  Axions or ALPs are hypothetical particles predicted by BSM theories, which
make one of the dark matter candidates. These particles can convert into
photons and vice-versa in the presence of magnetic field, with a probability
decided by its coupling strength $\mathrm{g_{a\gamma}}$. One of the ways to
detect these particles is using the CMB as a backlight. As the CMB photons pass
through a galaxy cluster, they can get converted into ALPs in the mass range
$10^{-15}$ eV to $10^{-11}$ eV through resonant conversion in the presence of
cluster magnetic fields. This leads to a polarized spectral distortion
($\alpha$-distortion) in the CMB as the photon polarization parallel to the
magnetic field in the galaxy cluster is involved in the conversion. The
fluctuations in the magnetic field and electron density in a galaxy cluster
lead to spatially varying $\alpha$-distortion around the cluster, with a power
spectrum that is different from the lensed CMB polarization power spectrum for
the standard model of cosmology. By measuring the difference in the
polarization power spectrum around a galaxy cluster from the all-sky signal,
one can find new $\alpha$-distortion in the sky. For galaxy clusters resolvable
in multiple EM bands, one can measure the coupling strength
$\mathrm{g_{a\gamma}}$ from the ALP power spectrum. Using multi-frequency
techniques like ILC to clean the foregrounds, we show that the new power
spectrum-based approach of the resolved galaxy clusters from upcoming CMB
experiments such as Simons Observatory and CMB-S4 can detect (or put
constraints) on the ALP-photon coupling strength of $\mathrm{g_{a\gamma} < 5.24
\times 10^{-12} \, GeV^{-1}}$ and $\mathrm{g_{a\gamma} < 3.61 \times 10^{-12}
\, GeV^{-1}}$ at 95\% C.I. respectively for ALPs of masses $10^{-13}$ eV or for
smaller $\mathrm{g_{a\gamma}}$ for lighter ALP masses (Abridged).
