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Gamma-ray emission provides constraints on the non-thermal radiationprocesses at play in astrophysical particle accelerators. This allows both thenature of accelerated particles and the maximum energy that they can reach tobe determined. Notably, it remains an open question to what extent supernovaremnants (SNRs) contribute to the sea of Galactic cosmic rays. In the Galacticplane, at around 312{\deg} of Galactic longitude, Fermi-LAT observations showan extended source (4FGL J1409.1-6121e) around five powerful pulsars. Thissource is described by one large disk of 0.7{\deg} radius with a highsignificance of 45 sigma in the 4FGL-DR3 catalog. Using 14 years of Fermi-LATobservations, we revisited this region with a detailed spectro-morphologicalanalysis in order to disentangle its underlying structure. Three sources havebeen distinguished, including the supernova remnant G312.4-0.4 whose gamma-rayemission correlates well with the shell observed at radio energies. The hardspectrum detected by the LAT, extending up to 100 GeV without any sign ofcut-off, is well reproduced by a purely hadronic model.

Fermi-LAT detection of the supernova remnant G312.4-0.4 in the vicinity of 4FGL J1409.1-6121e