Gamma-ray emission from star-forming complexes observed by MAGIC: The cases of W51 and HESS J1857+026
1 Università di Padova and INFN, 35131 Padova, Italy
2 Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, 28040 Madrid, Spain
3 Deutsches Elektronen-Synchrotron (DESY), 15738 Zeuthen, Germany
4 IFAE, Campus UAB, 08193 Bellaterra, Spain
5 Now at Deutsches Elektronen-Synchrotron (DESY), 15738 Zeuthen, Germany
6 Max-Planck-Institut für Physik, 80805 München, Germany
7 Now at Astroparticule et Cosmologie (APC), Université Paris 7 Denis Diderot, 75205 Paris Cedex 13, France
8 Now at School of Chemistry & Physics, University of Adelaide, Adelaide 5005, Australia
a e-mail: firstname.lastname@example.org
Published online: 8 December 2015
Massive star-forming regions assemble a large number of young stars with remnants of stellar evolution and a very dense environment. Therefore, particles accelerated in supernova remnants and pulsar wind nebulae encounter optimal conditions for interacting with target material and photon fields, and thus produce gamma-ray emission. However, observations are challenging because multiple phenomena may appear entangled within the resolution of current gamma-ray telescopes. We report on MAGIC observations aimed to understand the nature of the emission from the star-forming region W51 and the unidentified source HESS J1857+026. While gamma-ray emission from W51 is dominated by the interaction of the supernova remnant W51C with dense molecular clouds, HESS J1857+026 is associated to the pulsar wind nebula from PSR J1856+0245. However, an additional source is resolved north of HESSJ1857+026, with sufficient separation to determine that it cannot be powered by the same pulsar. We search for multiwavelength data to determine the origin of the new source.
© Owned by the authors, published by EDP Sciences, 2015
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