% IMPORTANT: The following is UTF-8 encoded. This means that in the presence
% of non-ASCII characters, it will not work with BibTeX 0.99 or older.
% Instead, you should use an up-to-date BibTeX implementation like “bibtex8” or
% “biber”.
@ARTICLE{Collaboration:193081,
author = {Abramowski, A. and Aharonian, F. and Benkhali, F. Ait and
Akhperjanian, A. G. and Angüner, E. and Anton, G. and
Backes, M. and Balenderan, S. and Balzer, A. and Barnacka,
A. and Becherini, Y. and Tjus, J. Becker and Bernlöhr, K.
and Birsin, E. and Bissaldi, E. and Biteau, J. and
Böttcher, M. and Boisson, C. and Bolmont, J. and Bordas, P.
and Brucker, J. and Brun, F. and Brun, P. and Bulik, T. and
Carrigan, S. and Casanova, S. and Chadwick, P. M. and
Chalme-Calvet, R. and Chaves, R. C. G. and Cheesebrough, A.
and Chrétien, M. and Colafrancesco, S. and Cologna, G. and
Conrad, J. and Couturier, C. and Cui, Y. and Dalton, M. and
Daniel, Marcus and Davids, I. D. and Degrange, B. and Deil,
C. and deWilt, P. and Dickinson, H. J. and Djannati-Ataï,
A. and Domainko, W. and Drury, L. O'C. and Dubus, G. and
Dutson, K. and Dyks, J. and Dyrda, M. and Edwards, T. and
Egberts, K. and Eger, P. and Espigat, P. and Farnier, C. and
Fegan, S. and Feinstein, F. and Fernandes, M. V. and
Fernandez, D. and Fiasson, A. and Fontaine, G. and Förster,
A. and Füßling, M. and Gajdus, M. and Gallant, Y. A. and
Garrigoux, T. and Giavitto, G. and Giebels, B. and
Glicenstein, J. F. and Grondin, M. -H. and Grudzińska, M.
and Häffner, S. and Hahn, J. and Harris, J. and
Heinzelmann, G. and Henri, G. and Hermann, G. and Hervet, O.
and Hillert, A. and Hinton, J. A. and Hofmann, W. and
Hofverberg, P. and Holler, M. and Horns, D. and
Jacholkowska, A. and Jahn, C. and Jamrozy, M. and Janiak, M.
and Jankowsky, F. and Jung, I. and Kastendieck, M. A. and
Katarzyński, K. and Katz, U. and Kaufmann, S. and Khélifi,
B. and Kieffer, M. and Klepser, S. and Klochkov, D. and
Kluźniak, W. and Kneiske, T. and Kolitzus, D. and Komin,
Nu. and Kosack, K. and Krakau, S. and Krayzel, F. and
Krüger, P. P. and Laffon, H. and Lamanna, G. and
Lefaucheur, J. and Lemière, A. and Lemoine-Goumard, M. and
Lenain, J. -P. and Lohse, T. and Lopatin, A. and Lu, C. -C.
and Marandon, V. and Marcowith, A. and Marx, R. and Maurin,
G. and Maxted, N. and Mayer, M. and McComb, T. J. L. and
Méhault, J. and Meintjes, P. J. and Menzler, U. and Meyer,
Manuel and Moderski, R. and Mohamed, M. and Moulin, E. and
Murach, T. and Naumann, C. L. and de Naurois, M. and
Niemiec, J. and Nolan, S. J. and Oakes, L. and Odaka, H. and
Ohm, S. and Wilhelmi, E. de Oña and Opitz, B. and
Ostrowski, M. and Oya, I. and Panter, M. and Parsons, R. D.
and Arribas, M. Paz and Pekeur, N. W. and Pelletier, G. and
Perez, J. and Petrucci, P. -O. and Peyaud, B. and Pita, S.
and Poon, H. and Pühlhofer, G. and Punch, M. and
Quirrenbach, A. and Raab, S. and Raue, M. and Reichardt, I.
and Reimer, A. and Reimer, O. and Renaud, M. and Reyes, R.
de los and Rieger, F. and Rob, L. and Romoli, C. and
Rosier-Lees, S. and Rowell, G. and Rudak, B. and Rulten, C.
B. and Sahakian, V. and Sanchez, D. A. and Santangelo, A.
and Schlickeiser, R. and Schüssler, F. and Schulz, A. and
Schwanke, U. and Schwarzburg, S. and Schwemmer, S. and Sol,
H. and Spengler, G. and Spies, F. and Stawarz, Ł. and
Steenkamp, R. and Stegmann, C. and Stinzing, F. and Stycz,
K. and Sushch, I. and Tavernet, J. -P. and Tavernier, T. and
Taylor, A. M. and Terrier, R. and Tluczykont, M. and
Trichard, C. and Valerius, K. and van Eldik, C. and van
Soelen, B. and Vasileiadis, G. and Venter, C. and Viana, A.
and Vincent, P. and Völk, H. J. and Volpe, F. and Vorster,
M. and Vuillaume, T. and Wagner, S. J. and Wagner, P. and
Wagner, R. M. and Ward, M. and Weidinger, M. and Weitzel, Q.
and White, R. and Wierzcholska, A. and Willmann, P. and
Wörnlein, A. and Wouters, D. and Yang, R. and Zabalza, V.
and Zacharias, M. and Zdziarski, A. A. and Zech, A. and
Zechlin, H. -S. and Acero, F. and Casandjian, J. M. and
Cohen-Tanugi, J. and Giordano, F. and Guillemot, L. and
Lande, J. and Pletsch, H. and Uchiyama, Y.},
collaboration = {H.E.S.S.{ Collaboration} and Fermi-{LAT Collaboration}},
title = {{P}robing the {G}amma-{R}ay {E}mission from {HESS}
{J}1834-087 using {H}.{E}.{S}.{S}. and {F}ermi {LAT}
{O}bservations},
journal = {Astronomy and astrophysics},
volume = {574},
number = {10},
issn = {0004-6361},
address = {Les Ulis},
publisher = {EDP Sciences},
reportid = {PUBDB-2014-04512, arXiv:1407.0862},
pages = {A27},
year = {2015},
note = {OA},
abstract = {Previous observations with HESS have revealed the existence
of an extended very-high-energy (VHE; E>100 GeV) gamma-ray
source, HESS J1834-087, coincident with the SNR W41. The
origin of the gamma-ray emission has been further
investigated with HESS and the Fermi-LAT. The gamma-ray data
provided by 61h (HESS) and 4 yrs (Fermi LAT) of observations
cover over 5 decades in energy (1.8GeV - 30TeV). The
morphology and spectrum of the TeV and GeV sources have been
studied and multi-wavelength data have been used to
investigate the origin of the observed emission. The TeV
source can be modeled with a sum of two components: one
point-like and one significantly extended $(sig_TeV$ =
$0.17{\deg}),$ both centered on SNR W41 and exhibiting
spectra described by a power law of index 2.6. The GeV
source detected with Fermi is extended $(sig_GeV$
$=0.15{\deg})$ and morphologically matches the VHE emission.
Its spectrum can be described by a power-law with index 2.15
and joins smoothly the one of the whole TeV source. A break
appears in the spectra around 100 GeV. Two main scenarios
are proposed to explain the emission: a pulsar wind nebula
(PWN) or the interaction of SNR W41 with a molecular cloud.
X-ray observations suggest the presence of a point-like
source (pulsar candidate) near the center of the SNR and
non-thermal X-ray diffuse emission which could arise from a
potential PWN. The PWN scenario is supported by the match of
of the TeV and GeV positions with the putative pulsar.
However, the overall spectrum is reproduced by a 1-zone
leptonic model only if an excess of low-energy electrons is
injected by a high spin-down power pulsar. This low-energy
component is not needed if 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 maser lines and the hadronic modeling.},
cin = {ZEU-EXP/AT},
ddc = {520},
cid = {$I:(DE-H253)ZEU-EXP_AT-20120731$},
pnm = {613 - Matter and Radiation from the Universe (POF3-613) /
P-WIND - New light on the gamma-ray sky: unveiling
cosmic-ray accelerators in the Milky Way and their relation
to pulsar wind nebulae (259391)},
pid = {G:(DE-HGF)POF3-613 / G:(EU-Grant)259391},
experiment = {EXP:(DE-MLZ)NOSPEC-20140101},
typ = {PUB:(DE-HGF)29 / PUB:(DE-HGF)16},
eprint = {1407.0862},
howpublished = {arXiv:1407.0862},
archivePrefix = {arXiv},
SLACcitation = {$\%\%CITATION$ = $arXiv:1407.0862;\%\%$},
UT = {WOS:000349467000027},
doi = {10.1051/0004-6361/201322694},
url = {https://bib-pubdb1.desy.de/record/193081},
}
guest ::