2007/05/31 by MAGIC Collaboration, J. Albert, E. Aliu +97 · 1 citation
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Crab Nebula #Crab Pulsar #Cutoff #Flux (metallurgy) #Gamma-ray bursts and supernovae #MAGIC (telescope) #Nebula #Physics #Pulsar #Pulsars and Gravitational Waves Research #Spectral energy distribution #Spectral line #Stars #Telescope #astro-ph
paper · pdf · doi:10.1086/525270
published as Astrophys.J.674:1037-1055,2008 · Version published in ApJ, added corresponding author
openalex publication_date 2008/02/15 · arxiv created 2008/07/09 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We report about very high energy (VHE) γ-ray observations of the Crab Nebula with the MAGIC telescope. The γ-ray flux from the nebula was measured between 60 GeV and 9 TeV. The energy spectrum can be described by a curved power law dF/dE = f 0 ( E /300 GeV) [ a+b log 10 ( E /300 GeV)] with a flux normalization f 0 of (6.0 ± 0.2 stat ) × 10 −10 cm −2 s −1 TeV −1 , a = − 2.31 ± 0.06 stat , and b = − 0.26 ± 0.07 stat . The peak in the spectral energy distribution is estimated at 77 ± 35 GeV. Within the observation time and the experimental resolution of the telescope, the γ-ray emission is steady and pointlike. The emission's center of gravity coincides with the position of the pulsar. Pulsed γ-ray emission from the pulsar could not be detected. We constrain the cutoff energy of the pulsed spectrum to be less than 27 GeV, assuming that the differential energy spectrum has an exponential cutoff. For a superexponential shape, the cutoff energy can be as high as 60 GeV.