  The exact sources of high-energy neutrinos detected by the IceCube neutrino
observatory still remain a mystery. For the first time, this work explores the
hypothesis that galaxy mergers may serve as sources for these high-energy
neutrinos. Galaxy mergers can host very high-energy hadronic and photohadronic
processes, which may produce very high-energy neutrinos. We perform an unbinned
maximum-likelihood-ratio analysis utilizing the galaxy merger data from six
catalogs and 10 years of public IceCube muon-track data to quantify any
correlation between these mergers and neutrino events. First, we perform the
single source search analysis, which reveals that none of the considered galaxy
mergers exhibit a statistically significant correlation with high-energy
neutrino events detected by IceCube. Furthermore, we conduct a stacking
analysis with three different weighting schemes to understand if these galaxy
mergers can contribute significantly to the diffuse flux of high-energy
astrophysical neutrinos detected by IceCube. We find that upper limits (at
$95\%$ c.l.) of the all flavour high-energy neutrino flux, associated with
galaxy mergers considered in this study, at $100$ TeV with spectral index
$\Gamma=-2$ are $2.57\times 10^{-18}$, $8.51 \times 10^{-19}$ and $2.36 \times
10^{-18}$ $\rm GeV^{-1}\,cm^2\,s^{-1}\,sr^{-1}$ for the three weighting
schemes. This work shows that these selected galaxy mergers do not contribute
significantly to the IceCube detected high energy neutrino flux. We hope that
in the near future with more data, the search for neutrinos from galaxy mergers
can either discover their neutrino production or impose more stringent
constraints on the production mechanism of high-energy neutrinos within galaxy
mergers.
