RT Journal Article T1 Periodic very high energy gamma-ray emission from LS I+61 degrees 303 observed with the MAGIC Telescope A1 Antoranz Canales, Pedro A1 Barrio Uña, Juan Abel A1 Contreras González, José Luis A1 Fonseca González, María Victoria A1 Miranda Pantoja, José Miguel A1 Nieto Castaño, Daniel AB The MAGIC collaboration has recently reported the discovery of gamma-ray emission from the binary system LS I +61 degrees 303 in the TeV energy region. Here we present new observational results on this source in the energy range between 300 GeV and 3 TeV. In total, 112 hr of data were taken between 2006 September and December covering four orbital cycles of this object. This large amount of data allowed us to produce an integral flux light curve covering for the first time all orbital phases of LS I +61 degrees 303. In addition, we also obtained a differential energy spectrum for two orbital phase bins covering the phase range 0.5 < phi < 0.6 and 0.6 < phi < 0.7. The photon index in the two phase bins is consistent within the errors with an average index Gamma = 2.6 +/- 0.2(stat) +/- 0.2(sys). LS I +61 degrees 303 was found to be variable at TeV energies on timescales of days. These new MAGIC measurements allowed us to search for intranight variability of the very high energy emission; however, no evidence for flux variability on timescales down to 30 min was found. To test for possible periodic structures in the light curve, we apply the formalism developed by Lomb and Scargle to the LS I +61 degrees 303 data taken in 2005 and 2006. We found the LS I +61 degrees 303 data set to be periodic with a period of (26.8 +/- 0.2) days (with a post-trial chance probability of 10(-7)), close to the orbital period. PB IOP Publishing SN 0004-637X YR 2009 FD 2009-03-01 LK https://hdl.handle.net/20.500.14352/43960 UL https://hdl.handle.net/20.500.14352/43960 LA eng NO © The American Astronomical Society. We thank the IAC for the excellent working conditions at the ORM. The support of the German BMBF, MPG, and the YIP of the Helmholtz Gemeinschaft, the Italian INFN, the Spanish MEC, the ETH Research Grant TH 34/04 3 and the Polish MNiI Grant 1P03D01028 is gratefully acknowledged. NO German BMBF NO MPG NO YIP of the Helmholtz Gemeinschaft NO Italian INFN NO Spanish MEC NO ETH Research Grant NO Polish MNiI DS Docta Complutense RD 8 jun 2025