2026-06-27T12:31:57Zhttps://docta.ucm.es/rest/oai/request

oai:docta.ucm.es:20.500.14352/438832024-09-05T17:51:16Zcom_20.500.14352_14col_20.500.14352_15

Observations of the Crab pulsar between 25 and 100 GeV with the MAGIC I telescope Antoranz Canales, Pedro Barrio Uña, Juan Abel Contreras González, José Luis Fonseca González, María Victoria López Moya, Marcos Miranda Pantoja, José Miguel Satalecka, Konstanzja Scapin, Valeria We report on the observation of gamma-rays above 25 GeV from the Crab pulsar (PSR B0532+ 21) using the MAGIC I telescope. Two data sets from observations during the winter period 2007/2008 and 2008/2009 are used. In order to discuss the spectral shape from 100 MeV to 100 GeV, one year of public Fermi Large Area Telescope (Fermi-LAT) data are also analyzed to complement the MAGIC data. The extrapolation of the exponential cutoff spectrum determined with the Fermi-LAT data is inconsistent with MAGIC measurements, which requires a modification of the standard pulsar emission models. In the energy region between 25 and 100 GeV, the emission in the P1 phase (from -0.06 to 0.04, location of the main pulse) and the P2 phase (from 0.32 to 0.43, location of the interpulse) can be described by power laws with spectral indices of -3.1 +/- 1.0(stat) +/- 0.3(syst) and -3.5 +/- 0.5(stat) +/- 0.3(syst), respectively. Assuming an asymmetric Lorentzian for the pulse shape, the peak positions of the main pulse and the interpulse are estimated to be at phases -0.009 +/- 0.007 and 0.393 +/- 0.009, while the full widths at half- maximum are 0.025 +/- 0.008 and 0.053 +/- 0.015, respectively. 2023-06-20T03:33:48Z 2023-06-20T03:33:48Z 2023-06-20T03:33:48Z 2011-11-20 journal article https://hdl.handle.net/20.500.14352/43883 0004-637X 10.1088/0004-637X/742/1/43 eng CSD2007-00042 CSD2009-00064 DO02-353 127740 SFB823/C4 SFB876/C3 restricted access IOP Publishing