Cosmic-ray acceleration and escape from supernova remnant W44 as probed by Fermi-LAT and MAGIC

被引：1

作者：

Abe, S. ^{[1
]}

Abhir, J. ^{[2
]}

Abhishek, A. ^{[3
,4
]}

Acciari, V. A. ^{[5
,6
]}

Aguasca-Cabot, A. ^{[7
]}

Agudo, I. ^{[8
]}

Aniello, T. ^{[9
]}

Ansoldi, S. ^{[10
,11
,55
]}

Antonelli, L. A. ^{[9
]}

Engels, A. Arbet ^{[12
]}

Arcaro, C. ^{[13
,14
]}

Asano, K. ^{[1
]}

Babic, A. ^{[15
]}

Baquero, A. ^{[16
,17
]}

Barres de Almeida, U. ^{[18
]}

Barrio, J. A. ^{[16
,17
]}

Batkovic, I. ^{[13
,14
]}

Bautista, A. ^{[12
]}

Baxter, J. ^{[1
]}

Becerra Gonzalez, J. ^{[5
,6
]}

Bednarek, W. ^{[19
]}

Bernardini, E. ^{[13
,14
]}

Bernete, J. ^{[20
]}

Berti, A. ^{[12
]}

Besenrieder, J. ^{[12
]}

Bigongiari, C. ^{[9
]}

Biland, A. ^{[2
]}

Blanch, O. ^{[21
]}

Bonnoli, G. ^{[9
]}

Bosnjak, Z. ^{[15
]}

Bronzini, E. ^{[9
]}

Burelli, I. ^{[10
,11
]}

Busetto, G. ^{[13
,14
]}

Campoy-Ordaz, A. ^{[22
,23
]}

Carosi, A. ^{[9
]}

Carosi, R. ^{[24
,25
]}

Carretero-Castrillo, M. ^{[7
]}

Castro-Tirado, A. J. ^{[8
]}

Cerasole, D. ^{[26
,27
]}

Ceribella, G. ^{[12
]}

Chai, Y. ^{[12
]}

Chilingarian, A. ^{[28
]}

Cifuentes, A. ^{[20
]}

Colombo, E. ^{[5
,6
]}

Contreras, J. L. ^{[16
,17
]}

Cortina, J. ^{[20
]}

Covino, S. ^{[9
]}

D'Amico, G. ^{[29
]}

D'Elia, V. ^{[9
]}

Da Vela, P. ^{[9
]}

机构：

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

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

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

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

[5] Uni La Laguna, Inst Astrofis Canarias, San Cristobal la Laguna 38200, Spain

[6] Uni La Laguna, Dept Astrofis, San Cristobal la Laguna 38200, Spain

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

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

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

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

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

[12] Max Planck Inst Phys & Astrophys, D-85748 Garching, Germany

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

[14] INFN, I-35131 Padua, Italy

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

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

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

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

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

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

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

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

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

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

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

[26] Univ Politecn Bari, INFN MAGIC Grp, INFN, Sez Bari, I-70125 Bari, Italy

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

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

[29] Univ Bergen, Dept Phys & Technol, Bergen, Norway

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

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

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

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

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

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

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

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

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

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

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

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

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

[43] Univ Turku, Dept Phys & Astron, Finnish MAGIC Grp, Finnish Ctr Astron ESO, Turku 20014, Finland

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

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

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

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

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

[49] Chiba Univ, ICEHAP, Japanese MAGIC Grp, Chiba 2638522, Japan

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

来源：

ASTRONOMY & ASTROPHYSICS | 2025年 / 693卷

基金：

芬兰科学院; 瑞典研究理事会; 美国国家航空航天局;

关键词：

acceleration of particles; diffusion; cosmic rays; ISM: supernova remnants; gamma rays: general; GAMMA-RAY; RADIO-EMISSION; LIKELIHOOD ANALYSIS; MAJOR UPGRADE; TELESCOPE; PERFORMANCE; MORPHOLOGY; SPECTRUM; CLOUDS; LIMITS;

D O I：

10.1051/0004-6361/202449748

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The supernova remnant (SNR) W44 and its surroundings are a prime target for studying the acceleration of cosmic rays (CRs). Several previous studies established an extended gamma-ray emission that is set apart from the radio shell of W44. This emission is thought to originate from escaped high-energy CRs that interact with a surrounding dense molecular cloud complex. Aims. We present a detailed analysis of Fermi-LAT data with an emphasis on the spatial and spectral properties of W44 and its surroundings. We also report the results of the observations performed with the MAGIC telescopes of the northwestern region of W44. Finally, we present an interpretation model to explain the gamma-ray emission of the SNR and its surroundings. Methods. We first performed a detailed spatial analysis of 12 years of Fermi-LAT data at energies above 1 GeV, in order to exploit the better angular resolution, while we set a threshold of 100MeV for the spectral analysis. We performed a likelihood analysis of 174 hours of MAGIC data above 130 GeV using the spatial information obtained with Fermi-LAT. Results. The combined spectra of Fermi-LAT and MAGIC, extending from 100MeV to several TeV, were used to derive constraints on the escape of CRs. Using a time-dependent model to describe the particle acceleration and escape from the SNR, we show that the maximum energy of the accelerated particles has to be similar or equal to 40 GeV. However, our gamma-ray data suggest that a small number of lower-energy particles also needs to escape. We propose a novel model, the broken-shock scenario, to account for this effect and explain the gamma-ray emission.

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