae or actual host galaxy for non-lensed transients). Following @Gold2017, the detection criterion can by formulated in the following way: $$\begin{aligned}
m_{\rm X}(t_{\rm peak}) & < & \langle M_{\rm X}\rangle(t_{\rm peak})+\mu(z_{\rm host})+\nonumber \\
 & & K_{\rm XX}(z_{\rm host},t_{\rm peak})+\Delta m,
\label{criterion_magnification}\end{aligned}$$ where $m_{\rm X}(t_{\rm peak})$ is the observed peak magnitude of the transient in band $X$, $\langle M_{\rm X}\rangle(t_{\rm peak})$ is a mean absolute magnitude of a reference class of brightest supernovae in band $X$ at peak, $\mu$ is the distance modulus, $z_{\rm host}$ is redshift of the apparent host galaxy, $K_{XX}(z_{\rm host},t_{\rm peak})$ is a K-correction for the assumed reference class of 