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Isotopic and elemental abundances seen in Galactic cosmic rays imply that$\sim20\%$ of the cosmic-ray (CR) nuclei are probably synthesized by massiveWolf-Rayet (WR) stars. Massive star clusters hosting WR and OB-type stars havebeen proposed as potential Galactic cosmic-ray accelerators for decades, inparticular via diffusive shock acceleration at wind termination shocks. Here wereport the analysis of {\em Fermi} Large Area Telescope's data towards thedirection of Masgomas-6a, a young massive star cluster candidate hosting two WRstars. We detect an extended $\gamma$-ray source with $\rm{TS}=183$ in thevicinity of Masgomas-6a, spatially coincident with two unassociated {\em Fermi}4FGL sources. We also present the CO observational results of molecular cloudsin this region, using the data from the Milky Way Imaging Scroll Paintingproject. The $\gamma$-ray emission intensity correlates well with thedistribution of molecular gas at the distance of Masgomas-6a, indicating thatthese gamma rays may be produced by CRs accelerated by massive stars inMasgomas-6a. At the distance of $3.9{\rm \ kpc}$ of Masgomas-6a, the luminosityof the extended source is $(1.81\pm0.02)\times 10^{35}{\rm \ erg \ s^{-1}}$.With a kinetic luminosity of $\sim 10^{37}{\rm erg \ s^{-1}}$ in the stellarwinds, the WR stars are capable of powering the $\gamma$-ray emission vianeutral pion decay resulted from cosmic ray $pp$ interactions. The size of theGeV source and the energetic requirement suggests a CR diffusion coefficientsmaller than that in the Galactic interstellar medium, indicating strongsuppression of CR diffusion in the molecular cloud.

Detection of diffuse gamma-ray emission towards a massive star forming region hosting Wolf-Rayet stars