  The supernova remnant (SNR) G51.26+0.11 was recently discovered and little is
known about its properties and environment. Using data from the \emph{Fermi}
Large Area Telescope we study the GeV emission seen in the direction of
G51.26+0.11 to constrain the origin of the gamma rays and their possible
relation to this SNR or to a star-forming region. We also search for emission
from molecular gas in the region that could provide dense material for the
production of gamma rays. By modeling the multi-wavelength spectrum of
G51.26+0.11 from radio to gamma rays we derive the properties of the particle
populations that could produce the emission in several possible scenarios. We
rule out the star-forming regions (such as G051.010+00.060) seen nearby as the
origin of the GeV emission. The correspondence seen between the gamma-ray and
radio morphologies support a scenario where G51.26+0.11 is the cause of the
gamma rays. The flat spectral energy distribution observed at GeV energies is
best fit by hadronic or inverse Compton emission, while a bremsstrahlung model
cannot 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 or
confirmed.
