EPJ Web of Conferences
Volume 105, 2015SuGAR 2015 – Searching for the Sources of Galactic Cosmic Rays
|Number of page(s)||4|
|Section||The Galaxy in Gamma Rays|
|Published online||08 December 2015|
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
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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