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The supernova remnant (SNR) G51.26+0.11 was recently discovered and little isknown about its properties and environment. Using data from the \emph{Fermi}Large Area Telescope we study the GeV emission seen in the direction ofG51.26+0.11 to constrain the origin of the gamma rays and their possiblerelation to this SNR or to a star-forming region. We also search for emissionfrom molecular gas in the region that could provide dense material for theproduction of gamma rays. By modeling the multi-wavelength spectrum ofG51.26+0.11 from radio to gamma rays we derive the properties of the particlepopulations that could produce the emission in several possible scenarios. Werule out the star-forming regions (such as G051.010+00.060) seen nearby as theorigin of the GeV emission. The correspondence seen between the gamma-ray andradio morphologies support a scenario where G51.26+0.11 is the cause of thegamma rays. The flat spectral energy distribution observed at GeV energies isbest fit by hadronic or inverse Compton emission, while a bremsstrahlung modelcannot properly account for the radio fluxes under a simple one-zone scenario.A pulsar wind nebula origin of the high-energy photons cannot be ruled out orconfirmed.

GeV emission in the region of the supernova remnant G51.26+0.11