2026-06-27T01:08:43Zhttps://docta.ucm.es/rest/oai/requestoai:docta.ucm.es:20.500.14352/438832024-09-05T17:51:16Zcom_20.500.14352_14col_20.500.14352_15
Docta Complutense
author
Antoranz Canales, Pedro
author
Barrio Uña, Juan Abel
author
Contreras González, José Luis
author
Fonseca González, María Victoria
author
López Moya, Marcos
author
Miranda Pantoja, José Miguel
author
Satalecka, Konstanzja
author
Scapin, Valeria
2023-06-20T03:33:48Z
2023-06-20T03:33:48Z
2011-11-20
0004-637X
10.1088/0004-637X/742/1/43
https://hdl.handle.net/20.500.14352/43883
http://dx.doi.org/10.1088/0004-637X/742/1/43
http://iopscience.iop.org
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.
eng
Observations of the Crab pulsar between 25 and 100 GeV with the MAGIC I telescope
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MirandaJM16libre.pdf
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MirandaJM16libre.pdf.txt