Authors
H Abdalla, F Aharonian, F Ait Benkhali, EO Angüner, M Arakawa, C Arcaro, C Armand, M Arrieta, M Backes, M Barnard, Yvonne Becherini, J Becker Tjus, D Berge, K Bernlöhr, R Blackwell, M Böttcher, C Boisson, J Bolmont, S Bonnefoy, P Bordas, J Bregeon, F Brun, P Brun, M Bryan, M Büchele, T Bulik, Tomas Bylund, M Capasso, S Caroff, A Carosi, S Casanova, M Cerruti, N Chakraborty, T Chand, S Chandra, RCG Chaves, A Chen, S Colafrancesco, B Condon, ID Davids, C Deil, J Devin, P Dewilt, L Dirson, A Djannati-Atai, A Dmytriiev, A Donath, V Doroshenko, LO’C Drury, J Dyks, K Egberts, G Emery, J-P Ernenwein, S Eschbach, S Fegan, A Fiasson, G Fontaine, S Funk, M Fuessling, S Gabici, YA Gallant, F Gate, G Giavitto, D Glawion, JF Glicenstein, D Gottschall, M-H Grondin, J Hahn, M Haupt, G Heinzelmann, G Henri, G Hermann, JA Hinton, W Hofmann, C Hoischen, TL Holch, M Holler, D Horns, D Huber, H Iwasaki, A Jacholkowska, Marek Jamrozy, D Jankowsky, F Jankowsky, L Jouvin, I Jung-Richardt, MA Kastendieck, K Katarzyński, M Katsuragawa, U Katz, D Kerszberg, D Khangulyan, B Khelifi, J King, S Klepser, W Kluźniak, Nu Komin, K Kosack, M Kraus, G Lamanna, J Lau, J Lefaucheur, A Lemiere, M Lemoine-Goumard, J-P Lenain, E Leser, T Lohse, R Lopez-Coto, I Lypova, D Malyshev, V Marandon, A Marcowith, C Mariaud, G Marti-Devesa, R Marx, G Maurin, PJ Meintjes, AMW Mitchell, R Moderski, M Mohamed, L Mohrmann, C Moore, E Moulin, T Murach, S Nakashima, M de Naurois, H Ndiyavala, F Niederwanger, J Niemiec, L Oakes, P O’Brien, H Odaka, S Ohm, Michał Ostrowski, I Oya, M Panter, RD Parsons, C Perennes, P-O Petrucci, B Peyaud, Q Piel, S Pita, V Poireau, A Priyana Noel, DA Prokhorov, H Prokoph, G Puehlhofer, Michael Punch, A Quirrenbach, S Raab
Publication date
2019/1/1
Journal
Astronomy & Astrophysics
Volume
621
Pages
A116
Publisher
EDP Sciences
Description
Context
We present a detailed view of the pulsar wind nebula (PWN) HESS J1825–137. We aim to constrain the mechanisms dominating the particle transport within the nebula, accounting for its anomalously large size and spectral characteristics.
Aims
The nebula was studied using a deep exposure from over 12 years of H.E.S.S. I operation, together with data from H.E.S.S. II that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) γ-ray properties of the nebula.
Methods
The nebula emission is revealed to extend out to 1.5° from the pulsar, ~1.5 times farther than previously seen, making HESS J1825–137, with an intrinsic diameter of ~100 pc, potentially the largest γ-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle …
Scholar articles
H Abdalla, F Aharonian, FA Benkhali, EO Angüner… - Astronomy & Astrophysics, 2019