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@ARTICLE{Abdalla:418021,
author = {Abdalla, H. and Abramowski, A. and Aharonian, F. and Ait
Benkhali, F. 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 Becker Tjus, J. 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 $Djannati-Ata\'i,$ 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
Fernandes, 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 Marandon,
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 Paz Arribas, M. 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 de los Reyes, R. 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, Anneli 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 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}. observations of {V}ela {J}unior
({RX} {J}0852.0−4622): {M}orphology studies and resolved
spectroscopy},
journal = {Astronomy and astrophysics},
volume = {612},
issn = {1432-0746},
address = {Les Ulis},
publisher = {EDP Sciences},
reportid = {PUBDB-2019-00149, arXiv:1611.01863},
pages = {A7},
year = {2018},
note = {(c) ESO},
abstract = {Aims. We study γ-ray emission from the shell-type
supernova remnant (SNR) RX J0852.0−4622 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 RX J0852.0−4622 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 Ecut = (6.7 ± 1.2stat ± 1.2syst)
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.Key words: astroparticle physics / gamma
rays: general / acceleration of particles / cosmic rays /
ISM: supernova remnants★ A FITS image of the region of
interest and two text files describingthe H.E.S.S. spectrum
of RX J0852.0–4622 are only available at the CDS via
anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or
viahttp://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/612/A7†
Deceased.},
keywords = {gamma ray: emission (INSPIRE) / model: hadronic (INSPIRE) /
particle: acceleration (INSPIRE) / HESS (INSPIRE) / spectral
(INSPIRE) / one-particle (INSPIRE) / supernova (INSPIRE) /
pulsar (INSPIRE) / GLAST (INSPIRE) / VHE (INSPIRE)},
cin = {ZEU-HESS},
ddc = {520},
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)29 / PUB:(DE-HGF)16},
eprint = {1611.01863},
howpublished = {arXiv:1611.01863},
archivePrefix = {arXiv},
SLACcitation = {$\%\%CITATION$ = $arXiv:1611.01863;\%\%$},
UT = {WOS:000429404700007},
doi = {10.1051/0004-6361/201630002},
url = {https://bib-pubdb1.desy.de/record/418021},
}
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