  Evidence of efficient acceleration of cosmic rays in massive young stellar
objects has been recently reported. Among these massive protostars, S255 NIRS 3
for which extreme flaring events associated with radio jets have been detected,
is one of the best objects to test this hypothesis. We search for gamma-ray
emission associated with this object in Fermi-LAT data and inspect the gas
content in different molecular lines using the MWISP survey. A GeV source
dubbed 4FGL J0613.1+1749c lies on top of the MYSO region, where two filamentary
~10 pc CO structures extend along the same direction of the sub-parsec radio
jets. We investigate the spectrum, morphology, and light curve of the gamma-ray
source and compare it with the theoretical emission expected from hadronic and
leptonic populations accelerated in the radio jets. We argue that the gamma-ray
source could be powered by particles accelerated in the S255 NIRS 3 jets,
radiating via Bremsstrahlung or proton-proton interaction, and with a
synchrotron component shinning in radio from primary or secondary electrons in
the case of a leptonic or hadronic population.
