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@ARTICLE{Collaboration:317105,
author = {Abdalla, H. and Abramowski, A. and Aharonian, F. and
Benkhali, F. Ait and Akhperjanian, A. G. and Andersson, T.
and Angüner, E. O. and Arakawa, M. and Arrieta, M. and
Aubert, P. and Backes, M. and Balzer, A. and Barnard, M. and
Becherini, Y. and Tjus, J. Becker and Berge, D. and
Bernhard, S. and Bernlöhr, K. and Blackwell, R. and
Böttcher, M. and Boisson, C. and Bolmont, J. and Bordas, P.
and Bregeon, J. and Brun, F. and Brun, P. and Bryan, M. and
Büchele, M. and Bulik, T. and Capasso, M. and Carr, J. and
Casanova, S. and Cerruti, M. and Chakraborty, N. and
Chalme-Calvet, R. and Chaves, R. C. G. and Chen, A. and
Chevalier, J. and Chrétien, M. and Coffaro, M. and
Colafrancesco, S. and Cologna, G. and Condon, B. and Conrad,
J. and Cui, Y. and Davids, I. D. and Decock, J. and
Degrange, B. and Deil, C. and Devin, J. and deWilt, P. and
Dirson, L. and Djannati-Ataï, A. and Domainko, W. and
Donath, A. and Drury, L. O'C. and Dutson, K. and Dyks, J.
and Edwards, T. and Egberts, K. and Eger, P. and Ernenwein,
J. -P. and Eschbach, S. and Farnier, C. and Fegan, S. and
Fern, M. V. and Fiasson, A. and Fontaine, G. and Förster,
A. and Funk, S. and Füßling, M. and Gabici, S. and Gajdus,
M. and Gallant, Y. A. and Garrigoux, T. and Giavitto, G. and
Giebels, B. and Glicenstein, J. F. and Gottschall, D. and
Goyal, A. and Grondin, M. -H. and Hahn, J. and Haupt, M. and
Hawkes, J. and Heinzelmann, G. and Henri, G. and Hermann, G.
and Hervet, O. and Hinton, J. A. and Hofmann, W. and
Hoischen, C. and Holler, M. and Horns, D. and Ivascenko, A.
and Iwasaki, H. and Jacholkowska, A. and Jamrozy, M. and
Janiak, M. and Jankowsky, D. and Jankowsky, F. and Jingo, M.
and Jogler, T. and Jouvin, L. and Jung-Richardt, I. and
Kastendieck, M. A. and Katarzyński, K. and Katsuragawa, M.
and Katz, U. and Kerszberg, D. and Khangulyan, D. and
Khélifi, B. and Kieffer, M. and King, J. and Klepser, S.
and Klochkov, D. and Kluźniak, W. and Kolitzus, D. and
Komin, Nu. and Kosack, K. and Krakau, S. and Kraus, M. and
Krüger, P. P. and Laffon, H. and Lamanna, G. and Lau, J.
and Lees, J. -P. and Lefaucheur, J. and Lefranc, V. and
Lemière, A. and Lemoine-Goumard, M. and Lenain, J. -P. and
Leser, E. and Lohse, T. and Lorentz, M. and Liu, R. and
López-Coto, R. and Lypova, I. and Mar, V. and Marcowith, A.
and Mariaud, C. and Marx, R. and Maurin, G. and Maxted, N.
and Mayer, M. and Meintjes, P. J. and Meyer, M. and
Mitchell, A. M. W. and Moderski, R. and Mohamed, M. and
Mohrmann, L. and Morå, K. and Moulin, E. and Murach, T. and
Nakashima, S. and de Naurois, M. and Niederwanger, F. and
Niemiec, J. and Oakes, L. and O'Brien, P. and Odaka, H. and
Öttl, S. and Ohm, S. and Ostrowski, M. and Oya, I. and
Padovani, M. and Panter, M. and Parsons, R. D. and Arribas,
M. Paz and Pekeur, N. W. and Pelletier, G. and Perennes, C.
and Petrucci, P. -O. and Peyaud, B. and Piel, Q. and Pita,
S. and Poon, H. and Prokhorov, D. and Prokoph, H. and
Pühlhofer, G. and Punch, M. and Quirrenbach, A. and Raab,
S. and Reimer, A. and Reimer, O. and Renaud, M. and Reyes,
R. de los and Richter, S. and Rieger, F. and Romoli, C. and
Rowell, G. and Rudak, B. and Rulten, C. B. and Sahakian, V.
and Saito, S. and Salek, D. and Sanchez, D. A. and
Santangelo, A. and Sasaki, M. and Schlickeiser, R. and
Schüssler, F. and Schulz, A. and Schwanke, U. and
Schwemmer, S. and Seglar-Arroyo, M. and Settimo, M. and
Seyffert, A. S. and Shafi, N. and Shilon, I. and Simoni, R.
and Sol, H. and Spanier, F. and Spengler, G. and Spies, F.
and Stawarz, Ł. and Steenkamp, R. and Stegmann, C. and
Stycz, K. and Sushch, I. and Takahashi, T. and Tavernet, J.
-P. and Tavernier, T. and Taylor, A. M. and Terrier, R. and
Tibaldo, L. and Tiziani, D. and Tluczykont, M. and Trichard,
C. and Tsuji, N. and Tuffs, R. and Uchiyama, Y. and van der
Walt, D. J. and van Eldik, C. and van Rensburg, C. and van
Soelen, B. and Vasileiadis, G. and Veh, J. and Venter, C.
and Viana, A. and Vincent, P. and Vink, J. and Voisin, F.
and Völk, H. J. and Vuillaume, T. and Wadiasingh, Z. and
Wagner, S. J. and Wagner, P. and Wagner, R. M. and White, R.
and Wierzcholska, A. and Willmann, P. and Wörnlein, A. and
Wouters, D. and Yang, R. and Zabalza, V. and Zaborov, D. and
Zacharias, M. and Zanin, R. and Zdziarski, A. A. and Zech,
A. and Zefi, F. and Ziegler, A. and Żywucka, N.},
collaboration = {H.E.S.S.{ Collaboration}},
title = {{D}eeper {H}.{E}.{S}.{S}. {O}bservations of {V}ela {J}unior
({RX} {J}0852.0-4622) : {M}orphology {S}tudies and
{R}esolved {S}pectroscopy},
reportid = {PUBDB-2017-00446},
year = {2016},
note = {Manuscript submitted to $A\&A$},
abstract = {The gamma-ray emission from the shell-type supernova
remnant (SNR) RX J0852.0-4622 is studied in order to better
characterize its spectral properties and its distribution
over the SNR.Methods. The analysis of an extended H.E.S.S.
data set at very-high energies (E > 100 GeV) permits
detailed studies of the morphology and the spectrum of the
whole RX J0852.0-4622 region, as well as spatially-resolved
spectroscopy. 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 cut-off at an energy of Ecut =
(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 cut-off. 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.},
cin = {ZEU-HESS},
cid = {I:(DE-H253)ZEU-HESS-20140213},
pnm = {613 - Matter and Radiation from the Universe (POF3-613)},
pid = {G:(DE-HGF)POF3-613},
experiment = {EXP:(DE-H253)HESS-20170101},
typ = {PUB:(DE-HGF)25},
eprint = {1611.01863},
howpublished = {arXiv:1611.01863},
archivePrefix = {arXiv},
SLACcitation = {$\%\%CITATION$ = $arXiv:1611.01863;\%\%$},
doi = {10.3204/PUBDB-2017-00446},
url = {https://bib-pubdb1.desy.de/record/317105},
}
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