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dc.contributor.authorAbdo, A.A.en_US
dc.contributor.authorVenter, C.en_US
dc.contributor.authorAckermann, M.en_US
dc.contributor.authorAjello, M.en_US
dc.contributor.authorAtwood, W.B.en_US
dc.date.accessioned2012-02-29T09:51:50Z
dc.date.available2012-02-29T09:51:50Z
dc.date.issued2010en_US
dc.identifier.citationAbdo, A.A. et al. 2010. Observations of the Large Magellanic Cloud with Fermi. Astronomy & astrophysics, 512(A7):13474-13489. [https://doi.org/10.1051/0004-6361/200913474 ]en_US
dc.identifier.issn0004-6361en_US
dc.identifier.issn1432-0746 (Online)en_US
dc.identifier.urihttp://hdl.handle.net/10394/6048
dc.identifier.urihttps://doi.org/10.1051/0004-6361/200913474
dc.description.abstractContext. The Large Magellanic Cloud (LMC) is to date the only normal external galaxy that has been detected in high-energy gamma rays. Highenergy gamma rays trace particle acceleration processes and gamma-ray observations allow the nature and sites of acceleration to be studied. Aims. We characterise the distribution and sources of cosmic rays in the LMC from analysis of gamma-ray observations. Methods. We analyse 11 months of continuous sky-survey observations obtained with the Large Area Telescope aboard the Fermi Gamma-Ray Space Telescope and compare it to tracers of the interstellar medium and models of the gamma-ray sources in the LMC. Results. The LMC is detected at 33σ significance. The integrated >100 MeV photon flux of the LMC amounts to (2.6 ± 0.2) × 10−7 ph cm−2 s−1 which corresponds to an energy flux of (1.6 ± 0.1) × 10−10 erg cm−2 s−1, with additional systematic uncertainties of <∼16%. The analysis reveals the massive star forming region 30 Doradus as a bright source of gamma-ray emission in the LMC in addition to fainter emission regions found in the northern part of the galaxy. The gamma-ray emission from the LMC shows very little correlation with gas density and is rather correlated to tracers of massive star forming regions. The close confinement of gamma-ray emission to star forming regions suggests a relatively short GeV cosmic-ray proton diffusion length. Conclusions. The close correlation between cosmic-ray density and massive star tracers supports the idea that cosmic rays are accelerated in massive star forming regions as a result of the large amounts of kinetic energy that are input by the stellar winds and supernova explosions of massive stars into the interstellar medium
dc.publisherEDP Sciencesen_US
dc.subjectAcceleration of particles
dc.subjectCosmic rays
dc.subjectMagellanic Clouds
dc.subjectGamma rays: galaxies
dc.titleObservations of the Large Magellanic Cloud with Fermien_US
dc.contributor.researchID12006653 - Venter, Christo


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