MAGIC observations provide compelling evidence of hadronic multi-TeV emission from the putative PeVatron SNR G106.3+2.7

被引：15

作者：

Abe, H. ^{[1
]}

Abe, S. ^{[1
]}

Acciari, V. A. ^{[2
,3
,8
]}

Agudo, I. ^{[4
]}

Aniello, T. ^{[5
]}

Ansoldi, S. ^{[6
,7
,56
]}

Antonelli, L. A. ^{[5
]}

Arbet Engels, A. ^{[8
]}

Arcaro, C. ^{[9
,10
]}

Artero, M. ^{[11
]}

Asano, K. ^{[1
]}

Baack, D. ^{[12
]}

Babic, A. ^{[13
]}

Baquero, A. ^{[14
,15
]}

Barres de Almeida, U. ^{[16
]}

Barrio, J. A. ^{[14
,15
]}

Batkovic, I. ^{[9
,10
]}

Baxter, J. ^{[1
]}

Becerra Gonzalez, J. ^{[2
,3
]}

Bednarek, W. ^{[17
]}

Bernardini, E. ^{[9
,10
]}

Bernardos, M. ^{[4
]}

Berti, A. ^{[8
]}

Besenrieder, J. ^{[8
]}

Bhattacharyya, W. ^{[18
]}

Bigongiari, C. ^{[5
]}

Biland, A. ^{[19
]}

Blanch, O. ^{[11
]}

Bonnoli, G. ^{[5
]}

Bosnjak, Z. ^{[13
]}

Burelli, I. ^{[6
,7
]}

Busetto, G. ^{[9
,10
]}

Carosi, R. ^{[20
,21
]}

Carretero-Castrillo, M. ^{[22
]}

Castro-Tirado, A. J. ^{[4
]}

Ceribella, G. ^{[1
]}

Chai, Y. ^{[8
]}

Chilingarian, A. ^{[23
]}

Cikota, S. ^{[13
]}

Colombo, E. ^{[2
,3
]}

Contreras, J. L. ^{[14
,15
]}

Cortina, J. ^{[24
]}

Covino, S. ^{[5
]}

D'Amico, G. ^{[25
]}

D'Elia, V. ^{[5
]}

Da Vela, P. ^{[5
,20
,21
]}

Dazzi, F. ^{[5
]}

De Angelis, A. ^{[9
,10
]}

De Lotto, B. ^{[6
,7
]}

Del Popolo, A. ^{[26
,27
]}

机构：

[1] Univ Tokyo, Japanese MAGIC Grp, Inst Cosm Ray Res ICRR, Kashiwa, Chiba 2778582, Japan

[2] Univ La Laguna, Inst Astrofis Canarias, San Cristobal la Laguna 38200, Spain

[3] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38200, Spain

[4] CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, Granada 18008, Spain

[5] Natl Inst Astrophys INAF, I-00136 Rome, Italy

[6] Univ Udine, I-33100 Udine, Italy

[7] INFN Trieste, I-33100 Udine, Italy

[8] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

[9] Univ Padua, I-35131 Padua, Italy

[10] INFN, I-35131 Padua, Italy

[11] Barcelona Inst Sci & Technol BIST, Inst Fis Altes Energies IFAE, Bellaterra 08193, Barcelona, Spain

[12] Tech Univ Dortmund, D-44221 Dortmund, Germany

[13] Univ Zagreb, Fac Elect Engn & Comp FER, Croatian MAGIC Grp, Zagreb 10000, Croatia

[14] Univ Complutense Madrid, IPARCOS Inst, Madrid 28040, Spain

[15] Univ Complutense Madrid, EMFTEL Dept, Madrid 28040, Spain

[16] Ctr Brasileiro Pesquisas Fis CBPF, BR-22290180 Rio De Janeiro, RJ, Brazil

[17] Univ Lodz, Fac Phys & Appl Informat, Dept Astrophys, PL-90236 Lodz, Poland

[18] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

[19] Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland

[20] Univ Pisa, I-56126 Pisa, Italy

[21] INFN Pisa, I-56126 Pisa, Italy

[22] Univ Barcelona, ICCUB, IEEC UB, Barcelona 08028, Spain

[23] A Alikhanyan Natl Sci Lab, Armenian MAGIC Grp, Yerevan 0036, Armenia

[24] Ctr Invest Energet Medioambient & Tecnol, Madrid 28040, Spain

[25] Univ Bergen, Dept Phys & Technol, N-5007 Bergen, Norway

[26] INFN, Sez Catania, INFN MAGIC Grp, I-95123 Catania, Italy

[27] Univ Catania, Dipartimento Fis & Astron, I-95123 Catania, Italy

[28] INFN, Sez Torino, INFN MAGIC Grp, I-10125 Turin, Italy

[29] Univ Torino, I-10125 Turin, Italy

[30] INFN, Sez Bari, INFN MAGIC Grp, I-70125 Bari, Italy

[31] Univ Politecn Bari, Dipartimento Interateneo Fis, I-70125 Bari, Italy

[32] Univ Rijeka, Fac Phys, Croatian MAGIC Grp, Rijeka 51000, Croatia

[33] Univ Wurzburg, D-97074 Wurzburg, Germany

[34] Univ Geneva, Chemin Ecogia 16, CH-1290 Versoix, Switzerland

[35] Univ Turku, ESO, Finnish Ctr Astron, Finnish MAGIC Grp, Turku 20014, Finland

[36] Univ Autonoma Barcelona, Dept Fis, Bellaterra 08193, Spain

[37] Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain

[38] Hiroshima Univ, Grad Sch Adv Sci & Engn, Phys Program, Japanese MAGIC Grp, Hiroshima 7398526, Japan

[39] ICRANet Armenia, Armenian MAGIC Grp, Yerevan 0019, Armenia

[40] Univ Split, Mech Engn & Naval Architecture FESB, Fac Elect Engn, Croatian MAGIC Grp, Split 21000, Croatia

[41] Josip Juraj Strossmayer Univ Osijek, Dept Phys, Croatian MAGIC Grp, Osijek 31000, Croatia

[42] Tokai Univ, Dept Phys, Japanese MAGIC Grp, Hiratsuka, Kanagawa 2591292, Japan

[43] Univ Siena, I-53100 Siena, Italy

[44] INFN Pisa, I-53100 Siena, Italy

[45] A CI Homi Bhabha Natl Inst, Saha Inst Nucl Phys, Kolkata 700064, India

[46] Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, Sofia 1784, Bulgaria

[47] Yamagata Univ, Dept Phys, Japanese MAGIC Grp, Yamagata 9908560, Japan

[48] Univ Oulu, Space Phys & Astron Res Unit, Finnish MAGIC Grp, Oulu 90014, Finland

[49] Kyoto Univ, Dept Phys, Japanese MAGIC Grp, Kyoto 6068502, Japan

[50] Nagoya Univ, Inst Space Earth Environm Res, Japanese MAGIC Grp, Nagoya, Aichi 4646801, Japan

来源：

ASTRONOMY & ASTROPHYSICS | 2023年 / 671卷

基金：

芬兰科学院;

关键词：

acceleration of particles; cosmic rays; gamma rays: general; gamma rays: ISM; ISM: clouds; ISM: supernova remnants; GAMMA-RAY EMISSION; SUPERNOVA REMNANT G106.3+2.7; HIGH-ENERGY ELECTRONS; GALACTIC-PLANE; X-RAY; SHOCK ACCELERATION; PULSAR; TELESCOPE; SPECTRUM; RADIATION;

D O I：

10.1051/0004-6361/202244931

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Certain types of supernova remnants (SNRs) in our Galaxy are assumed to be PeVatrons, capable of accelerating cosmic rays (CRs) to similar 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 gamma-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 gamma-ray emission is leptonic or hadronic. Aims. With the better angular resolution provided by new MAGIC data compared to earlier gamma-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 degrees 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 similar to 0.2 TeV, and the angular resolution is 0.07-0.1 degrees. We examined the gamma-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 gamma-rays, and 10 TeV gamma-rays to model the emission mechanism precisely. Results. We detect extended gamma-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 gamma-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 AS gamma 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 similar to 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 gamma-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 similar to PeV, while the emission mechanism of the head region could either be hadronic or leptonic.

引用

页数：12

共 55 条

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