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@ARTICLE{Abe:584597,
author = {Abe, H. and Abe, S. and Acciari, V. A. and Agudo, I. and
Aniello, T. and Ansoldi, S. and Antonelli, L. A. and Engels,
A. Arbet and Arcaro, C. and Artero, M. and Asano, K. and
Baack, D. and Babić, A. and Baquero, A. and de Almeida, U.
Barres and Barrio, J. A. and Batković, I. and Baxter, J.
and Becerra González, J. and Bednarek, W. and Bernardini,
E. and Bernardos, M. and Berti, A. and Besenrieder, J. and
Bhattacharyya, W. and Bigongiari, C. and Biland, A. and
Blanch, O. and Bonnoli, G. and Bošnjak, Ž. and Burelli, I.
and Busetto, G. and Carosi, R. and Carretero-Castrillo, M.
and Castro-Tirado, A. J. and Ceribella, G. and Chai, Y. and
Chilingarian, A. and Cikota, S. and Colombo, E. and
Contreras, J. L. and Cortina, J. and Covino, S. and D'Amico,
G. and D'Elia, V. and Da Vela, P. and Dazzi, F. and De
Angelis, A. and De Lotto, B. and Del Popolo, A. and Delfino,
M. and Delgado, J. and Mendez, C. Delgado and Depaoli, D.
and Di Pierro, F. and Di Venere, L. and Do Souto Espiñeira,
E. and Dominis Prester, D. and Donini, A. and Dorner, D. and
Doro, M. and Elsaesser, D. and Emery, G. and Escudero, J.
and Fallah Ramazani, V. and Fariña, L. and Fattorini, A.
and Font, L. and Fruck, C. and Fukami, S. and Fukazawa, Y.
and López, R. J. García and Garczarczyk, M. and Gasparyan,
S. and Gaug, M. and Paiva, J. G. Giesbrecht and Giglietto,
N. and Giordano, F. and Gliwny, P. and Godinović, N. and
Grau, R. and Green, D. and Green, J. G. and Hadasch, D. and
Hahn, A. and Hassan, T. and Heckmann, L. and Herrera, J. and
Hrupec, D. and Hütten, M. and Imazawa, R. and Inada, T. and
Iotov, R. and Ishio, K. and Martínez, I. Jiménez and
Jormanainen, J. and Kerszberg, D. and Kobayashi, Y. and
Kubo, H. and Kushida, J. and Lamastra, A. and Lelas, D. and
Leone, F. and Lindfors, E. and Linhoff, L. and Lombardi, S.
and Longo, F. and López-Coto, R. and López-Moya, M. and
López-Oramas, A. and Loporchio, S. and Lorini, A. and
Lyard, E. and Fraga, B. Machado de Oliveira and Majumdar, P.
and Makariev, M. and Maneva, G. and Mang, N. and Manganaro,
M. and Mangano, S. and Mannheim, K. and Mariotti, M. and
Martínez, M. and Aguilar, A. Mas and Mazin, D. and
Menchiari, S. and Mender, S. and Mićanović, S. and Miceli,
D. and Miener, T. and Miranda, J. M. and Mirzoyan, R. and
Molina, E. and Mondal, H. A. and Moralejo, A. and Morcuende,
D. and Moreno, V. and Nakamori, T. and Nanci, C. and Nava,
L. and Neustroev, V. and Nievas Rosillo, M. and Nigro, C.
and Nilsson, K. and Nishijima, K. and Ekoume, T. Njoh and
Noda, K. and Nozaki, S. and Ohtani, Y. and Oka, T. and
Okumura, A. and Otero-Santos, J. and Paiano, S. and
Palatiello, M. and Paneque, D. and Paoletti, R. and Paredes,
J. M. and Pavletić, L. and Persic, M. and Pihet, M. and
Pirola, G. and Podobnik, F. and Prada Moroni, P. G. and
Prandini, E. and Principe, G. and Priyadarshi, C. and Rhode,
W. and Ribó, M. and Rico, J. and Righi, C. and Rugliancich,
A. and Sahakyan, N. and Saito, T. and Sakurai, S. and
Satalecka, K. and Saturni, F. G. and Schleicher, B. and
Schmidt, K. and Schmuckermaier, F. and Schubert, J. L. and
Schweizer, T. and Sitarek, J. and Sliusar, V. and
Sobczynska, D. and Spolon, A. and Stamerra, A. and
Strišković, J. and Strom, D. and Strzys, M. and Suda, Y.
and Surić, T. and Tajima, H. and Takahashi, M. and
Takeishi, R. and Tavecchio, F. and Temnikov, P. and
Terauchi, K. and Terzić, T. and Teshima, M. and Tosti, L.
and Truzzi, S. and Tutone, A. and Ubach, S. and van
Scherpenberg, J. and Vazquez Acosta, M. and Ventura, S. and
Verguilov, V. and Viale, I. and Vigorito, C. F. and Vitale,
V. and Vovk, I. and Walter, R. and Will, M. and Wunderlich,
C. and Yamamoto, T. and Zarić, D.},
collaboration = {{MAGIC Collaboration}},
title = {{MAGIC} observations provide compelling evidence of
hadronic multi-{T}e{V} emission from the putative
{P}e{V}atron {SNR} {G}106.3+2.7},
journal = {Astronomy and astrophysics},
volume = {671},
issn = {0004-6361},
address = {Les Ulis},
publisher = {EDP Sciences},
reportid = {PUBDB-2023-03148, arXiv:2211.15321},
pages = {A12},
year = {2023},
abstract = {Context. Certain types of supernova remnants (SNRs) in our
Galaxy are assumed to be PeVatrons, capable of accelerating
cosmic rays (CRs) to ~ PeV energies. However, conclusive
observational evidence for this has not yet been found. The
SNR G106.3+2.7, detected at 1–100 TeV energies by
different γ-ray facilities, is one of the most promising
PeVatron candidates. This SNR has a cometary shape, which
can be divided into a head and a tail region with different
physical conditions. However, in which region the 100 TeV
emission is produced has not yet been identified because of
the limited position accuracy and/or angular resolution of
existing observational data. Additionally, it remains
unclear as to whether the origin of the γ-ray emission is
leptonic or hadronic.Aims. With the better angular
resolution provided by new MAGIC data compared to earlier
γ-ray datasets, we aim to reveal the acceleration site of
PeV particles and the emission mechanism by resolving the
SNR G106.3+2.7 with 0.1° resolution at TeV
energies.Methods. We observed the SNR G106.3+2.7 using the
MAGIC telescopes for 121.7 h in total – after quality cuts
– between May 2017 and August 2019. The analysis energy
threshold is ~0.2 TeV, and the angular resolution is
0.07−0.1°. We examined the γ-ray spectra of different
parts of the emission, whilst benefitting from the
unprecedented statistics and angular resolution at these
energies provided by our new data. We also used measurements
at other wavelengths such as radio, X-rays, GeV γ-rays, and
10 TeV γ-rays to model the emission mechanism
precisely.Results. We detect extended γ-ray emission
spatially coincident with the radio continuum emission at
the head and tail of SNR G106.3+2.7. The fact that we detect
a significant γ-ray emission with energies above 6.0 TeV
from only the tail region suggests that the emissions above
10 TeV detected with air shower experiments (Milagro, HAWC,
Tibet ASγ and LHAASO) are emitted only from the SNR tail.
Under this assumption, the multi-wavelength spectrum of the
head region can be explained with either hadronic or
leptonic models, while the leptonic model for the tail
region is in contradiction with the emission above 10 TeV
and X-rays. In contrast, the hadronic model could reproduce
the observed spectrum at the tail by assuming a proton
spectrum with a cutoff energy of ~1 PeV for that region.
Such high-energy emission in this middle-aged SNR (4−10
kyr) can be explained by considering a scenario where
protons escaping from the SNR in the past interact with
surrounding dense gases at present.Conclusions. The γ-ray
emission region detected with the MAGIC telescopes in the
SNR G106.3+2.7 is extended and spatially coincident with the
radio continuum morphology. The multi-wavelength spectrum of
the emission from the tail region suggests proton
acceleration up to ~PeV, while the emission mechanism of the
head region could either be hadronic or leptonic.Key words:
acceleration of particles / cosmic rays / gamma rays:
general / gamma rays: ISM / ISM: clouds / ISM: supernova
remnants★ Corresponding authors: T. Oka, T. Saito, M.
Strzys; e-mail: contact.magic@mpp.mpg.de},
keywords = {model: leptonic (INSPIRE) / p: spectrum (INSPIRE) / energy:
high (INSPIRE) / showers: atmosphere (INSPIRE) / model:
hadronic (INSPIRE) / energy: emission (INSPIRE) / TeV
(INSPIRE) / angular resolution (INSPIRE) / MAGIC (INSPIRE) /
acceleration (INSPIRE) / gas (INSPIRE) / site (INSPIRE) /
air (INSPIRE) / HAWC (INSPIRE) / resolution (INSPIRE) /
X-ray (INSPIRE)},
cin = {$Z_MAGIC$},
ddc = {520},
cid = {$I:(DE-H253)Z_MAGIC-20210408$},
pnm = {613 - Matter and Radiation from the Universe (POF4-613)},
pid = {G:(DE-HGF)POF4-613},
experiment = {EXP:(DE-H253)MAGIC-20170101},
typ = {PUB:(DE-HGF)16},
eprint = {2211.15321},
howpublished = {arXiv:2211.15321},
archivePrefix = {arXiv},
SLACcitation = {$\%\%CITATION$ = $arXiv:2211.15321;\%\%$},
UT = {WOS:000981831300001},
doi = {10.1051/0004-6361/202244931},
url = {https://bib-pubdb1.desy.de/record/584597},
}
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