Chen, A. W.A. W.ChenPiano, G.G.PianoTavani, M.M.TavaniAntonelli, L. A.L. A.AntonelliPittori, CarlottaCarlottaPittoriGiommi, PaoloPaoloGiommiVerrecchia, FrancescoFrancescoVerrecchiaLucarelli, FabrizioFabrizioLucarelliSantolamazza, P.P.SantolamazzaColafrancesco, SergioSergioColafrancesco2020-09-172020-09-172011-01-01https://hdl.handle.net/20.500.13025/2067Astronomy and Astrophysics, Volume 525, id.A33, <NUMPAGES>7</NUMPAGES> pp.Context. Identification of gamma-ray-emitting Galactic sources is a long-standing problem in astrophysics. One such source, 1AGL J2022+4032, coincident with the interior of the radio shell of the supernova remnant Gamma Cygni (SNR G78.2+2.1) in the Cygnus region, has recently been identified by Fermi as a gamma-ray pulsar, LAT PSR J2021+4026. <BR /> Aims We present long-term observations of 1AGL J2022+4032 with the AGILE gamma-ray telescope, measuring its flux and light curve. <BR /> Methods We compare the light curve of 1AGL J2022+4032 with that of 1AGL J2021+3652 (PSR J2021+3651), showing that the flux variability of 1AGL J2022+4032 appears to be greater than the level predicted from statistical and systematic effects and producing detailed simulations to estimate the probability of the apparent observed variability. <BR /> Results We evaluate the possibility that the gamma-ray emission may be due to the superposition of two or more point sources, some of which may be variable, considering a number of possible counterparts. <BR /> Conclusions We consider the possibility of a nearby X-ray quiet microquasar contributing to the flux of 1AGL J2022+4032 to be more likely than the hypotheses of a background blazar or intrinsic gamma-ray variabilty of LAT PSR J2021+4026.pulsars individual 1AGL J2022+4032gamma rays starspulsars individual 1FGL J2021.5+4026pulsars individual LAT PSR J2021+4026pulsars individual 3EG J2020+401710.1051/0004-6361/201015279http://adsabs.harvard.edu/abs/2011A&A...525A..33C2011A&A...525A..33C