TY - JOUR
A1 - Meyer, Dominique M.-A.
A1 - Velazquez, Pablo F.
A1 - Petruk, Oleh
A1 - Chiotellis, Alexandros
A1 - Pohl, Martin
A1 - Camps-Farina, Artemi
A1 - Petrov, Miroslav
A1 - Reynoso, Estela M.
A1 - Toledo-Roy, Juan C.
A1 - Schneiter, E. Matias
A1 - Castellanos-Ramirez, Antonio
A1 - Esquivel, Alejandro
T1 - Rectangular core-collapse supernova remnants
BT - application to Puppis A
JF - Monthly notices of the Royal Astronomical Society
N2 - Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n approximate to 1 cm(-3), T approximate to 8000 K), an organized magnetic field of strength 7 mu G has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper, we show through 2.5D magnetohydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35 M 0 star, that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age (15-20 kyr), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetized, shocked stellar progenitor bubble into which the supernova blast wave expands. Our calculations for non-thermal emission, i.e. radio synchrotron and inverse-Compton radiation, reveal that such supernova remnants can, due to projection effects, appear as rectangular objects in certain cases. This mechanism for shaping a supernova remnant is similar to the bipolar and elliptical planetary nebula production by wind-wind interaction in the low-mass regime of stellar evolution. If such a rectangular core-collapse supernova remnant is created, the progenitor star must not have been a runaway star. We propose that such a mechanism is at work in the shaping of the asymmetric core-collapse supernova remnant Puppis A.
KW - stars: evolution
KW - stars: massive
KW - ISM: supernova remnants
KW - methods: MHD
Y1 - 2022
U6 - https://doi.org/10.1093/mnras/stac1832
SN - 0035-8711
SN - 1365-2966
VL - 515
IS - 1
SP - 594
EP - 605
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Wilhelm, Alina
A1 - Telezhinsky, Igor
A1 - Dwarkadas, Vikram V.
A1 - Pohl, Martin
T1 - Stochastic re-acceleration and magnetic-field damping in Tycho’s supernova remnant
JF - Astronomy and astrophysics
N2 - Context.
Tycho's supernova remnant (SNR) is associated with the historical supernova (SN) event SN 1572 of Type Ia. The explosion occurred in a relatively clean environment, and was visually observed, providing an age estimate. This SNR therefore represents an ideal astrophysical test-bed for the study of cosmic-ray acceleration and related phenomena. A number of studies suggest that shock acceleration with particle feedback and very efficient magnetic-field amplification combined with Alfvenic drift are needed to explain the rather soft radio spectrum and the narrow rims observed in X-rays.
Aims.
We show that the broadband spectrum of Tycho's SNR can alternatively be well explained when accounting for stochastic acceleration as a secondary process. The re-acceleration of particles in the turbulent region immediately downstream of the shock should be efficient enough to impact particle spectra over several decades in energy. The so-called Alfvenic drift and particle feedback on the shock structure are not required in this scenario. Additionally, we investigate whether synchrotron losses or magnetic-field damping play a more profound role in the formation of the non-thermal filaments.
Methods.
We solved the full particle transport equation in test-particle mode using hydrodynamic simulations of the SNR plasma flow. The background magnetic field was either computed from the induction equation or follows analytic profiles, depending on the model considered. Fast-mode waves in the downstream region provide the diffusion of particles in momentum space.
Results.
We show that the broadband spectrum of Tycho can be well explained if magnetic-field damping and stochastic re-acceleration of particles are taken into account. Although not as efficient as standard diffusive shock acceleration, stochastic acceleration leaves its imprint on the particle spectra, which is especially notable in the emission at radio wavelengths. We find a lower limit for the post-shock magnetic-field strength similar to 330 mu G, implying efficient amplification even for the magnetic-field damping scenario. Magnetic-field damping is necessary for the formation of the filaments in the radio range, while the X-ray filaments are shaped by both the synchrotron losses and magnetic-field damping.
KW - acceleration of particles
KW - radiation mechanisms: non-thermal
KW - ISM: supernova remnants
KW - cosmic rays
KW - ISM: individual objects: Tycho's SNR
KW - shock waves
Y1 - 2020
U6 - https://doi.org/10.1051/0004-6361/201936079
SN - 0004-6361
SN - 1432-0746
VL - 639
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abdalla, H.
A1 - Adam, R.
A1 - Aharonian, Felix A.
A1 - Benkhali, F. Ait
A1 - Angüner, Ekrem Oǧuzhan
A1 - Arcaro, C.
A1 - Armand, C.
A1 - Armstrong, T.
A1 - Ashkar, H.
A1 - Backes, M.
A1 - Baghmanyan, V.
A1 - Martins, V. Barbosa
A1 - Barnacka, A.
A1 - Barnard, M.
A1 - Becherini, Y.
A1 - Berge, D.
A1 - Bernlohr, K.
A1 - Bi, B.
A1 - Bottcher, M.
A1 - Boisson, C.
A1 - Bolmont, J.
A1 - de Lavergne, M. de Bony
A1 - Bordas, Pol
A1 - Breuhaus, M.
A1 - Brun, F.
A1 - Brun, P.
A1 - Bryan, M.
A1 - Buchele, M.
A1 - Bulik, T.
A1 - Bylund, T.
A1 - Caroff, S.
A1 - Carosi, A.
A1 - Casanova, Sabrina
A1 - Chand, T.
A1 - Chandra, S.
A1 - Chen, A.
A1 - Cotter, G.
A1 - Curylo, M.
A1 - Mbarubucyeye, J. Damascene
A1 - Davids, I. D.
A1 - Davies, J.
A1 - Deil, C.
A1 - Devin, J.
A1 - deWilt, P.
A1 - Dirson, L.
A1 - Djannati-Atai, A.
A1 - Dmytriiev, A.
A1 - Donath, A.
A1 - Doroshenko, V.
A1 - Duffy, C.
A1 - Dyks, J.
A1 - Egberts, Kathrin
A1 - Eichhorn, F.
A1 - Einecke, S.
A1 - Emery, G.
A1 - Ernenwein, J. -P.
A1 - Feijen, K.
A1 - Fegan, S.
A1 - Fiasson, A.
A1 - de Clairfontaine, G. Fichet
A1 - Fontaine, G.
A1 - Funk, S.
A1 - Fussling, Matthias
A1 - Gabici, S.
A1 - Gallant, Y. A.
A1 - Giavitto, G.
A1 - Giunti, L.
A1 - Glawion, D.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Grondin, M. -H.
A1 - Hahn, J.
A1 - Haupt, M.
A1 - Hermann, G.
A1 - Hinton, J. A.
A1 - Hofmann, W.
A1 - Hoischen, Clemens
A1 - Holch, T. L.
A1 - Holler, M.
A1 - Horbe, M.
A1 - Horns, D.
A1 - Huber, D.
A1 - Jamrozy, M.
A1 - Jankowsky, D.
A1 - Jankowsky, F.
A1 - Jardin-Blicq, A.
A1 - Joshi, V.
A1 - Jung-Richardt, I.
A1 - Kasai, E.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Khangulyan, D.
A1 - Khelifi, B.
A1 - Klepser, S.
A1 - Kluzniak, W.
A1 - Komin, Nu.
A1 - Konno, R.
A1 - Kosack, K.
A1 - Kostunin, D.
A1 - Kreter, M.
A1 - Lamanna, G.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Levy, C.
A1 - Lohse, T.
A1 - Lypova, I.
A1 - Mackey, J.
A1 - Majumdar, J.
A1 - Malyshev, D.
A1 - Malyshev, D.
A1 - Marandon, V.
A1 - Marchegiani, P.
A1 - Marcowith, Alexandre
A1 - Mares, A.
A1 - Marti-Devesa, G.
A1 - Marx, R.
A1 - Maurin, G.
A1 - Meintjes, P. J.
A1 - Meyer, M.
A1 - Mitchell, A.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mohrmann, L.
A1 - Montanari, A.
A1 - Moore, C.
A1 - Morris, P.
A1 - Moulin, Emmanuel
A1 - Muller, J.
A1 - Murach, T.
A1 - Nakashima, K.
A1 - Nayerhoda, A.
A1 - de Naurois, M.
A1 - Ndiyavala, H.
A1 - Niederwanger, F.
A1 - Niemiec, J.
A1 - Oakes, L.
A1 - O'Brien, Patrick
A1 - Odaka, H.
A1 - Ohm, S.
A1 - Olivera-Nieto, L.
A1 - Wilhelmi, E. de Ona
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Panter, M.
A1 - Panny, S.
A1 - Parsons, R. D.
A1 - Peron, G.
A1 - Peyaud, B.
A1 - Piel, Q.
A1 - Pita, S.
A1 - Poireau, V.
A1 - Noel, A. Priyana
A1 - Prokhorov, D. A.
A1 - Prokoph, H.
A1 - Puhlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Rauth, R.
A1 - Reichherzer, P.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Remy, Q.
A1 - Renaud, M.
A1 - Rieger, F.
A1 - Rinchiuso, L.
A1 - Romoli, C.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Ruiz-Velasco, E.
A1 - Sahakian, V.
A1 - Sailer, S.
A1 - Sanchez, D. A.
A1 - Santangelo, Andrea
A1 - Sasaki, M.
A1 - Scalici, M.
A1 - Schussler, F.
A1 - Schutte, H. M.
A1 - Schwanke, U.
A1 - Schwemmer, S.
A1 - Seglar-Arroyo, M.
A1 - Senniappan, M.
A1 - Seyffert, A. S.
A1 - Shafi, N.
A1 - Shiningayamwe, K.
A1 - Simoni, R.
A1 - Sinha, A.
A1 - Sol, H.
A1 - Specovius, A.
A1 - Spencer, S.
A1 - Spir-Jacob, M.
A1 - Stawarz, L.
A1 - Sun, L.
A1 - Steenkamp, R.
A1 - Stegmann, C.
A1 - Steinmassl, S.
A1 - Steppa, C.
A1 - Takahashi, T.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tiziani, D.
A1 - Tluczykont, M.
A1 - Tomankova, L.
A1 - Trichard, C.
A1 - Tsirou, M.
A1 - Tuffs, R.
A1 - Uchiyama, Y.
A1 - van der Walt, D. J.
A1 - van Eldik, C.
A1 - van Rensburg, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Volk, H. J.
A1 - Vuillaume, T.
A1 - Wadiasingh, Z.
A1 - Wagner, S. J.
A1 - Watson, J.
A1 - Werner, F.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Wong, Yu Wun
A1 - Yusafzai, A.
A1 - Zacharias, M.
A1 - Zanin, R.
A1 - Zargaryan, D.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zhu, S. J.
A1 - Ziegler, A.
A1 - Zorn, J.
A1 - Zouari, S.
A1 - Zywucka, N.
T1 - An extreme particle accelerator in the Galactic plane
BT - HESS J1826-130
JF - Astronomy and astrophysics : an international weekly journal
N2 - The unidentified very-high-energy (VHE; E > 0.1 TeV) gamma -ray source, HESS J1826-130, was discovered with the High Energy Stereoscopic System (HESS) in the Galactic plane. The analysis of 215 h of HESS data has revealed a steady gamma -ray flux from HESS J1826-130, which appears extended with a half-width of 0.21 degrees +/- 0.02
(stat)degrees
stat degrees +/- 0.05
(sys)degrees sys degrees . The source spectrum is best fit with either a power-law function with a spectral index Gamma = 1.78 +/- 0.10(stat) +/- 0.20(sys) and an exponential cut-off at 15.2
(+5.5)(-3.2) -3.2+5.5 TeV, or a broken power-law with Gamma (1) = 1.96 +/- 0.06(stat) +/- 0.20(sys), Gamma (2) = 3.59 +/- 0.69(stat) +/- 0.20(sys) for energies below and above E-br = 11.2 +/- 2.7 TeV, respectively. The VHE flux from HESS J1826-130 is contaminated by the extended emission of the bright, nearby pulsar wind nebula, HESS J1825-137, particularly at the low end of the energy spectrum. Leptonic scenarios for the origin of HESS J1826-130 VHE emission related to PSR J1826-1256 are confronted by our spectral and morphological analysis. In a hadronic framework, taking into account the properties of dense gas regions surrounding HESS J1826-130, the source spectrum would imply an astrophysical object capable of accelerating the parent particle population up to greater than or similar to 200 TeV. Our results are also discussed in a multiwavelength context, accounting for both the presence of nearby supernova remnants, molecular clouds, and counterparts detected in radio, X-rays, and TeV energies.
KW - ISM: supernova remnants
KW - ISM: clouds
KW - gamma rays: general
KW - gamma rays:
KW - ISM
Y1 - 2020
U6 - https://doi.org/10.1051/0004-6361/202038851
SN - 0004-6361
SN - 1432-0746
VL - 644
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abramowski, A.
A1 - Aharonian, Felix A.
A1 - Benkhali, F. Ait
A1 - Akhperjanian, A. G.
A1 - Anguener, E. O.
A1 - Backes, M.
A1 - Balzer, A.
A1 - Becherini, Y.
A1 - Tjus, J. Becker
A1 - Berge, D.
A1 - Bernhard, S.
A1 - Bernloehr, K.
A1 - Birsin, E.
A1 - Blackwell, R.
A1 - Boettcher, M.
A1 - Boisson, C.
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Bregeon, J.
A1 - Brun, F.
A1 - Brun, P.
A1 - Bryan, M.
A1 - Bulik, T.
A1 - Carr, J.
A1 - Casanova, Sabrina
A1 - Chakraborty, N.
A1 - Chalme-Calvet, R.
A1 - Chaves, R. C. G.
A1 - Chen, A.
A1 - Chevalier, J.
A1 - Chretien, M.
A1 - Colafrancesco, S.
A1 - Cologna, G.
A1 - Condon, B.
A1 - Conrad, J.
A1 - Couturier, C.
A1 - Cui, Y.
A1 - Davids, I. D.
A1 - Degrange, B.
A1 - Deil, C.
A1 - deWilt, P.
A1 - Djannati-Atai, A.
A1 - Domainko, W.
A1 - Donath, A.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Dyrda, M.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Ernenwein, J. -P.
A1 - Espigat, P.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Feinstein, F.
A1 - Fernandes, M. V.
A1 - Fernandez, D.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Goyal, A.
A1 - Grondin, M. -H.
A1 - Grudzinska, M.
A1 - Hadasch, D.
A1 - Haeffner, S.
A1 - Hahn, J.
A1 - Hawkes, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hillert, A.
A1 - Hinton, J. A.
A1 - Hofmann, W.
A1 - Hofverberg, P.
A1 - Hoischen, Clemens
A1 - Holler, M.
A1 - Horns, D.
A1 - Ivascenko, A.
A1 - Jacholkowska, A.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, F.
A1 - Jung-Richardt, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kerszberg, D.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lau, J.
A1 - Lefaucheur, J.
A1 - Lefranc, V.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Lohse, T.
A1 - Lopatin, A.
A1 - Lorentz, M.
A1 - Lu, C. -C.
A1 - Lui, R.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Mariaud, C.
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - Meintjes, P. J.
A1 - Menzler, U.
A1 - Meyer, M.
A1 - Mitchell, A. M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - de Naurois, M.
A1 - Niemiec, J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Oettl, S.
A1 - Ohm, S.
A1 - Opitz, B.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Arribas, M. Paz
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Pita, S.
A1 - Poon, H.
A1 - Prokhorov, D.
A1 - Prokoph, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Reichardt, I.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Salek, D.
A1 - Sanchez, D. A.
A1 - Santangelo, Andrea
A1 - Sasaki, M.
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwemmer, S.
A1 - Seyffert, A. S.
A1 - Simoni, R.
A1 - Sol, H.
A1 - Spanier, F.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, I.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Tuffs, R.
A1 - Valerius, K.
A1 - van der Walt, J.
A1 - van Eldik, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voisin, F.
A1 - Voelk, H. J.
A1 - Vuillaume, T.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - Weidinger, M.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zabalza, V.
A1 - Zaborov, D.
A1 - Zacharias, M.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zefi, F.
A1 - Zywucka, N.
T1 - Detailed spectral and morphological analysis of the shell type supernova remnant RCW 86
JF - Astronomy and astrophysics : an international weekly journal
N2 - Aims. We aim for an understanding of the morphological and spectral properties of the supernova remnant RCW 86 and for insights into the production mechanism leading to the RCW 86 very high-energy gamma-ray emission. Methods. We analyzed High Energy Spectroscopic System (H.E.S.S.) data that had increased sensitivity compared to the observations presented in the RCW 86 H.E.S.S. discovery publication. Studies of the morphological correlation between the 0.5-1 keV X-ray band, the 2-5 keV X-ray band, radio, and gamma-ray emissions have been performed as well as broadband modeling of the spectral energy distribution with two different emission models. Results. We present the first conclusive evidence that the TeV gamma-ray emission region is shell-like based on our morphological studies. The comparison with 2-5 keV X-ray data reveals a correlation with the 0.4-50 TeV gamma-ray emission. The spectrum of RCW 86 is best described by a power law with an exponential cutoff at E-cut = (3.5 +/- 1.2(stat)) TeV and a spectral index of Gamma approximate to 1.6 +/- 0.2. A static leptonic one-zone model adequately describes the measured spectral energy distribution of RCW 86, with the resultant total kinetic energy of the electrons above 1 GeV being equivalent to similar to 0.1% of the initial kinetic energy of a Type Ia supernova explosion (10(51) erg). When using a hadronic model, a magnetic field of B approximate to 100 mu G is needed to represent the measured data. Although this is comparable to formerly published estimates, a standard E-2 spectrum for the proton distribution cannot describe the gamma-ray data. Instead, a spectral index of Gamma(p) approximate to 1.7 would be required, which implies that similar to 7 x 10(49)/n(cm-3) erg has been transferred into high-energy protons with the effective density n(cm-3) = n/1 cm(-3). This is about 10% of the kinetic energy of a typical Type Ia supernova under the assumption of a density of 1 cm(-3).
KW - astroparticle physics
KW - gamma rays: general
KW - ISM: supernova remnants
KW - cosmic rays
Y1 - 2018
U6 - https://doi.org/10.1051/0004-6361/201526545
SN - 1432-0746
VL - 612
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abdalla, Hassan E.
A1 - Abramowski, A.
A1 - Aharonian, Felix A.
A1 - Benkhali, F. Ait
A1 - Akhperjanian, A. G.
A1 - Andersson, T.
A1 - Anguener, E. O.
A1 - Arrieta, M.
A1 - Aubert, P.
A1 - Backes, M.
A1 - Balzer, A.
A1 - Barnard, M.
A1 - Becherini, Y.
A1 - Tjus, J. Becker
A1 - Berge, D.
A1 - Bernhard, S.
A1 - Bernloehr, K.
A1 - Blackwell, R.
A1 - Boettcher, M.
A1 - Boisson, C.
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Bregeon, J.
A1 - Brun, F.
A1 - Brun, P.
A1 - Bryan, M.
A1 - Bulik, T.
A1 - Capasso, M.
A1 - Carr, J.
A1 - Carrigan, S.
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chakraborty, N.
A1 - Chalme-Calvet, R.
A1 - Chaves, R. C. G.
A1 - Chen, A.
A1 - Chevalier, J.
A1 - Chretien, M.
A1 - Colafrancesco, S.
A1 - Cologna, G.
A1 - Condon, B.
A1 - Conrad, J.
A1 - Couturier, C.
A1 - Cui, Y.
A1 - Davids, I. D.
A1 - Degrange, B.
A1 - Deil, C.
A1 - Devin, J.
A1 - dewilt, P.
A1 - Dirson, L.
A1 - Djannati-Atai, A.
A1 - Domainko, W.
A1 - Donath, A.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Ernenwein, J. -P.
A1 - Eschbach, S.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Fernandes, M. V.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Funk, S.
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Goyal, A.
A1 - Grondin, M. -H.
A1 - Hadasch, D.
A1 - Hahn, J.
A1 - Haupt, M.
A1 - Hawkes, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hillert, A.
A1 - Hinton, J. A.
A1 - Hofmann, W.
A1 - Hoischen, Clemens
A1 - Holler, M.
A1 - Horns, D.
A1 - Ivascenko, A.
A1 - Jacholkowska, A.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, D.
A1 - Jankowsky, F.
A1 - Jingo, M.
A1 - Jogler, T.
A1 - Jouvin, L.
A1 - Jung-Richardt, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kerszberg, D.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - King, J.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Kraus, M.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lau, J.
A1 - Lees, J. -P.
A1 - Lefaucheur, J.
A1 - Lefranc, V.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Leser, Eva
A1 - Lohse, T.
A1 - Lorentz, M.
A1 - Liu, R.
A1 - Lopez-Coto, R.
A1 - Lypova, I.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Mariaud, C.
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - Meintjes, P. J.
A1 - Meyer, M.
A1 - Mitchell, A. M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mohrmann, L.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - de Naurois, M.
A1 - Niederwanger, F.
A1 - Niemiec, J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Oettl, S.
A1 - Ohm, S.
A1 - Wilhelmi, E. de Ona
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Padovani, M.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Arribas, M. Paz
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perennes, C.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Pita, S.
A1 - Poon, H.
A1 - Prokhorov, D.
A1 - Prokoph, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Salek, D.
A1 - Sanchez, D. A.
A1 - Santangelo, Andrea
A1 - Sasaki, M.
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwemmer, S.
A1 - Settimo, M.
A1 - Seyffert, A. S.
A1 - Shafi, N.
A1 - Shilon, I.
A1 - Simoni, R.
A1 - Sol, H.
A1 - Spanier, F.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, I.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tibaldo, L.
A1 - Tiziani, D.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Tuffs, R.
A1 - Uchiyama, Y.
A1 - Valerius, K.
A1 - van der Walt, D. J.
A1 - van Eldik, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voisin, F.
A1 - Voelk, H. J.
A1 - Vuillaume, T.
A1 - Wadiasingh, Z.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zabalza, V.
A1 - Zaborov, D.
A1 - Zacharias, M.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zefi, F.
A1 - Ziegler, A.
A1 - Zywucka, N.
T1 - The population of TeV pulsar wind nebulae in the HESS Galactic Plane Survey
JF - Astronomy and astrophysics : an international weekly journal
N2 - The nine-year H.E.S.S. Galactic Plane Survey (HGPS) has yielded the most uniform observation scan of the inner Milky Way in the TeV gamma-ray band to date. The sky maps and source catalogue of the HGPS allow for a systematic study of the population of TeV pulsar wind nebulae found throughout the last decade. To investigate the nature and evolution of pulsar wind nebulae, for the first time we also present several upper limits for regions around pulsars without a detected TeV wind nebula. Our data exhibit a correlation of TeV surface brightness with pulsar spindown power (E) over dot. This seems to be caused both by an increase of extension with decreasing (E) over dot, and hence with time, compatible with a power law R-PWN((E) over dot) similar to(E) over dot(0.65 +/- 0.20), and by a mild decrease of TeV gamma-ray luminosity with decreasing (E) over dot, compatible with L-1 (10 TeV) similar to (E) over dot(0.59 +/- 0.21). We also find that the off sets of pulsars with respect to the wind nebula centre with ages around 10 kyr are frequently larger than can be plausibly explained by pulsar proper motion and could be due to an asymmetric environment. In the present data, it seems that a large pulsar off set is correlated with a high apparent TeV efficiency L1- 10 TeV / (E) over dot. In addition to 14 HGPS sources considered firmly identified pulsar wind nebulae and 5 additional pulsar wind nebulae taken from literature, we find 10 HGPS sources that are likely TeV pulsar wind nebula candidates. Using a model that subsumes the present common understanding of the very high-energy radiative evolution of pulsar wind nebulae, we find that the trends and variations of the TeV observables and limits can be reproduced to a good level, drawing a consistent picture of present-day TeV data and theory.
KW - gamma rays: general
KW - catalogs
KW - surveys
KW - ISM: supernova remnants
KW - pulsars: general
Y1 - 2018
U6 - https://doi.org/10.1051/0004-6361/201629377
SN - 1432-0746
VL - 612
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abdalla, Hassan E.
A1 - Abramowski, A.
A1 - Aharonian, Felix A.
A1 - Benkhali, F. Ait
A1 - Akhperjanian, A. G.
A1 - Andersson, T.
A1 - Anguener, E. O.
A1 - Arakawa, M.
A1 - Arrieta, M.
A1 - Aubert, P.
A1 - Backes, M.
A1 - Balzer, A.
A1 - Barnard, M.
A1 - Becherini, Y.
A1 - Tjus, J. Becker
A1 - Berge, D.
A1 - Bernhard, S.
A1 - Bernloehr, K.
A1 - Blackwell, R.
A1 - Boettcher, M.
A1 - Boisson, C.
A1 - Bolmont, J.
A1 - Bonnefoy, S.
A1 - Bordas, Pol
A1 - Bregeon, J.
A1 - Brun, F.
A1 - Brun, P.
A1 - Bryan, M.
A1 - Buechele, M.
A1 - Bulik, T.
A1 - Capasso, M.
A1 - Carr, J.
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chakraborty, N.
A1 - Chaves, R. C. G.
A1 - Chen, A.
A1 - Chevalier, J.
A1 - Coffaro, M.
A1 - Colafrancesco, S.
A1 - Cologna, G.
A1 - Condon, B.
A1 - Conrad, J.
A1 - Cui, Y.
A1 - Davids, I. D.
A1 - Decock, J.
A1 - Degrange, B.
A1 - Deil, C.
A1 - Devin, J.
A1 - deWilt, P.
A1 - Dirson, L.
A1 - Djannati-Atai, A.
A1 - Domainko, W.
A1 - Donath, A.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Ernenwein, J. -P.
A1 - Eschbach, S.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Fernandes, M. V.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Funk, S.
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Goyal, A.
A1 - Grondin, M. -H.
A1 - Hahn, J.
A1 - Haupt, M.
A1 - Hawkes, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hinton, J. A.
A1 - Hofmann, W.
A1 - Hoischen, Clemens
A1 - Holch, T. L.
A1 - Holler, M.
A1 - Horns, D.
A1 - Ivascenko, A.
A1 - Iwasaki, H.
A1 - Jacholkowska, A.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, D.
A1 - Jankowsky, F.
A1 - Jingo, M.
A1 - Jogler, T.
A1 - Jouvin, L.
A1 - Jung-Richardt, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katsuragawa, M.
A1 - Katz, U.
A1 - Kerszberg, D.
A1 - Khangulyan, D.
A1 - Khelifi, B.
A1 - King, J.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Kraus, M.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lau, J.
A1 - Lees, J. -P.
A1 - Lefaucheur, J.
A1 - Lefranc, V.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Leser, Eva
A1 - Lohse, T.
A1 - Lorentz, M.
A1 - Liu, R.
A1 - Lopez-Coto, R.
A1 - Lypova, I.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Mariaud, C.
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - Meintjes, P. J.
A1 - Meyer, M.
A1 - Mitche, A. M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mohrmann, L.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - Nakashima, S.
A1 - de Naurois, M.
A1 - Niederwanger, F.
A1 - Niemiec, J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Oettl, S.
A1 - Ohm, S.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Padovani, M.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perennes, C.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Piel, Q.
A1 - Pita, S.
A1 - Poon, H.
A1 - Prokhorov, D.
A1 - Prokoph, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Richter, S.
A1 - Rieger, F.
A1 - Romoli, C.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Saito, S.
A1 - Salek, D.
A1 - Sanchez, D. A.
A1 - Santangelo, Andrea
A1 - Sasaki, M.
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwemmer, S.
A1 - Seglar-Arroyo, M.
A1 - Settimo, M.
A1 - Seyffert, A. S.
A1 - Shafi, N.
A1 - Shilon, I.
A1 - Simoni, R.
A1 - Sol, H.
A1 - Spanier, F.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stycz, K.
A1 - Sushch, I.
A1 - Takahashi, T.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tibaldo, L.
A1 - Tiziani, D.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Tsuji, N.
A1 - Tuffs, R.
A1 - Uchiyama, Y.
A1 - van der Wale, D. J.
A1 - van Eldik, C.
A1 - van Rensburg, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voisin, F.
A1 - Voelk, H. J.
A1 - Vuillaume, T.
A1 - Wadiasingh, Z.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zabalza, V.
A1 - Zaborov, D.
A1 - Zacharias, M.
A1 - Zanin, R.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zefi, F.
A1 - Ziegler, A.
A1 - Zywucka, N.
A1 - Bamba, A.
A1 - Fukui, Y.
A1 - Sano, H.
A1 - Yoshiike, S.
T1 - A search for new supernova remnant shells in the Galactic plane with HESS
JF - Astronomy and astrophysics : an international weekly journal
N2 - A search for new supernova remnants (SNRs) has been conducted using TeV gamma-ray data from the H.E.S.S. Galactic plane survey. As an identification criterion, shell morphologies that are characteristic for known resolved TeV SNRs have been used. Three new SNR candidates were identified in the H.E.S.S. data set with this method. Extensive multiwavelength searches for counterparts were conducted. A radio SNR candidate has been identified to be a counterpart to HESS J1534-571. The TeV source is therefore classified as a SNR. For the other two sources, HESS J1614-518 and HESS J1912 + 101, no identifying counterparts have been found, thus they remain SNR candidates for the time being. TeV-emitting SNRs are key objects in the context of identifying the accelerators of Galactic cosmic rays. The TeV emission of the relativistic particles in the new sources is examined in view of possible leptonic and hadronic emission scenarios, taking the current multiwavelength knowledge into account.
KW - astroparticle physics
KW - ISM: supernova remnants
KW - cosmic rays
Y1 - 2018
U6 - https://doi.org/10.1051/0004-6361/201730737
SN - 1432-0746
VL - 612
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abdalla, Hassan E.
A1 - Abramowski, A.
A1 - Aharonian, Felix A.
A1 - Benkhali, F. Ait
A1 - Anguener, E. O.
A1 - Arakawa, M.
A1 - Arrieta, M.
A1 - Aubert, P.
A1 - Backes, M.
A1 - Balzer, A.
A1 - Barnard, M.
A1 - Becherini, Y.
A1 - Tjus, J. Becker
A1 - Berge, D.
A1 - Bernhard, S.
A1 - Bernloehr, K.
A1 - Blackwell, R.
A1 - Boettcher, M.
A1 - Boisson, C.
A1 - Bolmont, J.
A1 - Bonnefoy, S.
A1 - Bordas, Pol
A1 - Bregeon, J.
A1 - Brun, F.
A1 - Brun, P.
A1 - Bryan, M.
A1 - Buechele, M.
A1 - Bulik, T.
A1 - Capasso, M.
A1 - Caroff, S.
A1 - Carosi, A.
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chakraborty, N.
A1 - Chaves, R. C. G.
A1 - Chen, A.
A1 - Chevalier, J.
A1 - Colafrancesco, S.
A1 - Condon, B.
A1 - Conrad, J.
A1 - Davids, I. D.
A1 - Decock, J.
A1 - Deil, C.
A1 - Devin, J.
A1 - deWilt, P.
A1 - Dirson, L.
A1 - Djannati-Atai, A.
A1 - Donath, A.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Emery, G.
A1 - Ernenwein, J. -P.
A1 - Eschbach, S.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Fernandes, M. V.
A1 - Fernandez, D.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Funk, S.
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Gate, F.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glawion, D.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Grondin, M. -H.
A1 - Hahn, J.
A1 - Haupt, M.
A1 - Hawkes, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hinton, J. A.
A1 - Hofmann, W.
A1 - Hoischen, Clemens
A1 - Holch, T. L.
A1 - Holler, M.
A1 - Horns, D.
A1 - Ivascenko, A.
A1 - Iwasaki, H.
A1 - Jacholkowska, A.
A1 - Jamrozy, M.
A1 - Jankowsky, D.
A1 - Jankowsky, F.
A1 - Jingo, M.
A1 - Jouvin, L.
A1 - Jung-Richardt, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katsuragawa, M.
A1 - Katz, U.
A1 - Kerszberg, D.
A1 - Khangulyan, D.
A1 - Khelifi, B.
A1 - King, J.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Kraus, M.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lau, J.
A1 - Lees, J. -P.
A1 - Lefaucheur, J.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Leser, Eva
A1 - Lohse, T.
A1 - Lorentz, M.
A1 - Liu, R.
A1 - Lopez-Coto, R.
A1 - Lypova, I.
A1 - Malyshev, D.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Mariaud, C.
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - Meintjes, P. J.
A1 - Meyer, M.
A1 - Mitchell, A. M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mohrmann, L.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - Nakashima, S.
A1 - de Naurois, M.
A1 - Ndiyavala, H.
A1 - Niederwanger, F.
A1 - Niemiec, J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Ohm, S.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Padovani, M.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perennes, C.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Piel, Q.
A1 - Pita, S.
A1 - Poireau, V.
A1 - Poon, H.
A1 - Prokhorov, D.
A1 - Prokoph, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Rauth, R.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Rinchiuso, L.
A1 - Romoli, C.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Safi-Harb, S.
A1 - Sahakian, V.
A1 - Saito, S.
A1 - Sanchez, D. A.
A1 - Santangelo, Andrea
A1 - Sasaki, M.
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwemmer, S.
A1 - Seglar-Arroyo, M.
A1 - Settimo, M.
A1 - Seyffert, A. S.
A1 - Shafi, N.
A1 - Shilon, I.
A1 - Shiningayamwe, K.
A1 - Simoni, R.
A1 - Sol, H.
A1 - Spanier, F.
A1 - Spir-Jacob, M.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Steppa, Constantin Beverly
A1 - Sushch, I.
A1 - Takahashi, T.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tibaldo, L.
A1 - Tiziani, D.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Tsirou, M.
A1 - Tsuji, N.
A1 - Tuffs, R.
A1 - Uchiyama, Y.
A1 - van der Walt, D. J.
A1 - van Eldik, C.
A1 - van Rensburg, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voisin, F.
A1 - Voelk, H. J.
A1 - Vuillaume, T.
A1 - Wadiasingh, Z.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zaborov, D.
A1 - Zacharias, M.
A1 - Zanin, R.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zefi, F.
A1 - Ziegler, A.
A1 - Zorn, J.
A1 - Zywucka, N.
T1 - Population study of Galactic supernova remnants at very high gamma-ray energies with HESS
JF - Astronomy and astrophysics : an international weekly journal
N2 - Shell-type supernova remnants (SNRs) are considered prime candidates for the acceleration of Galactic cosmic rays (CRs) up to the knee of the CR spectrum at E approximate to 3 x 10(15) eV. Our MilkyWay galaxy hosts more than 350 SNRs discovered at radio wavelengths and at high energies, of which 220 fall into the H.E.S.S. Galactic Plane Survey (HGPS) region. Of those, only 50 SNRs are coincident with a H.E.S.S source and in 8 cases the very high-energy (VHE) emission is firmly identified as an SNR. The H.E.S.S. GPS provides us with a legacy for SNR population study in VHE gamma-rays and we use this rich data set to extract VHE flux upper limits from all undetected SNRs. Overall, the derived flux upper limits are not in contradiction with the canonical CR paradigm. Assuming this paradigm holds true, we can constrain typical ambient density values around shell-type SNRs to n <= 7 cm(-3) and electron-to-proton energy fractions above 10 TeV to epsilon(ep) <= 5 x 10(-3). Furthermore, comparisons of VHE with radio luminosities in non-interacting SNRs reveal a behaviour that is in agreement with the theory of magnetic field amplification at shell-type SNRs.
KW - gamma rays: general
KW - ISM: supernova remnants
Y1 - 2018
U6 - https://doi.org/10.1051/0004-6361/201732125
SN - 1432-0746
VL - 612
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abdalla, Hassan E.
A1 - Abramowski, A.
A1 - Aharonian, Felix A.
A1 - Benkhali, F. Ait
A1 - Akhperjanian, A. G.
A1 - Andersson, T.
A1 - Anguener, E. O.
A1 - Arakawa, M.
A1 - Arrieta, M.
A1 - Aubert, P.
A1 - Backes, M.
A1 - Balzer, A.
A1 - Barnard, M.
A1 - Becherini, Y.
A1 - Tjus, J. Becker
A1 - Berge, D.
A1 - Bernhard, S.
A1 - Bernloehr, K.
A1 - Blackwell, R.
A1 - Boettcher, M.
A1 - Boisson, C.
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Bregeon, J.
A1 - Brun, F.
A1 - Brun, P.
A1 - Bryan, M.
A1 - Bilchele, M.
A1 - Bulik, T.
A1 - Capasso, M.
A1 - Carr, J.
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chakraborty, N.
A1 - Chalme-Calvet, R.
A1 - Chaves, R. C. G.
A1 - Chen, A.
A1 - Chevalier, J.
A1 - Chretien, M.
A1 - Coffaro, M.
A1 - Colafrancesco, S.
A1 - Cologna, G.
A1 - Condon, B.
A1 - Conrad, J.
A1 - Cui, Y.
A1 - Davids, I. D.
A1 - Decock, J.
A1 - Degrange, B.
A1 - Deil, C.
A1 - Devin, J.
A1 - deWilt, P.
A1 - Dirson, L.
A1 - Djannati-Atai, A.
A1 - Domainko, W.
A1 - Donath, A.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Ernenwein, J. -P.
A1 - Eschbach, S.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Fernandes, M. V.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Funk, S.
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Goya, A.
A1 - Grondin, M. -H.
A1 - Hahn, J.
A1 - Haupt, M.
A1 - Hawkes, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hinton, J. A.
A1 - Hofmann, W.
A1 - Hoischen, Clemens
A1 - Holler, M.
A1 - Horns, D.
A1 - Ivascenko, A.
A1 - Iwasaki, H.
A1 - Jacholkowska, A.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, D.
A1 - Jankowsky, F.
A1 - Jingo, M.
A1 - Jogler, T.
A1 - Jouvin, L.
A1 - Jung-Richardt, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katsuragawa, M.
A1 - Katz, U.
A1 - Kerszberg, D.
A1 - Khangulyan, D.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - King, J.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Kraus, M.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lau, J.
A1 - Lees, J. -P.
A1 - Lefaucheur, J.
A1 - Lefranc, V.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Leser, Eva
A1 - Lohse, T.
A1 - Lorentz, M.
A1 - Liu, R.
A1 - Lopez-Coto, R.
A1 - Lypova, I.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Mariaud, C.
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - Meintjes, P. J.
A1 - Meyer, M.
A1 - Mitche, A. M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mohrmann, L.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - Nakashima, S.
A1 - de Naurois, M.
A1 - Niederwanger, F.
A1 - Niemiec, J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Oettl, S.
A1 - Ohm, S.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Padovani, M.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Arribas, M. Paz
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perennes, C.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Piel, Q.
A1 - Pita, S.
A1 - Poon, H.
A1 - Prokhorov, D.
A1 - Prokoph, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Richter, S.
A1 - Rieger, F.
A1 - Romoli, C.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Saito, S.
A1 - Salek, D.
A1 - Sanchez, D. A.
A1 - Santangelo, Andrea
A1 - Sasaki, M.
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwemmer, S.
A1 - Seglar-Arroyo, M.
A1 - Settimo, M.
A1 - Seyffert, A. S.
A1 - Shafi, N.
A1 - Shilon, I.
A1 - Simoni, R.
A1 - Sol, H.
A1 - Spanier, F.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stycz, K.
A1 - Sushch, I.
A1 - Takahashi, T.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tibaldo, L.
A1 - Tiziani, D.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Tsuji, N.
A1 - Tuffs, R.
A1 - Uchiyama, Y.
A1 - van der Walt, D. J.
A1 - van Eldik, C.
A1 - van Rensburg, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voisin, F.
A1 - Voelk, H. J.
A1 - Vuillaume, T.
A1 - Wadiasingh, Z.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zabalza, V.
A1 - Zaborov, D.
A1 - Zacharias, M.
A1 - Zanin, R.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zefi, F.
A1 - Ziegler, A.
A1 - Zywucka, N.
T1 - Deeper HESS observations of Vela Junior (RX J0852.0-4622)
BT - Morphology studies and resolved spectroscopy
JF - Astronomy and astrophysics : an international weekly journal
N2 - Aims. We study gamma-ray emission from the shell-type supernova remnant (SNR) RXJ0852.0-4622 to better characterize its spectral properties and its distribution over the SNR. Methods. The analysis of an extended High Energy Spectroscopic System (H.E.S.S.) data set at very high energies (E > 100 GeV) permits detailed studies, as well as spatially resolved spectroscopy, of the morphology and spectrum of the whole RXJ0852.0-4622 region. The H.E.S.S. data are combined with archival data from other wavebands and interpreted in the framework of leptonic and hadronic models. The joint Fermi-LAT-H.E.S.S. spectrum allows the direct determination of the spectral characteristics of the parent particle population in leptonic and hadronic scenarios using only GeV-TeV data. Results. An updated analysis of the H.E.S.S. data shows that the spectrum of the entire SNR connects smoothly to the high-energy spectrum measured by Fermi-LAT. The increased data set makes it possible to demonstrate that the H.E.S.S. spectrum deviates significantly from a power law and is well described by both a curved power law and a power law with an exponential cutoff at an energy of E-cut = (6.7 +/- 1.2(stat) +/- 1.2(syst)) TeV. The joint Fermi-LAT-H.E.S.S. spectrum allows the unambiguous identification of the spectral shape as a power law with an exponential cutoff. No significant evidence is found for a variation of the spectral parameters across the SNR, suggesting similar conditions of particle acceleration across the remnant. A simple modeling using one particle population to model the SNR emission demonstrates that both leptonic and hadronic emission scenarios remain plausible. It is also shown that at least a part of the shell emission is likely due to the presence of a pulsar wind nebula around PSR J0855-4644.
KW - astroparticle physics
KW - gamma rays: general
KW - acceleration of particles
KW - cosmic rays
KW - ISM: supernova remnants
Y1 - 2018
U6 - https://doi.org/10.1051/0004-6361/201630002
SN - 1432-0746
VL - 612
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abdalla, Hassan E.
A1 - Abramowski, A.
A1 - Aharonian, Felix A.
A1 - Benkhali, F. Ait
A1 - Akhperjanian, A. G.
A1 - Andersson, T.
A1 - Anguener, O.
A1 - Arrieta, M.
A1 - Aubert, P.
A1 - Backes, M.
A1 - Balzer, A.
A1 - Barnard, M.
A1 - Becherini, Y.
A1 - Tjus, J. Becker
A1 - Berge, D.
A1 - Bernhard, S.
A1 - Bernloehr, K.
A1 - Blackwell, R.
A1 - Boettcher, M.
A1 - Boisson, C.
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Bregeon, J.
A1 - Brun, F.
A1 - Brun, P.
A1 - Bryan, M.
A1 - Bulik, T.
A1 - Capasso, M.
A1 - Carr, J.
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chakraborty, N.
A1 - Chalme-Calvet, R.
A1 - Chaves, R. C. G.
A1 - Chen, A.
A1 - Chevalier, J.
A1 - Chretien, M.
A1 - Colafrancesco, S.
A1 - Cologna, G.
A1 - Condon, B.
A1 - Conrad, J.
A1 - Cui, Y.
A1 - Davids, I. D.
A1 - Decock, J.
A1 - Degrange, B.
A1 - Deil, C.
A1 - Devin, J.
A1 - deWilt, P.
A1 - Dirson, L.
A1 - Djannati-Atai, A.
A1 - Domainko, W.
A1 - Donath, A.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Ernenwein, J. -P.
A1 - Eschbach, S.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Fernandes, M. V.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Funk, S.
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Goyal, A.
A1 - Grondin, M. -H.
A1 - Hadasch, D.
A1 - Hahn, J.
A1 - Haupt, M.
A1 - Hawkes, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hinton, J. A.
A1 - Hofmann, W.
A1 - Hoischen, Clemens
A1 - Holler, M.
A1 - Horns, D.
A1 - Ivascenko, A.
A1 - Jacholkowska, A.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, D.
A1 - Jankowsky, F.
A1 - Jingo, M.
A1 - Jogler, T.
A1 - Jouvin, L.
A1 - Jung-Richardt, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kerszberg, D.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - King, J.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Kraus, M.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lau, J.
A1 - Lees, J. -P.
A1 - Lefaucheur, J.
A1 - Lefranc, V.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Leser, Eva
A1 - Lohse, T.
A1 - Lorentz, M.
A1 - Liu, R.
A1 - Lopez-Coto, R.
A1 - Lypova, I.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Mariaud, C.
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - Meintjes, P. J.
A1 - Meyer, M.
A1 - Mitchell, A. M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mohrmann, L.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - de Naurois, M.
A1 - Niederwanger, F.
A1 - Niemiec, J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Oettl, S.
A1 - Ohm, S.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Padovani, M.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perennes, C.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Piel, Q.
A1 - Pita, S.
A1 - Poon, H.
A1 - Prokhorov, D.
A1 - Prokoph, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Salek, D.
A1 - Sanchez, D. A.
A1 - Santangelo, Andrea
A1 - Sasaki, M.
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwemmer, S.
A1 - Settimo, M.
A1 - Seyffert, A. S.
A1 - Shafi, N.
A1 - Shilon, I.
A1 - Simoni, R.
A1 - Sol, H.
A1 - Spanier, F.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, I.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tibaldo, L.
A1 - Tiziani, D.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Tuffs, R.
A1 - Uchiyama, Y.
A1 - van der Walt, D. J.
A1 - van Eldik, C.
A1 - van Rensburg, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voisin, F.
A1 - Voelk, H. J.
A1 - Vuillaume, T.
A1 - Wadiasingh, Z.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zabalza, V.
A1 - Zaborov, D.
A1 - Zacharias, M.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zefi, F.
A1 - Ziegler, A.
A1 - Zywucka, N.
A1 - Katsuta, J.
T1 - The supernova remnant W49B as seen with HESS and Fermi-LAT
JF - Astronomy and astrophysics : an international weekly journal
N2 - The supernova remnant (SNR) W49B originated from a core-collapse supernova that occurred between one and four thousand years ago, and subsequently evolved into a mixed-morphology remnant, which is interacting with molecular clouds (MC). Gamma-ray observations of SNR-MC associations are a powerful tool to constrain the origin of Galactic cosmic rays, as they can probe the acceleration of hadrons through their interaction with the surrounding medium and subsequent emission of non-thermal photons. We report the detection of a gamma-ray source coincident with W49B at very high energies (VHE; E > 100 GeV) with the H.E.S.S. Cherenkov telescopes together with a study of the source with five years of Fermi-LAT high-energy gamma-ray (0.06-300 GeV) data. The smoothly connected, combined source spectrum, measured from 60 MeV to multi-TeV energies, shows two significant spectral breaks at 304 +/- 20 MeV and 8.4(-2.5)(+2.5) GeV; the latter is constrained by the joint fit from the two instruments. The detected spectral features are similar to those observed in several other SNR-MC associations and are found to be indicative of gamma-ray emission produced through neutral-pion decay.
KW - gamma rays: general
KW - ISM: supernova remnants
KW - ISM: clouds
Y1 - 2018
U6 - https://doi.org/10.1051/0004-6361/201527843
SN - 1432-0746
VL - 612
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abdalla, Hassan E.
A1 - Abramowski, A.
A1 - Aharonian, Felix A.
A1 - Benkhali, F. Ait
A1 - Akhperjanian, A. G.
A1 - Andersson, T.
A1 - Anguener, E. O.
A1 - Arrieta, M.
A1 - Aubert, P.
A1 - Backes, M.
A1 - Balzer, A.
A1 - Barnard, M.
A1 - Becherini, Y.
A1 - Tjus, J. Becker
A1 - Berge, D.
A1 - Bernhard, S.
A1 - Bernloehr, K.
A1 - Blackwell, R.
A1 - Boettcher, M.
A1 - Boisson, C.
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Bregeon, J.
A1 - Brun, F.
A1 - Brun, P.
A1 - Bryan, M.
A1 - Bulik, T.
A1 - Capasso, M.
A1 - Carr, J.
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chakraborty, N.
A1 - Chalme-Calvet, R.
A1 - Chaves, R. C. G.
A1 - Chen, A.
A1 - Chevalier, J.
A1 - Chretien, M.
A1 - Colafrancesco, S.
A1 - Cologna, G.
A1 - Condon, B.
A1 - Conrad, J.
A1 - Cui, Y.
A1 - Davids, I. D.
A1 - Decock, J.
A1 - Degrange, B.
A1 - Dei, C.
A1 - Devin, J.
A1 - deWilt, P.
A1 - Dirson, L.
A1 - Djannati-Atai, A.
A1 - Domainko, W.
A1 - Donath, A.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Ernenwein, J. -P.
A1 - Eschbach, S.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Fernandes, M. V.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Fukuyama, T.
A1 - Funk, S.
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Goyal, A.
A1 - Grondin, M. -H.
A1 - Hadasch, D.
A1 - Hahn, J.
A1 - Haupt, M.
A1 - Hawkes, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hinton, J. A.
A1 - Hofmann, W.
A1 - Hoischen, Clemens
A1 - Holler, M.
A1 - Horns, D.
A1 - Ivascenko, A.
A1 - Jacholkowska, A.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, D.
A1 - Jankowsky, F.
A1 - Jingo, M.
A1 - Jogler, T.
A1 - Jouvin, L.
A1 - Jung-Richardt, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kerszberg, D.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - King, J.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Kraus, M.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lau, J.
A1 - Lees, J. -P.
A1 - Lefaucheur, J.
A1 - Lefranc, V.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Leser, Eva
A1 - Lohse, T.
A1 - Lorentz, M.
A1 - Liu, R.
A1 - Lopez-Coto, R.
A1 - Lypova, I.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Mariaud, C.
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - Meintjes, P. J.
A1 - Meyer, M.
A1 - Mitchell, A. M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mohrmann, L.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - de Naurois, M.
A1 - Niederwanger, F.
A1 - Niemiec, J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Oettl, S.
A1 - Ohm, S.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Padovani, M.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perennes, C.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Piel, Q.
A1 - Pita, S.
A1 - Poon, H.
A1 - Prokhorov, D.
A1 - Prokoph, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Salek, D.
A1 - Sanchez, D. A.
A1 - Santangelo, Andrea
A1 - Sasaki, M.
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwemmer, S.
A1 - Settimo, M.
A1 - Seyffert, A. S.
A1 - Shafi, N.
A1 - Shilon, I.
A1 - Simoni, R.
A1 - Sol, H.
A1 - Spanie, F.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, I.
A1 - Takahashi, T.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tibaldo, L.
A1 - Tiziani, D.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Tuffs, R.
A1 - Uchiyama, Y.
A1 - van der Walt, D. J.
A1 - van Edik, C.
A1 - van Rensburg, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voisin, F.
A1 - Voelk, H. J.
A1 - Volpe, F.
A1 - Vuillaume, T.
A1 - Wadiasingh, Z.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zabalza, V.
A1 - Zaborov, D.
A1 - Zacharias, M.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zefi, F.
A1 - Ziegler, A.
A1 - Zywucka, N.
T1 - HESS observations of RX J1713.7-3946 with improved angular and spectral resolution
BT - Evidence for gamma-ray emission extending beyond the X-ray emitting shell
JF - Astronomy and astrophysics : an international weekly journal
KW - acceleration of particles
KW - cosmic rays
KW - ISM: supernova remnants
KW - gamma rays: general
KW - astroparticle physic
Y1 - 2018
U6 - https://doi.org/10.1051/0004-6361/201629790
SN - 1432-0746
VL - 612
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abeysekara, A. U.
A1 - Archer, A.
A1 - Aune, Taylor
A1 - Benbow, Wystan
A1 - Bird, Ralph
A1 - Brose, Robert
A1 - Buchovecky, M.
A1 - Bugaev, V.
A1 - Cui, Wei
A1 - Daniel, M. K.
A1 - Falcone, A.
A1 - Feng, Qi
A1 - Finley, John P.
A1 - Fleischhack, H.
A1 - Flinders, A.
A1 - Fortson, L.
A1 - Furniss, Amy
A1 - Gotthelf, Eric V.
A1 - Grube, J.
A1 - Hanna, David
A1 - Hervet, O.
A1 - Holder, J.
A1 - Huang, K.
A1 - Hughes, G.
A1 - Humensky, T. B.
A1 - Huetten, M.
A1 - Johnson, Caitlin A.
A1 - Kaaret, Philip
A1 - Kar, P.
A1 - Kelley-Hoskins, N.
A1 - Kertzman, M.
A1 - Kieda, David
A1 - Krause, Maria
A1 - Kumar, S.
A1 - Lang, M. J.
A1 - Lin, T. T. Y.
A1 - Maier, Gernot
A1 - McArthur, S.
A1 - Moriarty, P.
A1 - Mukherjee, Reshmi
A1 - Ong, R. A.
A1 - Otte, Adam Nepomuk
A1 - Pandel, Dirk
A1 - Park, Nahee
A1 - Petrashyk, A.
A1 - Pohl, Martin
A1 - Popkow, Alexis
A1 - Pueschel, Elisa
A1 - Quinn, J.
A1 - Ragan, K.
A1 - Reynolds, P. T.
A1 - Richards, Gregory T.
A1 - Roache, E.
A1 - Rousselle, J.
A1 - Rulten, C.
A1 - Sadeh, I.
A1 - Santander, M.
A1 - Sembroski, G. H.
A1 - Shahinyan, Karlen
A1 - Tyler, J.
A1 - Vassiliev, V. V.
A1 - Wakely, S. P.
A1 - Ward, J. E.
A1 - Weinstein, A.
A1 - Wells, R. M.
A1 - Wilcox, P.
A1 - Wilhelm, Alina
A1 - Williams, David A.
A1 - Zitzer, B.
T1 - A Very High Energy gamma-Ray Survey toward the Cygnus Region of the Galaxy
JF - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2 - We present results from deep observations toward the Cygnus region using 300 hr of very high energy (VHE)gamma-ray data taken with the VERITAS Cerenkov telescope array and over 7 yr of high-energy.-ray data taken with the Fermi satellite at an energy above 1 GeV. As the brightest region of diffuse gamma-ray emission in the northern sky, the Cygnus region provides a promising area to probe the origins of cosmic rays. We report the identification of a potential Fermi-LAT counterpart to VER J2031+415 (TeV J2032+4130) and resolve the extended VHE source VER J2019+368 into two source candidates (VER J2018+367* and VER J2020+368*) and characterize their energy spectra. The Fermi-LAT morphology of 3FGL J2021.0+4031e (the Gamma Cygni supernova remnant) was examined, and a region of enhanced emission coincident with VER J2019+407 was identified and jointly fit with the VERITAS data. By modeling 3FGL J2015.6+3709 as two sources, one located at the location of the pulsar wind nebula CTB 87 and one at the quasar QSO J2015+371, a continuous spectrum from 1 GeV to 10 TeV was extracted for VER J2016+371 (CTB 87). An additional 71 locations coincident with Fermi-LAT sources and other potential objects of interest were tested for VHE gamma-ray emission, with no emission detected and upper limits on the differential flux placed at an average of 2.3% of the Crab Nebula flux. We interpret these observations in a multiwavelength context and present the most detailed gamma-ray view of the region to date.
KW - acceleration of particles
KW - cosmic rays
KW - gamma rays: general
KW - ISM: supernova remnants
Y1 - 2018
U6 - https://doi.org/10.3847/1538-4357/aac4a2
SN - 0004-637X
SN - 1538-4357
VL - 861
IS - 2
PB - IOP Publ. Ltd.
CY - Bristol
ER -
TY - JOUR
A1 - Petruk, Oleh
A1 - Kuzyo, T.
A1 - Orlando, S.
A1 - Pohl, Martin
A1 - Miceli, M.
A1 - Bocchino, F.
A1 - Beshley, V.
A1 - Brose, Robert
T1 - Post-adiabatic supernova remnants in an interstellar magnetic field
BT - oblique shocks and non-uniform environment
JF - Monthly notices of the Royal Astronomical Society
N2 - We present very-high-resolution 1D MHD simulations of the late-stage supernova remnants (SNRs). In the post-adiabatic stage, the magnetic field has an important and significant dynamical effect on the shock dynamics, the flow structure, and hence the acceleration and emission of cosmic rays. We find that the tangential component of the magnetic field provides pressure support that to a fair degree prevents the collapse of the radiative shell and thus limits the total compression ratio of the partially or fully radiative forward shock. A consequence is that the spectra of cosmic rays would not be as hard as in hydrodynamic simulations. We also investigated the effect on the flow profiles of the magnetic-field inclination and a large-scale gradient in the gas density and/or the magnetic field. A positive density gradient shortens the evolutionary stages, whereas a shock obliquity lowers the shock compression. The compression of the tangential component of the magnetic field leads to its dominance in the downstream region of post-adiabatic shocks for a wide range of orientation of the upstream field, which may explain why one preferentially observes tangential radio polarization in old SNRs. As most cosmic rays are produced at late stages of SNR evolution, the post-adiabatic phase and the influence of the magnetic field during it are most important for modeling the cosmic-ray acceleration at old SNRs and the gamma-ray emission from late-stage SNRs interacting with clouds.
KW - shock waves
KW - ISM: magnetic fields
KW - ISM: supernova remnants
Y1 - 2018
U6 - https://doi.org/10.1093/mnras/sty1750
SN - 0035-8711
SN - 1365-2966
VL - 479
IS - 3
SP - 4253
EP - 4270
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Sushch, Iurii
A1 - Brose, Robert
A1 - Pohl, Martin
T1 - Modeling of the spatially resolved nonthermal emission from the Vela Jr. supernova remnant
JF - Astronomy and astrophysics : an international weekly journal
N2 - Vela Jr. (RX J0852.0-4622) is one of just a few known supernova remnants (SNRs) with a resolved shell across the whole electromagnetic spectrum from radio to very-high-energy (>100 GeV; VHE) gamma-rays. Its proximity and large size allow for detailed spatially resolved observations of the source, making Vela Jr. one of the primary sources used for the study of particle acceleration and emission mechanisms in SNRs. High-resolution X-ray observations reveal a steepening of the spectrum toward the interior of the remnant. In this study we aim for a self-consistent radiation model of Vela Jr. which at the same time would explain the broadband emission from the source and its intensity distribution. We solve the full particle transport equation combined with the high-resolution one-dimensional (1D) hydrodynamic simulations (using Pluto code) and subsequently calculate the radiation from the remnant. The equations are solved in the test particle regime. We test two models for the magnetic field profile downstream of the shock: damped magnetic field, which accounts for the damping of strong magnetic turbulence downstream, and transported magnetic field. Neither of these scenarios can fully explain the observed radial dependence of the X-ray spectrum under spherical symmetry. We show, however, that the softening of the spectrum and the X-ray intensity profile can be explained under the assumption that the emission is enhanced within a cone.
KW - radiation mechanisms: non-thermal
KW - acceleration of particles
KW - cosmic rays
KW - ISM: supernova remnants
KW - X-rays: individuals: Vela Jr (RX J08520-4622)
KW - shock waves
Y1 - 2018
U6 - https://doi.org/10.1051/0004-6361/201832879
SN - 1432-0746
SN - 0004-6361
VL - 618
PB - EDP Sciences
CY - Les Ulis
ER -
TY - GEN
A1 - Petruk, Oleh
A1 - Kuzyo, T.
A1 - Orlando, S.
A1 - Pohl, Martin
A1 - Miceli, M.
A1 - Bocchino, F.
A1 - Beshley, V.
A1 - Brose, Robert
T1 - Erratum: Post-adiabatic supernova remnants in an interstellar magnetic field: oblique shocks and non-uniform environment. - (Monthly notices of the Royal Astronomical Society. - 479, (2018), pg. 4253 - 4270)
T2 - Monthly notices of the Royal Astronomical Society
N2 - This is a correction notice for ‘Post-adiabatic supernova remnants in an interstellar magnetic field: oblique shocks and non-uniform environment’ (DOI: https://doi.org/10.1093/mnras/sty1750), which was published in MNRAS 479, 4253–4270 (2018). The publisher regrets to inform that the colour was missing from the colour scales in Figs 8(a)–(d) and Figs 9(a) and (b). This has now been corrected online. The publisher apologizes for this error.
KW - errata
KW - addenda
KW - shock waves
KW - ISM: magnetic fields
KW - ISM: supernova remnants
Y1 - 2018
U6 - https://doi.org/10.1093/mnras/sty2861
SN - 0035-8711
SN - 1365-2966
VL - 482
IS - 2
SP - 1979
EP - 1980
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Gvaramadze, V. V.
A1 - Kniazev, Alexei Y.
A1 - Oskinova, Lidia M.
T1 - Discovery of a putative supernova remnant around the long-period X-ray pulsar SXP 1323 in the Small Magellanic Cloud
JF - Monthly notices of the Royal Astronomical Society
N2 - We report the discovery of a circular shell centred on the Be X-ray binary (BeXB) SXP 1323 in the Small Magellanic Cloud. The shell was detected in an H α image obtained with the Very Large Telescope. Follow-up spectroscopy with the Southern African Large Telescope showed that the shell expands with a velocity of ≈100kms−1 and that its emission is due to shock excitation. We suggest that this shell is a remnant of the supernova explosion that led to the formation of SXP 1323’s neutron star ≈40000 yr ago. SXP 1323 represents the second known case of a BeXB associated with a supernova remnant (the first one is SXP 1062). Interestingly, both of these BeXBs harbour long-period pulsars and are located in a low-metallicity galaxy.
KW - stars: emission-line, Be
KW - stars: individual: [MA93] 1393
KW - stars: massive
KW - ISM: supernova remnants
KW - X-rays: binaries
KW - X-rays: individual: SXP 1323
Y1 - 2019
U6 - https://doi.org/10.1093/mnrasl/slz018
SN - 0035-8711
SN - 1365-2966
VL - 485
IS - 1
SP - L6
EP - L10
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Bohdan, Artem
A1 - Niemiec, Jacek
A1 - Pohl, Martin
A1 - Matsumoto, Yosuke
A1 - Amano, Takanobu
A1 - Hoshino, Masahiro
T1 - Kinetic Simulations of Nonrelativistic Perpendicular Shocks of Young Supernova Remnants
BT - I. Electron Shock-surfing Acceleration
JF - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2 - Electron injection at high Mach number nonrelativistic perpendicular shocks is studied here for parameters that are applicable to young SNR shocks. Using high-resolution large-scale two-dimensional fully kinetic particle-in-cell simulations and tracing individual particles, we in detail analyze the shock-surfing acceleration (SSA) of electrons at the leading edge of the shock foot. The central question is to what degree the process can be captured in 2D3V simulations. We find that the energy gain in SSA always arises from the electrostatic field of a Buneman wave. Electron energization is more efficient in the out-of-plane orientation of the large-scale magnetic field because both the phase speed and the amplitude of the waves are higher than for the in-plane scenario. Also, a larger number of electrons is trapped by the waves compared to the in-plane configuration. We conclude that significant modifications of the simulation parameters are needed to reach the same level of SSA efficiency as in simulations with out-of-plane magnetic field or 3D simulations.
KW - acceleration of particles
KW - instabilities
KW - ISM: supernova remnants
KW - methods: numerical
KW - plasmas
KW - shock waves
Y1 - 2019
U6 - https://doi.org/10.3847/1538-4357/ab1b6d
SN - 0004-637X
SN - 1538-4357
VL - 878
IS - 1
PB - IOP Publ. Ltd.
CY - Bristol
ER -
TY - JOUR
A1 - Brose, Robert
A1 - Sushch, Iuri
A1 - Pohl, Martin
A1 - Luken, K. J.
A1 - Filipovic, M. D.
A1 - Lin, R.
T1 - Nonthermal emission from the reverse shock of the youngest galactic supernova remnant G1.9+0.3
JF - Astronomy and astrophysics : an international weekly journal
N2 - Context. The youngest Galactic supernova remnant G1.9+0.3 is an interesting target for next-generation gamma-ray observatories. So far, the remnant is only detected in the radio and the X-ray bands, but its young age of approximate to 100 yr and inferred shock speed of approximate to 14 000 km s(-1) could make it an efficient particle accelerator. Aims. We aim to model the observed radio and X-ray spectra together with the morphology of the remnant. At the same time, we aim to estimate the gamma-ray flux from the source and evaluate the prospects of its detection with future gamma-ray experiments. Methods. We performed spherical symmetric 1D simulations with the RATPaC code, in which we simultaneously solved the transport equation for cosmic rays, the transport equation for magnetic turbulence, and the hydro-dynamical equations for the gas flow. Separately computed distributions of the particles accelerated at the forward and the reverse shock were then used to calculate the spectra of synchrotron, inverse Compton, and pion-decay radiation from the source. Results. The emission from G1.9+0.3 can be self-consistently explained within the test-particle limit. We find that the X-ray flux is dominated by emission from the forward shock while most of the radio emission originates near the reverse shock, which makes G1.9+0.3 the first remnant with nonthermal radiation detected from the reverse shock. The flux of very-high-energy gamma-ray emission from G1.9+0.3 is expected to be close to the sensitivity threshold of the Cherenkov Telescope Array. The limited time available to grow large-scale turbulence limits the maximum energy of particles to values below 100 TeV, hence G1.9+0.3 is not a PeVatron.
KW - acceleration of particles
KW - turbulence
KW - ISM: supernova remnants
KW - gamma rays: ISM
Y1 - 2019
U6 - https://doi.org/10.1051/0004-6361/201834430
SN - 1432-0746
VL - 627
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Kobzar, Oleh
A1 - Niemiec, Jacek
A1 - Pohl, Martin
A1 - Bohdan, Artem
T1 - Spatio-temporal evolution of the non-resonant instability in shock precursors of young supernova remnants
JF - Monthly notices of the Royal Astronomical Society
N2 - A non-resonant cosmic ray (CR) current-driven instability may operate in the shock precursors of young supernova remnants and be responsible for magnetic-field amplification, plasma heating and turbulence. Earlier simulations demonstrated magnetic-field amplification, and in kinetic studies a reduction of the relative drift between CRs and thermal plasma was observed as backreaction. However, all published simulations used periodic boundary conditions, which do not account for mass conservation in decelerating flows and only allow the temporal development to be studied. Here we report results of fully kinetic particle-in-cell simulations with open boundaries that permit inflow of plasma on one side of the simulation box and outflow at the other end, hence allowing an investigation of both the temporal and the spatial development of the instability. Magnetic-field amplification proceeds as in studies with periodic boundaries and, observed here for the first time, the reduction of relative drifts causes the formation of a shock-like compression structure at which a fraction of the plasma ions are reflected. Turbulent electric field generated by the non-resonant instability inelastically scatters CRs, modifying and anisotropizing their energy distribution. Spatial CR scattering is compatible with Bohm diffusion. Electromagnetic turbulence leads to significant non-adiabatic heating of the background plasma maintaining bulk equipartition between ions and electrons. The highest temperatures are reached at sites of large-amplitude electrostatic fields. Ion spectra show supra-thermal tails resulting from stochastic scattering in the turbulent electric field. Together, these modifications in the plasma flow will affect the properties of the shock and particle acceleration there.
KW - acceleration of particles
KW - shock waves
KW - turbulence
KW - methods: numerical
KW - cosmic rays
KW - ISM: supernova remnants
Y1 - 2017
U6 - https://doi.org/10.1093/mnras/stx1201
SN - 0035-8711
SN - 1365-2966
VL - 469
SP - 4985
EP - 4998
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Bohdan, Artem
A1 - Niemiec, Jacek
A1 - Kobzar, Oleh
A1 - Pohl, Martin
T1 - Electron Pre-acceleration at Nonrelativistic High-Mach-number Perpendicular Shocks
JF - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2 - We perform particle-in-cell simulations of perpendicular nonrelativistic collisionless shocks to study electron heating and pre-acceleration for parameters that permit the extrapolation to the conditions at young supernova remnants. Our high-resolution large-scale numerical experiments sample a representative portion of the shock surface and demonstrate that the efficiency of electron injection is strongly modulated with the phase of the shock reformation. For plasmas with low and moderate temperature (plasma beta beta p =5.10(-4) and 0.5 beta p =), we explore the nonlinear shock structure and electron pre-acceleration for various orientations of the large-scale magnetic field with respect to the simulation plane, while keeping it at 90 degrees to the shock normal. Ion reflection off of the shock leads to the formation of magnetic filaments in the shock ramp, resulting from Weibel-type instabilities, and electrostatic Buneman modes in the shock foot. In all of the cases under study, the latter provides first-stage electron energization through the shock-surfing acceleration mechanism. The subsequent energization strongly depends on the field orientation and proceeds through adiabatic or second-order Fermi acceleration processes for configurations with the out-of-plane and in-plane field components, respectively. For strictly out-of-plane field, the fraction of suprathermal electrons is much higher than for other configurations, because only in this case are the Buneman modes fully captured by the 2D simulation grid. Shocks in plasma with moderate bp provide more efficient pre-acceleration. The relevance of our results to the physics of fully 3D systems is discussed.
KW - acceleration of particles
KW - instabilities
KW - ISM: supernova remnants
KW - methods: numerical
KW - plasmas
KW - shock
Y1 - 2017
U6 - https://doi.org/10.3847/1538-4357/aa872a
SN - 0004-637X
SN - 1538-4357
VL - 847
PB - IOP Publ. Ltd.
CY - Bristol
ER -
TY - JOUR
A1 - Fraschetti, F.
A1 - Pohl, Martin
T1 - Particle acceleration model for the broad-band baseline spectrum of the Crab nebula
JF - Monthly notices of the Royal Astronomical Society
N2 - We develop a simple one-zone model of the steady-state Crab nebula spectrum encompassing both the radio/soft X-ray and the GeV/multi-TeV observations. By solving the transport equation for GeV-TeV electrons injected at the wind termination shock as a log-parabola momentum distribution and evolved via energy losses, we determine analytically the resulting differential energy spectrum of photons. We find an impressive agreement with the observed spectrum of synchrotron emission, and the synchrotron self-Compton component reproduces the previously unexplained broad 200-GeV peak that matches the Fermi/Large Area Telescope (LAT) data beyond 1 GeV with the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) data. We determine the parameters of the single log-parabola electron injection distribution, in contrast with multiple broken power-law electron spectra proposed in the literature. The resulting photon differential spectrum provides a natural interpretation of the deviation from power law customarily fitted with empirical multiple broken power laws. Our model can be applied to the radio-to-multi-TeV spectrum of a variety of astrophysical outflows, including pulsar wind nebulae and supernova remnants, as well as to interplanetary shocks.
KW - acceleration of particles
KW - shock waves
KW - cosmic rays
KW - ISM: supernova remnants
Y1 - 2017
U6 - https://doi.org/10.1093/mnras/stx1833
SN - 0035-8711
SN - 1365-2966
VL - 471
SP - 4866
EP - 4874
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Brose, Robert
A1 - Telezhinsky, Igor O.
A1 - Pohl, Martin
T1 - Transport of magnetic turbulence in supernova remnants
JF - Physical review letters
N2 - Context. Supernova remnants are known as sources of Galactic cosmic rays for their nonthermal emission of radio waves, X-rays, and gamma rays. However, the observed soft broken power-law spectra are hard to reproduce within standard acceleration theory based on the assumption of Bohm diffusion and steady-state calculations. Aims. We point out that a time-dependent treatment of the acceleration process together with a self-consistent treatment of the scattering turbulence amplification is necessary. Methods. We numerically solve the coupled system of transport equations for cosmic rays and isotropic Alfvenic turbulence. The equations are coupled through the growth rate of turbulence determined by the cosmic-ray gradient and the spatial diffusion coefficient of cosmic rays determined by the energy density of the turbulence. The system is solved on a comoving expanding grid extending upstream for dozens of shock radii, allowing for the self-consistent study of cosmic-ray diffusion in the vicinity of their acceleration site. The transport equation for cosmic rays is solved in a test-particle approach. Results. We demonstrate that the system is typically not in a steady state. In fact, even after several thousand years of evolution, no equilibrium situation is reached. The resulting time-dependent particle spectra strongly differ from those derived assuming a steady state and Bohm diffusion. Our results indicate that proper accounting for the evolution of the scattering turbulence and hence the particle diffusion coefficient is crucial for the formation of the observed soft spectra. In any case, the need to continuously develop magnetic turbulence upstream of the shock introduces nonlinearity in addition to that imposed by cosmic-ray feedback.
KW - ISM: supernova remnants
KW - acceleration of particles
KW - turbulence
Y1 - 2016
U6 - https://doi.org/10.1051/0004-6361/201527345
SN - 1432-0746
VL - 593
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Pohl, Manuela
A1 - Wilhelm, Alina
A1 - Telezhinsky, Igor O.
T1 - Reacceleration of electrons in supernova remnants
JF - Astronomy and astrophysics : an international weekly journal
N2 - Context. radio spectra of many shell-type supernova remnants show deviations from those expected on theoretical grounds.
Aims. In this paper we determine the effect of stochastic reacceleration on the spectra of electrons in the GeV band and at lower energies, and we investigate whether reacceleration can explain the observed variation in radio spectral indices.
Methods. We explicitely calculated the momentum diffusion coefficient for 3 types of turbulence expected downstream of the forward shock: fast-mode waves, small-scale non-resonant modes, and large-scale modes arising from turbulent dynamo activity. After noting that low-energy particles are efficiently coupled to the quasi-thermal plasma, a simplified cosmic-ray transport equation can be formulated and is numerically solved.
Results. Only fast-mode waves can provide momentum diffusion fast enough to significantly modify the spectra of particles. Using a synchrotron emissivity that accurately reflects a highly turbulent magnetic field, we calculated the radio spectral index and find that soft spectra with index a alpha less than or similar to -0.6 can be maintained over more than 2 decades in radio frequency, even if the electrons experience reacceleration for only one acceleration time. A spectral hardening is possible but considerably more frequency-dependent. The spectral modification imposed by stochastic reacceleration downstream of the forward shock depends only weakly on the initial spectrum provided by, e.g., diffusive shock acceleration at the shock itself.
KW - acceleration of particles
KW - turbulence
KW - cosmic rays
KW - ISM: supernova remnants
Y1 - 2015
U6 - https://doi.org/10.1051/0004-6361/201425027
SN - 0004-6361
SN - 1432-0746
VL - 574
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abramowski, Attila
A1 - Aharonian, Felix A.
A1 - Benkhali, Faical Ait
A1 - Akhperjanian, A. G.
A1 - Angüner, Ekrem Oǧuzhan
A1 - Backes, Michael
A1 - Balenderan, Shangkari
A1 - Balzer, Arnim
A1 - Barnacka, Anna
A1 - Becherini, Yvonne
A1 - Tjus, J. Becker
A1 - Berge, David
A1 - Bernhard, Sabrina
A1 - Bernlöhr, K.
A1 - Birsin, E.
A1 - Biteau, Jonathan
A1 - Boettcher, Markus
A1 - Boisson, Catherine
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Bregeon, Johan
A1 - Brun, Francois
A1 - Brun, Pierre
A1 - Bryan, Mark
A1 - Bulik, Tomasz
A1 - Carrigan, Svenja
A1 - Casanova, Sabrina
A1 - Chadwick, Paula M.
A1 - Chatraborty, N.
A1 - Chalme-Calvet, R.
A1 - Chaves, Ryan C. G.
A1 - Chretien, M.
A1 - Colafrancesco, Sergio
A1 - Cologna, Gabriele
A1 - Conrad, Jan
A1 - Couturier, C.
A1 - Cui, Y.
A1 - Davids, I. D.
A1 - Degrange, B.
A1 - Deil, C.
A1 - deWilt, P.
A1 - Djannati-Ataï, A.
A1 - Domainko, W.
A1 - Donath, A.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Dyrda, M.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Espigat, P.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Feinstein, F.
A1 - Fernandes, M. V.
A1 - Fernandez, D.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Gottschall, D.
A1 - Grondin, M. -H.
A1 - Grudzinska, M.
A1 - Hadasch, D.
A1 - Haeffner, S.
A1 - Hahn, J.
A1 - Harris, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hillert, A.
A1 - Hinton, James Anthony
A1 - Hofmann, W.
A1 - Hofverberg, P.
A1 - Holler, Markus
A1 - Horns, D.
A1 - Ivascenko, A.
A1 - Jacholkowska, A.
A1 - Jahn, C.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, F.
A1 - Jung-Richardt, O.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kaufmann, S.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kolitzus, D.
A1 - Komin, Nu
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lefaucheur, J.
A1 - Lefranc, V.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. P.
A1 - Lohse, T.
A1 - Lopatin, A.
A1 - Lu, C-C
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, Markus
A1 - McComb, T. J. L.
A1 - Mehault, J.
A1 - Meintjes, P. J.
A1 - Menzler, U.
A1 - Meyer, M.
A1 - Mitchell, A. M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - de Naurois, M.
A1 - Niemiec, J.
A1 - Nolan, S. J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Ohm, S.
A1 - Opitz, B.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Anibas, M. Paz
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Petrucci, P-O
A1 - Peyaud, B.
A1 - Pita, S.
A1 - Poon, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Reichardt, I.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Salek, D.
A1 - Sanchez, David M.
A1 - Santangelo, Andrea
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwarzburg, S.
A1 - Schwemmer, S.
A1 - Sol, H.
A1 - Spanier, F.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, Iurii
A1 - Tavernet, J-P
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Valerius, K.
A1 - van Eldik, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Veh, J.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voelk, H. J.
A1 - Volpe, F.
A1 - Vorster, M.
A1 - Vuillaume, T.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - Ward, M.
A1 - Weidinger, M.
A1 - Weitzel, Q.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zabalza, V.
A1 - Zaborov, D.
A1 - Zacharias, M.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zechlin, H-S
T1 - HESS detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud
JF - Astronomy and astrophysics : an international weekly journal
N2 - G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV < E < 100 GeV) gamma-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E > 100 GeV) gamma-ray emission coincident with this SNR with the High Energy Stereoscopic System (HESS.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F(E > 400 GeV) = (6.5 +/- 1.1(stat) +/- 1.3(syst)) x 10-11 ph cm(-2) s(-1) corresponding to similar to 0.7% of that of the Crab Nebula and to a luminosity of similar to 10(34) erg s(-1) above the same energy threshold, and a steep photon index Gamma(VHE) = 2.8 +/- 0.27(stat) +/- 0.20(syst) are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index Gamma(HE) = 2.2 +/- 0.04.2(stat-0.31sys)(+0.13), The combined gamma-ray spectrum of 0349.7+0.2 can be described by either a broken power law (I3PL) or a power law with exponential (or sub exponential) cutoff (PLC). In the former case, the photon break energy is found at E-br,E-gamma = 551(-30)(+70) GeV, slightly higher than what is usually observed in the HE/VHE gamma-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case. the exponential (respectively sub-exponential) cutoff energy is measured at E-cat,E-gamma = 1.4(-0.55)(+1.6) (respectively 0.35(-0.21)(+0.75)) TeV. A pion decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the gamma-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product or the average gas density and the total energy content of accelerated protons and nuclei amounts to nu W-p similar to 5 x 10(51) erg cm(-3)
KW - gamma rays: general
KW - ISM: supernova remnants
KW - ISM: clouds
Y1 - 2015
U6 - https://doi.org/10.1051/0004-6361/201425070
SN - 0004-6361
SN - 1432-0746
VL - 574
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abramowski, Attila
A1 - Aharonian, Felix A.
A1 - Benkhali, Faical Ait
A1 - Akhperjanian, A. G.
A1 - Angüner, Ekrem Oǧuzhan
A1 - Anton, Gisela
A1 - Backes, Michael
A1 - Balenderan, Shangkari
A1 - Balzer, Arnim
A1 - Barnacka, Anna
A1 - Becherini, Yvonne
A1 - Tjus, J. Becker
A1 - Bernlöhr, K.
A1 - Birsin, E.
A1 - Bissaldi, E.
A1 - Biteau, Jonathan
A1 - Boettcher, Markus
A1 - Boisson, Catherine
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Brucker, J.
A1 - Brun, Francois
A1 - Brun, Pierre
A1 - Bulik, Tomasz
A1 - Carrigan, Svenja
A1 - Casanova, Sabrina
A1 - Chadwick, Paula M.
A1 - Chalme-Calvet, R.
A1 - Chaves, Ryan C. G.
A1 - Cheesebrough, A.
A1 - Chretien, M.
A1 - Colafrancesco, Sergio
A1 - Cologna, Gabriele
A1 - Conrad, Jan
A1 - Couturier, C.
A1 - Cui, Y.
A1 - Dalton, M.
A1 - Daniel, M. K.
A1 - Davids, I. D.
A1 - Degrange, B.
A1 - Deil, C.
A1 - deWilt, P.
A1 - Dickinson, H. J.
A1 - Djannati-Ataï, A.
A1 - Domainko, W.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Dyrda, M.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Espigat, P.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Feinstein, F.
A1 - Fernandes, M. V.
A1 - Fernandez, D.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Füßling, Matthias
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Grondin, M. -H.
A1 - Grudzinska, M.
A1 - Haeffner, S.
A1 - Hahn, J.
A1 - Harris, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hillert, A.
A1 - Hinton, James Anthony
A1 - Hofmann, W.
A1 - Hofverberg, P.
A1 - Holler, Markus
A1 - Horns, D.
A1 - Jacholkowska, A.
A1 - Jahn, C.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, F.
A1 - Jung, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kaufmann, S.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kneiske, T.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lefaucheur, J.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Lohse, T.
A1 - Lopatin, A.
A1 - Lu, C. -C.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, Markus
A1 - McComb, T. J. L.
A1 - Mehault, J.
A1 - Meintjes, P. J.
A1 - Menzler, U.
A1 - Meyer, M.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - Naumann, C. L.
A1 - de Naurois, M.
A1 - Niemiec, J.
A1 - Nolan, S. J.
A1 - Oakes, L.
A1 - Odaka, H.
A1 - Ohm, S.
A1 - Wilhelmi, E. de Ona
A1 - Opitz, B.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Arribas, M. Paz
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perez, J.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Pita, S.
A1 - Poon, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Raue, M.
A1 - Reichardt, I.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - Reyes, R. de los
A1 - Rieger, F.
A1 - Rob, L.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Sanchez, David M.
A1 - Santangelo, Andrea
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwarzburg, S.
A1 - Schwemmer, S.
A1 - Sol, H.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, Iurii
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Valerius, K.
A1 - van Eldik, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Voelk, H. J.
A1 - Volpe, F.
A1 - Vorster, M.
A1 - Vuillaume, T.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - Ward, M.
A1 - Weidinger, M.
A1 - Weitzel, Q.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, R.
A1 - Zabalza, V.
A1 - Zacharias, M.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zechlin, H. -S.
A1 - Acero, F.
A1 - Casandjian, J. M.
A1 - Cohen-Tanugi, J.
A1 - Giordano, F.
A1 - Guillemot, L.
A1 - Lande, J.
A1 - Pletsch, H.
A1 - Uchiyama, Y.
T1 - Probing the gamma-ray emission from HESS J1834-087 using HESS and Fermi LAT observations
JF - Astronomy and astrophysics : an international weekly journal
N2 - Aims. Previous observations with the High Energy Stereoscopic System (H.E.S.S.) have revealed an extended very-high-energy (VHE; E > 100 GeV) gamma-ray source, HESS J1834-087, coincident with the supernova remnant (SNR) W41. The origin of the gamma-ray emission was investigated in more detail with the H.E.S.S. array and the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope.
Methods. The gamma-ray data provided by 61 h of observations with H.E.S.S., and four years with the Fermi LAT were analyzed, covering over five decades in energy from 1.8 GeV up to 30 TeV. The morphology and spectrum of the TeV and GeV sources were studied and multiwavelength data were used to investigate the origin of the gamma-ray emission toward W41.
Results. The TeV source can be modeled with a sum of two components: one point-like and one significantly extended (sigma(TeV) = 0.17 degrees +/- 0.01 degrees), both centered on SNR W41 and exhibiting spectra described by a power law with index Gamma(TeV) similar or equal to 2.6. The GeV source detected with Fermi LAT is extended (sigma(GeV) = 0.15 degrees +/- 0.03 degrees) and morphologically matches the VHE emission. Its spectrum can be described by a power-law model with an index Gamma(GeV) = 2.15 +/- 0.12 and smoothly joins the spectrum of the whole TeV source. A break appears in the gamma-ray spectra around 100 GeV. No pulsations were found in the GeV range.
Conclusions. Two main scenarios are proposed to explain the observed emission: a pulsar wind nebula (PWN) or the interaction of SNR W41 with an associated molecular cloud. X-ray observations suggest the presence of a point-like source (a pulsar candidate) near the center of the remnant and nonthermal X-ray diffuse emission that could arise from the possibly associated PWN. The PWN scenario is supported by the compatible positions of the TeV and GeV sources with the putative pulsar. However, the spectral energy distribution from radio to gamma-rays is reproduced by a one-zone leptonic model only if an excess of low-energy electrons is injected following a Maxwellian distribution by a pulsar with a high spin-down power (> 10(37) erg s(-1)). This additional low-energy component is not needed if we consider that the point-like TeV source is unrelated to the extended GeV and TeV sources. The interacting SNR scenario is supported by the spatial coincidence between the gamma-ray sources, the detection of OH (1720 MHz) maser lines, and the hadronic modeling.
KW - acceleration of particles
KW - ISM: supernova remnants
KW - ISM: clouds
KW - cosmic rays
Y1 - 2015
U6 - https://doi.org/10.1051/0004-6361/201322694
SN - 0004-6361
SN - 1432-0746
VL - 574
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Federici, Simone
A1 - Pohl, Martin
A1 - Telezhinsky, Igor O.
A1 - Wilhelm, Alina
A1 - Dwarkadas, Vikram V.
T1 - Analysis of GeV-band gamma-ray emission from supernova remnant RX J1713.7-3946
JF - Astronomy and astrophysics : an international weekly journal
N2 - Context. RX J1713.7-3946 is the brightest shell-type supernova remnant (SNR) of the TeV gamma-ray sky. Earlier Fermi-LAT results on low energy gamma-ray emission suggested that, despite large uncertainties in the background determination, the spectrum is inconsistent with a hadronic origin.
Aims. We update the GeV-band spectra using improved estimates for the diffuse Galactic gamma-ray emission and more than double the volume of data. We further investigate the viability of hadronic emission models for RX J1713.7-3946.
Methods. We produced a high-resolution map of the diffuse Galactic gamma-ray background corrected for the HI self-absorption and used it in the analysis of more than five years worth of Fermi-LAT data. We used hydrodynamic scaling relations and a kinetic transport equation to calculate the acceleration and propagation of cosmic rays in SNR. We then determined spectra of hadronic gamma-ray emission from RX J1713.7-3946, separately for the SNR interior and the cosmic-ray precursor region of the forward shock, and computed flux variations that would allow us to test the model with observations.
Results. We find that RX J1713.7-3946 is now detected by Fermi-LAT with very high statistical significance, and the source morphology is best described by that seen in the TeV band. The measured spectrum of RX J1713.7-3946 is hard with index gamma = 1.53 +/- 0.07, and the integral flux above 500 MeV is F = (5 : 5 +/- 1 : 1) x 10(-9) photons cm(-2) s(-1). We demonstrate that scenarios based on hadronic emission from the cosmic-ray precursor region are acceptable for RX J1713.7-3946, and we predict a secular flux increase at a few hundred GeV at the level of around 15% over ten years, which may be detectable with the upcoming Cherenkov Telescope Array (CTA) observatory.
KW - astroparticle physics
KW - cosmic rays
KW - ISM: supernova remnants
KW - gamma rays: ISM
Y1 - 2015
U6 - https://doi.org/10.1051/0004-6361/201424947
SN - 0004-6361
SN - 1432-0746
VL - 577
PB - EDP Sciences
CY - Les Ulis
ER -
TY - GEN
A1 - Abramowski, Attila
A1 - Aharonian, Felix A.
A1 - Benkhali, Faical Ait
A1 - Akhperjanian, A. G.
A1 - Angüner, Ekrem Oǧuzhan
A1 - Backes, Michael
A1 - Balenderan, Shangkari
A1 - Balzer, Arnim
A1 - Barnacka, Anna
A1 - Becherini, Yvonne
A1 - Tjus, Julia Becker
A1 - Berge, David
A1 - Bernhard, Sabrina
A1 - Bernlöhr, Konrad
A1 - Birsin, E.
A1 - Biteau, Jonathan
A1 - Böttcher, Markus
A1 - Boisson, Catherine
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Bregeon, Johan
A1 - Brun, Francois
A1 - Brun, Pierre
A1 - Bryan, Mark
A1 - Bulik, Tomasz
A1 - Carrigan, Svenja
A1 - Casanova, Sabrina
A1 - Chadwick, Paula M.
A1 - Chakraborty, Nachiketa
A1 - Chalme-Calvet, R.
A1 - Chaves, Ryan C. G.
A1 - Chretien, M.
A1 - Colafrancesco, Sergio
A1 - Cologna, Gabriele
A1 - Conrad, Jan
A1 - Couturier, Claire
A1 - Cui, Yudong
A1 - Davids, Isak Delberth
A1 - Degrange, Bernhard
A1 - Deil, Christoph
A1 - deWilt, P.
A1 - Djannati-Ataï, A.
A1 - Domainko, Wilfried
A1 - Donath, Axel
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Dyrda, M.
A1 - Edwards, Tanya
A1 - Egberts, Kathrin
A1 - Eger, Peter
A1 - Espigat, P.
A1 - Farnier, C.
A1 - Fegan, Stephen
A1 - Feinstein, Fabrice
A1 - Fernandes, Milton Virgilio
A1 - Fernandez, Diane
A1 - Fiasson, A.
A1 - Fontaine, Gerard
A1 - Förster, Andreas
A1 - Fuessling, M.
A1 - Gabici, S.
A1 - Gajdus, M.
A1 - Gallant, Yves A.
A1 - Garrigoux, Tania
A1 - Giavitto, G.
A1 - Giebels, Berrie
A1 - Glicenstein, Jean-Francois
A1 - Gottschall, Daniel
A1 - Grondin, M. -H.
A1 - Grudzinska, M.
A1 - Hadasch, Daniela
A1 - Haeffner, S.
A1 - Hahn, Joachim
A1 - Harris, Jonathan
A1 - Heinzelmann, Götz
A1 - Henri, G.
A1 - Hermann, German
A1 - Hervet, O.
A1 - Hillert, Andreas
A1 - Hinton, James Anthony
A1 - Hofmann, Werner
A1 - Hofverberg, Petter
A1 - Holler, Markus
A1 - Horns, Dieter
A1 - Ivascenko, Alex
A1 - Jacholkowska, A.
A1 - Jahn, C.
A1 - Jamrozy, Marek
A1 - Janiak, M.
A1 - Jankowsky, F.
A1 - Jung-Richardt, I.
A1 - Kastendieck, Max Anton
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kaufmann, S.
A1 - Khelifi, B.
A1 - Kieffer, Michel
A1 - Klepser, S.
A1 - Klochkov, Dmitry
A1 - Kluzniak, W.
A1 - Kolitzus, David
A1 - Komin, Nu
A1 - Kosack, Karl
A1 - Krakau, Steffen
A1 - Krayzel, F.
A1 - Krueger, Pat P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lefaucheur, J.
A1 - Lefranc, Valentin
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Lohse, Thomas
A1 - Lopatin, A.
A1 - Lu, Chia-Chun
A1 - Marandon, Vincent
A1 - Marcowith, Alexandre
A1 - Marx, Ramin
A1 - Maurin, G.
A1 - Maxted, Nigel
A1 - Mayer, Michael
A1 - McComb, T. J. Lowry
A1 - Mehault, J.
A1 - Meintjes, P. J.
A1 - Menzler, Ulf
A1 - Meyer, M.
A1 - Mitchell, Alison M. W.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Mora, K.
A1 - Moulin, Emmanuel
A1 - Murach, Thomas
A1 - de Naurois, Mathieu
A1 - Niemiec, J.
A1 - Nolan, Sam J.
A1 - Oakes, Louise
A1 - Odaka, Hirokazu
A1 - Ohm, S.
A1 - Optiz, Björn
A1 - Ostrowski, Michal
A1 - Oya, I.
A1 - Panter, Michael
A1 - Parsons, R. Daniel
A1 - Arribas, M. Paz
A1 - Pekeur, Nikki W.
A1 - Pelletier, G.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Pita, S.
A1 - Poon, Helen
A1 - Pühlhofer, Gerd
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Reichardt, I.
A1 - Reimer, Anita
A1 - Reimer, Olaf
A1 - Renaud, Metz
A1 - de los Reyes, Raquel
A1 - Rieger, Frank
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, Vardan
A1 - Salek, D.
A1 - Sanchez, David M.
A1 - Santangelo, Andrea
A1 - Schlickeiser, Reinhard
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, Ullrich
A1 - Schwarzburg, S.
A1 - Schwemmer, S.
A1 - Sol, H.
A1 - Spanier, Felix
A1 - Spengler, G.
A1 - Spies, Franziska
A1 - Stawarz, Lukasz
A1 - Steenkamp, Riaan
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, Iurii
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tluczykont, Martin
A1 - Trichard, C.
A1 - Valerius, K.
A1 - van Eldik, C.
A1 - van Soelen, B.
A1 - Vasileiadis, Georges
A1 - Veh, J.
A1 - Venter, Christo
A1 - Viana, Aion
A1 - Vincent, P.
A1 - Vink, Jacco
A1 - Völk, Heinrich J.
A1 - Volpe, Francesca
A1 - Vorster, Martine
A1 - Vuillaume, T.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Wagner, R. M.
A1 - Ward, Martin
A1 - Weidinger, Matthias
A1 - Weitzel, Quirin
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Yang, Ruizhi
A1 - Zabalza, Victor
A1 - Zaborov, Dmitry
A1 - Zacharias, M.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zechlin, Hannes -S.
T1 - H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud (vol 574, A100, 2015)
T2 - Astronomy and astrophysics : an international weekly journal
KW - gamma rays: general
KW - ISM: supernova remnants
KW - ISM: clouds
KW - errata, addenda
Y1 - 2015
U6 - https://doi.org/10.1051/0004-6361/201425070e
SN - 1432-0746
VL - 580
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Abramowski, Attila
A1 - Aharonian, Felix A.
A1 - Benkhali, Faical Ait
A1 - Akhperjanian, A. G.
A1 - Angüner, Ekrem Oǧuzhan
A1 - Anton, Gisela
A1 - Balenderan, Shangkari
A1 - Balzer, Arnim
A1 - Barnacka, Anna
A1 - Becherini, Yvonne
A1 - Tjus, J. Becker
A1 - Bernlöhr, K.
A1 - Birsin, E.
A1 - Bissaldi, E.
A1 - Biteau, Jonathan
A1 - Boettcher, Markus
A1 - Boisson, Catherine
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Brucker, J.
A1 - Brun, Francois
A1 - Brun, Pierre
A1 - Bulik, Tomasz
A1 - Carrigan, Svenja
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chadwick, Paula M.
A1 - Chalme-Calvet, R.
A1 - Chaves, Ryan C. G.
A1 - Cheesebrough, A.
A1 - Chretien, M.
A1 - Colafrancesco, Sergio
A1 - Cologna, Gabriele
A1 - Conrad, Jan
A1 - Couturier, C.
A1 - Cui, Y.
A1 - Dalton, M.
A1 - Daniel, Michael K.
A1 - Davids, I. D.
A1 - Degrange, B.
A1 - Deil, C.
A1 - deWilt, P.
A1 - Dickinson, H. J.
A1 - Djannati-Ataï, A.
A1 - Domainko, W.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Dyrda, M.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Espigat, P.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Feinstein, F.
A1 - Fernandes, M. V.
A1 - Fernandez, D.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Fuessling, M.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Grondin, M. -H.
A1 - Grudzinska, M.
A1 - Haeffner, S.
A1 - Hahn, J.
A1 - Harris, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hillert, A.
A1 - Hinton, James Anthony
A1 - Hofmann, W.
A1 - Hofverberg, P.
A1 - Holler, M.
A1 - Horns, D.
A1 - Jacholkowska, A.
A1 - Jahn, C.
A1 - Jamrozy, Marek
A1 - Janiak, M.
A1 - Jankowsky, F.
A1 - Jung, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, Krzysztof
A1 - Katz, Uli
A1 - Kaufmann, S.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kneiske, T.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lefaucheur, J.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Lennarz, D.
A1 - Lohse, T.
A1 - Lopatin, A.
A1 - Lu, C. -C.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - McComb, T. J. L.
A1 - Mehault, J.
A1 - Meintjes, P. J.
A1 - Menzler, U.
A1 - Meyer, M.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - Naumann, C. L.
A1 - de Naurois, M.
A1 - Niemiec, J.
A1 - Nolan, S. J.
A1 - Oakes, L.
A1 - Ohm, S.
A1 - Wilhelmi, E. de Ona
A1 - Opitz, B.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Arribas, M. Paz
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perez, J.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Pita, S.
A1 - Poon, H.
A1 - Puehlhofer, G.
A1 - Punch, Michael
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Raue, M.
A1 - Reimer, A.
A1 - Reimer, Olaf
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Rob, L.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Sanchez, David M.
A1 - Santangelo, Andrea
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwarzburg, S.
A1 - Schwemmer, S.
A1 - Sol, H.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, Iurii
A1 - Szostek, A.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Valerius, K.
A1 - van Eldik, Christopher
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voelk, H. J.
A1 - Volpe, F.
A1 - Vorster, M.
A1 - Vuillaume, T.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Ward, M.
A1 - Weidinger, M.
A1 - Weitzel, Q.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Zabalza, V.
A1 - Zacharias, M.
A1 - Zajczyk, A.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zechlin, H. -S.
T1 - HESS J1640-465-an exceptionally luminous TeV gamma-ray supernova remnant
JF - Monthly notices of the Royal Astronomical Society
N2 - The results of follow-up observations of the TeV gamma-ray source HESS J1640-465 from 2004 to 2011 with the High Energy Stereoscopic System (HESS) are reported in this work. The spectrum is well described by an exponential cut-off power law with photon index Gamma = 2.11 +/- 0.09(stat) +/- 0.10(sys), and a cut-off energy of E-2 = 6.0(-1.2)(+2.0) TeV. The TeV emission is significantly extended and overlaps with the northwestern part of the shell of the SNR G338.3-0.0. The new HESS results, a re-analysis of archival XMM-Newton data and multiwavelength observations suggest that a significant part of the gamma-ray emission from HESS J1640-465 originates in the supernova remnant shell. In a hadronic scenario, as suggested by the smooth connection of the GeV and TeV spectra, the product of total proton energy and mean target density could be as high as W(p)n(H) similar to 4 x 10(52)(d/10kpc)(2) erg cm(-3).
KW - radiation mechanisms: non-thermal
KW - ISM: individual objects: G338.3-0.0
KW - ISM: supernova remnants
Y1 - 2014
U6 - https://doi.org/10.1093/mnras/stu139
SN - 0035-8711
SN - 1365-2966
VL - 439
IS - 3
SP - 2828
EP - 2836
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Abramowski, Attila
A1 - Aharonian, Felix A.
A1 - Benkhali, Faical Ait
A1 - Akhperjanian, A. G.
A1 - Angüner, Ekrem Oǧuzhan
A1 - Anton, Gisela
A1 - Balenderan, Shangkari
A1 - Balzer, Arnim
A1 - Barnacka, Anna
A1 - Becherini, Yvonne
A1 - Tjus, J. Becker
A1 - Bernlöhr, K.
A1 - Birsin, E.
A1 - Bissaldi, E.
A1 - Biteau, Jonathan
A1 - Boettcher, Markus
A1 - Boisson, Catherine
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Brucker, J.
A1 - Brun, Francois
A1 - Brun, Pierre
A1 - Bulik, Tomasz
A1 - Carrigan, Svenja
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chadwick, Paula M.
A1 - Chalme-Calvet, R.
A1 - Chaves, Ryan C. G.
A1 - Cheesebrough, A.
A1 - Chretien, M.
A1 - Colafrancesco, Sergio
A1 - Cologna, Gabriele
A1 - Conrad, Jan
A1 - Couturier, C.
A1 - Cui, Y.
A1 - Dalton, M.
A1 - Daniel, M. K.
A1 - Davids, I. D.
A1 - Degrange, B.
A1 - Deil, C.
A1 - deWilt, P.
A1 - Dickinson, H. J.
A1 - Djannati-Ataï, A.
A1 - Domainko, W.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Dyrda, M.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Espigat, P.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Feinstein, F.
A1 - Fernandes, M. V.
A1 - Fernandez, D.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Fuessling, Matthias
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Grondin, M. -H.
A1 - Grudzinska, M.
A1 - Haeffner, S.
A1 - Hahn, J.
A1 - Harris, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hillert, A.
A1 - Hinton, James Anthony
A1 - Hofmann, W.
A1 - Hofverberg, P.
A1 - Holler, M.
A1 - Horns, D.
A1 - Jacholkowska, A.
A1 - Jahn, C.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, F.
A1 - Jung, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kaufmann, S.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kneiske, T.
A1 - Kolitzus, D.
A1 - Komin, Nu
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lefaucheur, J.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Lennarz, D.
A1 - Lohse, T.
A1 - Lopatin, A.
A1 - Lu, C. -C.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, M.
A1 - McComb, T. J. L.
A1 - Mehault, J.
A1 - Meintjes, P. J.
A1 - Menzler, U.
A1 - Meyer, M.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - Naumann, C. L.
A1 - de Naurois, M.
A1 - Niemiec, J.
A1 - Nolan, S. J.
A1 - Oakes, L.
A1 - Ohm, S.
A1 - Wilhelmi, E. de Ona
A1 - Opitz, B.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Arribas, M. Paz
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perez, J.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Pita, S.
A1 - Poon, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Raue, M.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Rob, L.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Sanchez, David M.
A1 - Santangelo, Andrea
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwarzburg, S.
A1 - Schwemmer, S.
A1 - Sol, H.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, Iurii
A1 - Szostek, A.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Valerius, K.
A1 - van Eldik, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Voelk, H. J.
A1 - Volpe, F.
A1 - Vorster, M.
A1 - Vuillaume, T.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Ward, M.
A1 - Weidinger, M.
A1 - Weitzel, Q.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Zabalza, V.
A1 - Zacharias, M.
A1 - Zajczyk, A.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zechlin, H. -S.
T1 - TeV gamma-ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with HESS
JF - Monthly notices of the Royal Astronomical Society
N2 - The non-thermal nature of the X-ray emission from the shell-type supernova remnants (SNRs) G1.9+0.3 and G330.2+1.0 is an indication of intense particle acceleration in the shock fronts of both objects. This suggests that the SNRs are prime candidates for very-high-energy (VHE; E > 0.1 TeV) gamma-ray observations. G1.9+0.3, recently established as the youngest known SNR in the Galaxy, also offers a unique opportunity to study the earliest stages of SNR evolution in the VHE domain. The purpose of this work is to probe the level of VHE gamma-ray emission from both SNRs and use this to constrain their physical properties. Observations were conducted with the H. E. S. S. (High Energy Stereoscopic System) Cherenkov Telescope Array over a more than six-year period spanning 2004-2010. The obtained data have effective livetimes of 67 h for G1.9+0.3 and 16 h for G330.2+1.0. The data are analysed in the context of the multiwavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant gamma-ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99 per cent confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index Gamma = 2.5 were set at 5.6 x 10(-1)3 cm(-2) s(-1) above 0.26 TeV and 3.2 x 10(-12) cm(-2) s(-1) above 0.38 TeV, respectively. In a one-zone leptonic scenario, these upper limits imply lower limits on the interior magnetic field to B-G1.9 greater than or similar to 12 mu G for G1.9+0.3 and to B-G330 greater than or similar to 8 mu G for G330.2+1.0. In a hadronic scenario, the low ambient densities and the large distances to the SNRs result in very low predicted fluxes, for which the H.E.S.S. upper limits are not constraining.
KW - radiation mechanisms: non-thermal
KW - ISM: individual objects: SNR G1.9+0.3
KW - ISM: individual objects: SNR G330.2+1.0
KW - ISM: magnetic fields
KW - ISM: supernova remnants
KW - gamma-rays: ISM
Y1 - 2014
U6 - https://doi.org/10.1093/mnras/stu459
SN - 0035-8711
SN - 1365-2966
VL - 441
IS - 1
SP - 790
EP - 799
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Aliu, E.
A1 - Archambault, S.
A1 - Aune, T.
A1 - Behera, B.
A1 - Beilicke, M.
A1 - Benbow, W.
A1 - Berger, K.
A1 - Bird, R.
A1 - Buckley, J. H.
A1 - Bugaev, V.
A1 - Cardenzana, J. V.
A1 - Cerruti, M.
A1 - Chen, Xuhui
A1 - Ciupik, L.
A1 - Collins-Hughes, E.
A1 - Connolly, M. P.
A1 - Cui, W.
A1 - Dumm, J.
A1 - Dwarkadas, Vikram V.
A1 - Errando, M.
A1 - Falcone, A.
A1 - Federici, Simone
A1 - Feng, Q.
A1 - Finley, J. P.
A1 - Fleischhack, H.
A1 - Fortin, P.
A1 - Fortson, L.
A1 - Furniss, A.
A1 - Galante, N.
A1 - Gall, D.
A1 - Gillanders, G. H.
A1 - Griffin, S.
A1 - Griffiths, S. T.
A1 - Grube, J.
A1 - Gyuk, G.
A1 - Hanna, D.
A1 - Holder, J.
A1 - Hughes, G.
A1 - Humensky, T. B.
A1 - Kaaret, P.
A1 - Kertzman, M.
A1 - Khassen, Y.
A1 - Kieda, D.
A1 - Krennrich, F.
A1 - Kumar, S.
A1 - Lang, M. J.
A1 - Madhavan, A. S.
A1 - Maier, G.
A1 - McCann, A. J.
A1 - Meagher, K.
A1 - Millis, J.
A1 - Moriarty, P.
A1 - Mukherjee, R.
A1 - Nieto, D.
A1 - Ong, R. A.
A1 - Otte, A. N.
A1 - Pandel, D.
A1 - Park, N.
A1 - Pohl, Martin
A1 - Popkow, A.
A1 - Prokoph, H.
A1 - Quinn, J.
A1 - Ragan, K.
A1 - Rajotte, J.
A1 - Ratliff, G.
A1 - Reyes, L. C.
A1 - Reynolds, P. T.
A1 - Richards, G. T.
A1 - Roache, E.
A1 - Rousselle, J.
A1 - Sembroski, G. H.
A1 - Shahinyan, K.
A1 - Sheidaei, F.
A1 - Smith, A. W.
A1 - Staszak, D.
A1 - Telezhinsky, Igor O.
A1 - Tsurusaki, K.
A1 - Tucci, J. V.
A1 - Tyler, J.
A1 - Varlotta, A.
A1 - Vassiliev, V. V.
A1 - Vincent, S.
A1 - Wakely, S. P.
A1 - Ward, J. E.
A1 - Weinstein, A.
A1 - Welsing, R.
A1 - Wilhelm, Alina
T1 - Investigating the TeV morpholoy of MGRO J1908+06 with veritas
JF - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2 - We report on deep observations of the extended TeV gamma-ray source MGRO J1908+06 made with the VERITAS very high energy gamma-ray observatory. Previously, the TeV emission has been attributed to the pulsar wind nebula (PWN) of the Fermi-LAT pulsar PSR J1907+0602. We detect MGRO J1908+06 at a significance level of 14 standard deviations (14 sigma) and measure a photon index of 2.20 +/- 0.10(stat) +/- 0.20(sys). The TeV emission is extended, covering the region near PSR J1907+0602 and also extending toward SNR G40.5-0.5. When fitted with a two-dimensional Gaussian, the intrinsic extension has a standard deviation of sigma(src) = 0 degrees.44 +/- 0 degrees.02. In contrast to other TeV PWNe of similar age in which the TeV spectrum softens with distance from the pulsar, the TeV spectrum measured near the pulsar location is consistent with that measured at a position near the rim of G40.5-0.5, 0 degrees.33 away.
KW - gamma rays: general
KW - gamma-ray burst: individual (MGRO J1908+06, VER J1907+062)
KW - pulsars: individual (PSR J1907+0602)
KW - ISM: supernova remnants
Y1 - 2014
U6 - https://doi.org/10.1088/0004-637X/787/2/166
SN - 0004-637X
SN - 1538-4357
VL - 787
IS - 2
PB - IOP Publ. Ltd.
CY - Bristol
ER -
TY - GEN
A1 - Abramowski, Attila
A1 - Aharonian, Felix A.
A1 - Benkhali, Faical Ait
A1 - Akhperjanian, A. G.
A1 - Angüner, Ekrem Oǧuzhan
A1 - Anton, Gisela
A1 - Balenderan, Shangkari
A1 - Balzer, Arnim
A1 - Barnacka, Anna
A1 - Becherini, Yvonne
A1 - Tjus, J. Becker
A1 - Bernlöhr, K.
A1 - Birsin, E.
A1 - Bissaldi, E.
A1 - Biteau, Jonathan
A1 - Boettcher, Markus
A1 - Boisson, Catherine
A1 - Bolmont, J.
A1 - Bordas, Pol
A1 - Brucker, J.
A1 - Brun, Francois
A1 - Brun, Pierre
A1 - Bulik, Tomasz
A1 - Carrigan, Svenja
A1 - Casanova, Sabrina
A1 - Cerruti, M.
A1 - Chadwick, Paula M.
A1 - Chalme-Calvet, R.
A1 - Chaves, Ryan C. G.
A1 - Cheesebrough, A.
A1 - Chretien, M.
A1 - Colafrancesco, Sergio
A1 - Cologna, Gabriele
A1 - Conrad, Jan
A1 - Couturier, C.
A1 - Cui, Y.
A1 - Dalton, M.
A1 - Daniel, M. K.
A1 - Davids, I. D.
A1 - Degrange, B.
A1 - Deil, C.
A1 - deWilt, P.
A1 - Dickinson, H. J.
A1 - Djannati-Ataï, A.
A1 - Domainko, W.
A1 - Dubus, G.
A1 - Dutson, K.
A1 - Dyks, J.
A1 - Dyrda, M.
A1 - Edwards, T.
A1 - Egberts, Kathrin
A1 - Eger, P.
A1 - Espigat, P.
A1 - Farnier, C.
A1 - Fegan, S.
A1 - Feinstein, F.
A1 - Fernandes, M. V.
A1 - Fernandez, D.
A1 - Fiasson, A.
A1 - Fontaine, G.
A1 - Foerster, A.
A1 - Fuessling, M.
A1 - Gajdus, M.
A1 - Gallant, Y. A.
A1 - Garrigoux, T.
A1 - Giavitto, G.
A1 - Giebels, B.
A1 - Glicenstein, J. F.
A1 - Grondin, M. -H.
A1 - Grudzinska, M.
A1 - Haeffner, S.
A1 - Hahn, J.
A1 - Harris, J.
A1 - Heinzelmann, G.
A1 - Henri, G.
A1 - Hermann, G.
A1 - Hervet, O.
A1 - Hillert, A.
A1 - Hinton, James Anthony
A1 - Hofmann, W.
A1 - Hofverberg, P.
A1 - Holler, M.
A1 - Horns, D.
A1 - Jacholkowska, A.
A1 - Jahn, C.
A1 - Jamrozy, M.
A1 - Janiak, M.
A1 - Jankowsky, F.
A1 - Jung, I.
A1 - Kastendieck, M. A.
A1 - Katarzynski, K.
A1 - Katz, U.
A1 - Kaufmann, S.
A1 - Khelifi, B.
A1 - Kieffer, M.
A1 - Klepser, S.
A1 - Klochkov, D.
A1 - Kluzniak, W.
A1 - Kneiske, T.
A1 - Kolitzus, D.
A1 - Komin, Nu.
A1 - Kosack, K.
A1 - Krakau, S.
A1 - Krayzel, F.
A1 - Krueger, P. P.
A1 - Laffon, H.
A1 - Lamanna, G.
A1 - Lefaucheur, J.
A1 - Lemiere, A.
A1 - Lemoine-Goumard, M.
A1 - Lenain, J. -P.
A1 - Lennarz, D.
A1 - Lohse, T.
A1 - Lopatin, A.
A1 - Lu, C. -C.
A1 - Marandon, V.
A1 - Marcowith, Alexandre
A1 - Marx, R.
A1 - Maurin, G.
A1 - Maxted, N.
A1 - Mayer, Michael
A1 - McComb, T. J. L.
A1 - Mehault, J.
A1 - Meintjes, P. J.
A1 - Menzler, U.
A1 - Meyer, M.
A1 - Moderski, R.
A1 - Mohamed, M.
A1 - Moulin, Emmanuel
A1 - Murach, T.
A1 - Naumann, C. L.
A1 - de Naurois, M.
A1 - Niemiec, J.
A1 - Nolan, S. J.
A1 - Oakes, L.
A1 - Ohm, S.
A1 - Wilhelmi, E. de Ona
A1 - Opitz, B.
A1 - Ostrowski, M.
A1 - Oya, I.
A1 - Panter, M.
A1 - Parsons, R. D.
A1 - Arribas, M. Paz
A1 - Pekeur, N. W.
A1 - Pelletier, G.
A1 - Perez, J.
A1 - Petrucci, P. -O.
A1 - Peyaud, B.
A1 - Pita, S.
A1 - Poon, H.
A1 - Puehlhofer, G.
A1 - Punch, M.
A1 - Quirrenbach, A.
A1 - Raab, S.
A1 - Raue, M.
A1 - Reimer, A.
A1 - Reimer, O.
A1 - Renaud, M.
A1 - de los Reyes, R.
A1 - Rieger, F.
A1 - Rob, L.
A1 - Romoli, C.
A1 - Rosier-Lees, S.
A1 - Rowell, G.
A1 - Rudak, B.
A1 - Rulten, C. B.
A1 - Sahakian, V.
A1 - Sanchez, David M.
A1 - Santangelo, Andrea
A1 - Schlickeiser, R.
A1 - Schuessler, F.
A1 - Schulz, A.
A1 - Schwanke, U.
A1 - Schwarzburg, S.
A1 - Schwemmer, S.
A1 - Sol, H.
A1 - Spengler, G.
A1 - Spies, F.
A1 - Stawarz, L.
A1 - Steenkamp, R.
A1 - Stegmann, Christian
A1 - Stinzing, F.
A1 - Stycz, K.
A1 - Sushch, Iurii
A1 - Szostek, A.
A1 - Tavernet, J. -P.
A1 - Tavernier, T.
A1 - Taylor, A. M.
A1 - Terrier, R.
A1 - Tluczykont, M.
A1 - Trichard, C.
A1 - Valerius, K.
A1 - van Eldik, C.
A1 - van Soelen, B.
A1 - Vasileiadis, G.
A1 - Venter, C.
A1 - Viana, A.
A1 - Vincent, P.
A1 - Vink, J.
A1 - Voelk, H. J.
A1 - Volpe, F.
A1 - Vorster, M.
A1 - Vuillaume, T.
A1 - Wagner, S. J.
A1 - Wagner, P.
A1 - Ward, M.
A1 - Weidinger, M.
A1 - Weitzel, Q.
A1 - White, R.
A1 - Wierzcholska, A.
A1 - Willmann, P.
A1 - Woernlein, A.
A1 - Wouters, D.
A1 - Zabalza, V.
A1 - Zacharias, M.
A1 - Zajczyk, A.
A1 - Zdziarski, A. A.
A1 - Zech, Alraune
A1 - Zechlin, H. -S.
T1 - HESS J1640-465 - an exceptionally luminous TeV gamma-ray supernova remnant (vol 439, pg 2828, 2014)
T2 - Monthly notices of the Royal Astronomical Society
KW - errata, addenda
KW - radiation mechanisms: non-thermal
KW - ISM: individual objects: G338.3-0.0
KW - ISM: supernova remnants
Y1 - 2014
U6 - https://doi.org/10.1093/mnras/stu826
SN - 0035-8711
SN - 1365-2966
VL - 441
IS - 4
SP - 3640
EP - 3642
PB - Oxford Univ. Press
CY - Oxford
ER -
TY - JOUR
A1 - Abdo, A. A.
A1 - Ackermann, Margit
A1 - Ajello, M.
A1 - Allafort, A. J.
A1 - Baldini, L.
A1 - Ballet, J.
A1 - Barbiellini, G.
A1 - Baring, M. G.
A1 - Bastieri, D.
A1 - Bellazzini, R.
A1 - Berenji, B.
A1 - Blandford, R. D.
A1 - Bloom, E. D.
A1 - Bonamente, E.
A1 - Borgland, A. W.
A1 - Bouvier, A.
A1 - Brandt, T. J.
A1 - Bregeon, Johan
A1 - Brigida, M.
A1 - Bruel, P.
A1 - Buehler, R.
A1 - Buson, S.
A1 - Caliandro, G. A.
A1 - Cameron, R. A.
A1 - Caraveo, P. A.
A1 - Casandjian, J. M.
A1 - Cecchi, C.
A1 - Chaty, S.
A1 - Chekhtman, A.
A1 - Cheung, C. C.
A1 - Chiang, J.
A1 - Cillis, A. N.
A1 - Ciprini, S.
A1 - Claus, R.
A1 - Cohen-Tanugi, J.
A1 - Conrad, Jan
A1 - Corbel, S.
A1 - Cutini, S.
A1 - de Angelis, A.
A1 - de Palma, F.
A1 - Dermer, C. D.
A1 - Digel, S. W.
A1 - do Couto e Silva, E.
A1 - Drell, P. S.
A1 - Drlica-Wagner, A.
A1 - Dubois, R.
A1 - Dumora, D.
A1 - Favuzzi, C.
A1 - Ferrara, E. C.
A1 - Fortin, P.
A1 - Frailis, M.
A1 - Fukazawa, Y.
A1 - Fukui, Y.
A1 - Funk, S.
A1 - Fusco, P.
A1 - Gargano, F.
A1 - Gasparrini, D.
A1 - Gehrels, N.
A1 - Germani, S.
A1 - Giglietto, N.
A1 - Giordano, F.
A1 - Giroletti, M.
A1 - Glanzman, T.
A1 - Godfrey, G.
A1 - Grenier, I. A.
A1 - Grondin, M. -H.
A1 - Guiriec, S.
A1 - Hadasch, D.
A1 - Hanabata, Y.
A1 - Harding, A. K.
A1 - Hayashida, M.
A1 - Hayashi, K.
A1 - Hays, E.
A1 - Horan, D.
A1 - Jackson, M. S.
A1 - Johannesson, G.
A1 - Johnson, A. S.
A1 - Kamae, T.
A1 - Katagiri, H.
A1 - Kataoka, J.
A1 - Kerr, M.
A1 - Knoedlseder, J.
A1 - Kuss, M.
A1 - Lande, J.
A1 - Latronico, L.
A1 - Lee, S. -H.
A1 - Lemoine-Goumard, M.
A1 - Longo, F.
A1 - Loparco, F.
A1 - Lovellette, M. N.
A1 - Lubrano, P.
A1 - Madejski, G. M.
A1 - Makeev, A.
A1 - Mazziotta, Mario Nicola
A1 - McEnery, J. E.
A1 - Michelson, P. F.
A1 - Mignani, R. P.
A1 - Mitthumsiri, W.
A1 - Mizuno, T.
A1 - Moiseev, A. A.
A1 - Monte, C.
A1 - Monzani, M. E.
A1 - Morselli, A.
A1 - Moskalenko, I. V.
A1 - Murgia, S.
A1 - Naumann-Godo, M.
A1 - Nolan, P. L.
A1 - Norris, J. P.
A1 - Nuss, E.
A1 - Ohsugi, T.
A1 - Okumura, A.
A1 - Orlando, E.
A1 - Ormes, J. F.
A1 - Paneque, D.
A1 - Parent, D.
A1 - Pelassa, V.
A1 - Pesce-Rollins, M.
A1 - Pierbattista, M.
A1 - Piron, F.
A1 - Pohl, Martin
A1 - Porter, T. A.
A1 - Raino, S.
A1 - Rando, R.
A1 - Razzano, M.
A1 - Reimer, O.
A1 - Reposeur, T.
A1 - Ritz, S.
A1 - Romani, R. W.
A1 - Roth, M.
A1 - Sadrozinski, H. F. -W.
A1 - Parkinson, P. M. Saz
A1 - Sgro, C.
A1 - Smith, D. A.
A1 - Smith, P. D.
A1 - Spandre, G.
A1 - Spinelli, P.
A1 - Strickman, M. S.
A1 - Tajima, H.
A1 - Takahashi, H.
A1 - Takahashi, T.
A1 - Tanaka, T.
A1 - Thayer, J. G.
A1 - Thayer, J. B.
A1 - Thompson, D. J.
A1 - Tibaldo, L.
A1 - Tibolla, O.
A1 - Torres, D. F.
A1 - Tosti, G.
A1 - Tramacere, A.
A1 - Troja, E.
A1 - Uchiyama, Y.
A1 - Vandenbroucke, J.
A1 - Vasileiou, V.
A1 - Vianello, G.
A1 - Vilchez, N.
A1 - Vitale, V.
A1 - Waite, A. P.
A1 - Wang, P.
A1 - Winer, B. L.
A1 - Wood, K. S.
A1 - Yamamoto, H.
A1 - Yamazaki, R.
A1 - Yang, Z.
A1 - Ziegler, M.
T1 - Observations of the young supernova remnant RX J1713.7-3946 with the fermi large area telescope
JF - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2 - We present observations of the young supernova remnant (SNR) RX J1713.7-3946 with the Fermi Large Area Telescope (LAT). We clearly detect a source positionally coincident with the SNR. The source is extended with a best-fit extension of 0 degrees.55 +/- 0 degrees.04 matching the size of the non-thermal X-ray and TeV gamma-ray emission from the remnant. The positional coincidence and the matching extended emission allow us to identify the LAT source with SNR RX J1713.7-3946. The spectrum of the source can be described by a very hard power law with a photon index of Gamma = 1.5 +/- 0.1 that coincides in normalization with the steeper H. E. S. S.-detected gamma-ray spectrum at higher energies. The broadband gamma-ray emission is consistent with a leptonic origin as the dominant mechanism for the gamma-ray emission.
KW - acceleration of particles
KW - gamma rays: general
KW - gamma rays: ISM
KW - ISM: individual objects (RX J1713.7-3946)
KW - ISM: supernova remnants
KW - radiation mechanisms: non-thermal
Y1 - 2011
U6 - https://doi.org/10.1088/0004-637X/734/1/28
SN - 0004-637X
VL - 734
IS - 1
PB - IOP Publ. Ltd.
CY - Bristol
ER -
TY - JOUR
A1 - Henault-Brunet, V.
A1 - Oskinova, Lidia M.
A1 - Guerrero, Martín A.
A1 - Sun, W.
A1 - Chu, Y.-H.
A1 - Evans, C. J.
A1 - Gallagher, J. S.
A1 - Gruendl, R. A.
A1 - Reyes-Iturbide, J.
T1 - Discovery of a Be/X-ray pulsar binary and associated supernova remnant in the wing of the small magellanic cloud
JF - Monthly notices of the Royal Astronomical Society
N2 - We report on a new Be/X-ray pulsar binary located in the Wing of the Small Magellanic Cloud (SMC). The strong pulsed X-ray source was discovered with the Chandra and XMM-Newton X-ray observatories. The X-ray pulse period of 1062 s is consistently determined from both Chandra and XMM-Newton observations, revealing one of the slowest rotating X-ray pulsars known in the SMC. The optical counterpart of the X-ray source is the emission-line star 2dFS 3831. Its B0-0.5(III)e+ spectral type is determined from VLT-FLAMES and 2dF optical spectroscopy, establishing the system as a Be/X-ray binary (Be-XRB). The hard X-ray spectrum is well fitted by a power law with additional thermal and blackbody components, the latter reminiscent of persistent Be-XRBs. This system is the first evidence of a recent supernova in the low-density surroundings of NGC602. We detect a shell nebula around 2dFS 3831 in H alpha and [OIII] images and conclude that it is most likely a supernova remnant. If it is linked to the supernova explosion that created this new X-ray pulsar, its kinematic age of (2-4) x 10(4) yr provides a constraint on the age of the pulsar.
KW - stars: emission-line, Be
KW - ISM: supernova remnants
KW - Magellanic Clouds
KW - X-rays: binaries
Y1 - 2012
U6 - https://doi.org/10.1111/j.1745-3933.2011.01183.x
SN - 0035-8711
VL - 420
IS - 1
SP - L13
EP - L17
PB - Wiley-Blackwell
CY - Malden
ER -
TY - JOUR
A1 - Telezhinsky, Igor O.
A1 - Dwarkadas, Vikram V.
A1 - Pohl, Martin
T1 - Time-dependent escape of cosmic rays from supernova remnants, and their interaction with dense media
JF - Astronomy and astrophysics : an international weekly journal
N2 - Context. Supernova remnants (SNRs) are thought to be the main source of Galactic cosmic rays (CRs) up to the "knee" in CR spectrum. During the evolution of a SNR, the bulk of the CRs are confined inside the SNR shell. The highest-energy particles leave the system continuously, while the remaining adiabatically cooled particles are released when the SNR has expanded sufficiently and decelerated so that the magnetic field at the shock is no longer able to confine them. Particles escaping from the parent system may interact with nearby molecular clouds, producing.-rays in the process via pion decay. The soft gamma-ray spectra observed for a number of SNRs interacting with molecular clouds, however, challenge current theories of non-linear particle acceleration that predict harder spectra.
Aims. We study how the spectrum of escaped particles depends on the time-dependent acceleration history in both Type Ia and core-collapse SNRs, as well as on different assumptions about the diffusion coefficient in the vicinity of the SNR.
Methods. We solve the CR transport equation in a test-particle approach combined with numerical simulations of SNR evolution.
Results. We extend our method for calculating the CR acceleration in SNRs to trace the escaped particles in a large volume around SNRs. We calculate the evolution of the spectra of CRs that have escaped from a SNR into a molecular cloud or dense shell for two diffusion models. We find a strong confinement of CRs in a close region around the SNR, and a strong dilution effect for CRs that were able to propagate out as far as a few SNR radii.
KW - ISM: supernova remnants
KW - ISM: clouds
KW - cosmic rays
Y1 - 2012
U6 - https://doi.org/10.1051/0004-6361/201118639
SN - 0004-6361
VL - 541
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Rettig, R.
A1 - Pohl, M.
T1 - The properties of non-thermal X-ray filaments in young supernova remnants
JF - Astronomy and astrophysics : an international weekly journal
N2 - Context. Young supernova remnants (SNRs) exhibit narrow filaments of non-thermal X-ray emission whose widths can be limited either by electron energy losses or damping of the magnetic field.
Aims. We want to investigate whether or not different models of these filaments can be observationally tested.
Methods. Using observational parameters of four historical remnants, we calculated the filament profiles and compared the spectra of the filaments with those of the total non-thermal emission. For that purpose, we solved a one-dimensional stationary transport equation for the isotropic differential number density of the electrons.
Results. We find that the difference between the spectra of filament and total non-thermal emission above 1 keV is more pronounced in the damping model than in the energy-loss model.
Conclusions. A considerable damping of the magnetic field can result in an observable difference between the spectra of filament and total non-thermal emission, thus potentially permitting an observational discrimination between the energy-loss model and the damping model of the X-ray filaments.
KW - acceleration of particles
KW - ISM: supernova remnants
KW - ISM: magnetic fields
KW - X-rays: ISM
Y1 - 2012
U6 - https://doi.org/10.1051/0004-6361/201219409
SN - 0004-6361
VL - 545
IS - 5
PB - EDP Sciences
CY - Les Ulis
ER -
TY - JOUR
A1 - Niemiec, Jacek
A1 - Pohl, Martin
A1 - Bret, Antoine
A1 - Wieland, Volkmar
T1 - Nonrelativistic parallel shocks in unmagnetized and weakly magnetized plasmas
JF - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2 - We present results of 2D3V particle-in-cell simulations of nonrelativistic plasma collisions with absent or parallel large-scale magnetic field for parameters applicable to the conditions at young supernova remnants. We study the collision of plasma slabs of different density, leading to two different shocks and a contact discontinuity. Electron dynamics play an important role in the development of the system. While nonrelativistic shocks in both unmagnetized and magnetized plasmas can be mediated by Weibel-type instabilities, the efficiency of shock-formation processes is higher when a large-scale magnetic field is present. The electron distributions downstream of the forward and reverse shocks are generally isotropic, whereas that is not always the case for the ions. We do not see any significant evidence of pre-acceleration, neither in the electron population nor in the ion distribution.
KW - acceleration of particles
KW - instabilities
KW - ISM: supernova remnants
KW - methods: numerical
KW - plasmas
KW - shock waves
Y1 - 2012
U6 - https://doi.org/10.1088/0004-637X/759/1/73
SN - 0004-637X
SN - 1538-4357
VL - 759
IS - 1
PB - IOP Publ. Ltd.
CY - Bristol
ER -
TY - JOUR
A1 - tAliu, E.
A1 - Archambault, S.
A1 - Arlen, T.
A1 - Aune, T.
A1 - Beilicke, M.
A1 - Benbow, W.
A1 - Bird, R.
A1 - Bouvier, A.
A1 - Bradbury, S. M.
A1 - Buckley, J. H.
A1 - Bugaev, V.
A1 - Byrum, K.
A1 - Cannon, A.
A1 - Cesarini, A.
A1 - Ciupik, L.
A1 - Collins-Hughes, E.
A1 - Connolly, M. P.
A1 - Cui, W.
A1 - Dickherber, R.
A1 - Duke, C.
A1 - Dumm, J.
A1 - Dwarkadas, Vikram V.
A1 - Errando, M.
A1 - Falcone, A.
A1 - Federici, Simone
A1 - Feng, Q.
A1 - Finley, J. P.
A1 - Finnegan, G.
A1 - Fortson, L.
A1 - Furniss, A.
A1 - Galante, N.
A1 - Gall, D.
A1 - Gillanders, G. H.
A1 - Godambe, S.
A1 - Gotthelf, E. V.
A1 - Griffin, S.
A1 - Grube, J.
A1 - Gyuk, G.
A1 - Hanna, D.
A1 - Holder, J.
A1 - Huan, H.
A1 - Hughes, G.
A1 - Humensky, T. B.
A1 - Kaaret, P.
A1 - Karlsson, N.
A1 - Kertzman, M.
A1 - Khassen, Y.
A1 - Kieda, D.
A1 - Krawczynski, H.
A1 - Krennrich, F.
A1 - Lang, M. J.
A1 - Lee, K.
A1 - Madhavan, A. S.
A1 - Maier, G.
A1 - Majumdar, P.
A1 - McArthur, S.
A1 - McCann, A.
A1 - Millis, J.
A1 - Moriarty, P.
A1 - Mukherjee, R.
A1 - Nelson, T.
A1 - de Bhroithe, A. O'Faolain
A1 - Ong, R. A.
A1 - Orr, M.
A1 - Otte, A. N.
A1 - Pandel, D.
A1 - Park, N.
A1 - Perkins, J. S.
A1 - Pohl, Martin
A1 - Popkow, A.
A1 - Prokoph, H.
A1 - Quinn, J.
A1 - Ragan, K.
A1 - Reyes, L. C.
A1 - Reynolds, P. T.
A1 - Roache, E.
A1 - Rose, H. J.
A1 - Ruppel, Jens
A1 - Saxon, D. B.
A1 - Schroedter, M.
A1 - Sembroski, G. H.
A1 - Sentuerk, G. D.
A1 - Skole, C.
A1 - Telezhinsky, Igor O.
A1 - Tesic, G.
A1 - Theiling, M.
A1 - Thibadeau, S.
A1 - Tsurusaki, K.
A1 - Tyler, J.
A1 - Varlotta, A.
A1 - Vassiliev, V. V.
A1 - Vincent, S.
A1 - Wakely, S. P.
A1 - Ward, J. E.
A1 - Weekes, T. C.
A1 - Weinstein, A.
A1 - Weisgarber, T.
A1 - Welsing, R.
A1 - Williams, D. A.
A1 - Zitzer, B.
T1 - Discovery of TeV Gamma-Ray emission toward supernova remnant SNR G78.2+2.1
JF - The astrophysical journal : an international review of spectroscopy and astronomical physics
N2 - We report the discovery of an unidentified, extended source of very-high-energy gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hr of data taken by the VERITAS gamma-ray observatory in 2009. These data confirm the preliminary indications of gamma-ray emission previously seen in a two-year (2007-2009) blind survey of the Cygnus region by VERITAS. VER J2019+407, which is detected at a post-trials significance of 7.5 standard deviations in the 2009 data, is localized to the northwestern rim of the remnant in a region of enhanced radio and X-ray emission. It has an intrinsic extent of 0 degrees.23 +/- 0 degrees.03(stat-0 degrees.02sys)(+0 degrees.04) and its spectrum is well-characterized by a differential power law (dN/dE = N-0 x (E/TeV)-Gamma) with a photon index of Gamma = 2.37 +/- 0.14(stat) +/- 0.20(sys) and a flux normalization of N-0 = 1.5 +/- 0.2(stat) +/- 0.4(sys) x 10(-12) photon TeV-1 cm(-2) s(-1). This yields an integral flux of 5.2 +/- 0.8(stat) +/- 1.4(sys) x 10(-12) photon cm(-2) s(-1) above 320 GeV, corresponding to 3.7% of the Crab Nebula flux. We consider the relationship of the TeV gamma-ray emission with the GeV gamma-ray emission seen from SNR G78.2+2.1 as well as that seen from a nearby cocoon of freshly accelerated cosmic rays. Multiple scenarios are considered as possible origins for the TeV gamma-ray emission, including hadronic particle acceleration at the SNR shock.
KW - acceleration of particles
KW - cosmic rays
KW - gamma rays: general
KW - ISM: supernova remnants
Y1 - 2013
U6 - https://doi.org/10.1088/0004-637X/770/2/93
SN - 0004-637X
VL - 770
IS - 2
PB - IOP Publ. Ltd.
CY - Bristol
ER -