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The recent detection of significant neutrino flux from the inner Galacticplane by the IceCube detector has provided us valuable insights on the spectrumof cosmic rays in our Galaxy. This flux can be produced either by a populationof Galactic point sources or by diffused emission from cosmic ray interactionswith the interstellar medium or by a mixture of both. In this work, we computediffused gamma-ray and neutrino fluxes produced by a population of giantmolecular clouds (GMCs) in our Galaxy, assuming different parametrizations ofthe Galactic diffused cosmic ray distribution. In particular, we take intoaccount two main cases: (I) constant cosmic ray luminosity in our Galaxy, and(II) space-dependent cosmic ray luminosity based on the supernovae distributionin our Galaxy. For Case-I, we found that the neutrino flux from GMCs is afactor of $\sim 10$ below compared to $\pi^0$ and KRA$_\gamma$ best-fittedmodels of IceCube observations at $10^5$ GeV. Instead, for Case-II the modelcan explain up to $\sim 90 \%$ of the neutrino flux at that energy. Moreover,for this scenario IceCube detector could be able to detect neutrino events fromthe Galactic centre regions. We then calculated the gamma-ray and neutrinofluxes from individual GMCs and noticed that several current and futureCherenkov telescopes and neutrino observatories have the right sensitivities tostudy these objects. In particular, very neutrino-bright region such as AquilaRift is favourable for detection by the IceCube-Gen2 observatory.

Gamma-rays and Neutrinos from Giant Molecular Cloud Populations in the Galactic Plane