University of Oulu

MAGIC Collaboration:, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Babić, A., Banerjee, B., Bangale, P., Barres de Almeida, U., Barrio, J. A., Becerra González, J., Bednarek, W., Bernardini, E., Berti, A., Bhattacharyya, W., Biasuzzi, B., Biland, A., Blanch, O., Bonnoli, G., … Smits, R. Statistics of VHE γ-rays in temporal association with radio giant pulses from the Crab pulsar A&A 634 A25 (2020),

Statistics of VHE γ-rays in temporal association with radio giant pulses from the Crab pulsar

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Author: Ahnen, M. L.1; Ansoldi, S.2,3,4,5,6; Antonelli, L. A.7;
Arcaro, C.8,9; Babic, A.10,11,12,13,14; Banerjee, B.15; Bangale, P.16; de Almeida, U. Barres16,17; Barrio, J. A.18; Becerra Gonzalez, J.19,20; Bednarek, W.21; Bernardini, E.22,23; Berti, A.2,3,24; Bhattacharyya, W.22; Biasuzzi, B.2,3; Biland, A.1; Blanch, O.25; Bonnoli, G.26,27; Carosi, R.26,27; Carosi, A.7; Chatterjee, A.15; Colak, S. M.25; Colin, P.16; Colombo, E.19,20; Contreras, J. L.18; Cortina, J.25; Covino, S.7; Cumani, P.25; De Vela, P.26,27; Dazzi, F.7; De Angelis, A.8,9; De Lotto, B.2,3; Di Pierro, F.8,9; Doert, M.28; Dominguez, A.18; Prester, D. Dominis10,11,12,13,14; Dorner, D.29; Doro, M.8,9; Einecke, S.28; Glawion, D. Eisenacher29; Elsaesser, D.28; Engelkemeier, M.28; Ramazani, V. Fallah30,31,32; Fernandez-Barral, A.25; Fidalgo, D.18; Fonseca, M., V18; Font, L.33,34; Fruck, C.16; Galindo, D.35; Garcia Lopez, R. J.19,20; Garczarczyk, M.22; Gaug, M.33,34; Giammaria, P.7; Godinovic, N.10,11,12,13,14; Gora, D.22; Guberman, D.25; Hadasch, D.4,5,6; Hahn, A.16; Hassan, T.25; Hayashida, M.4,5,6; Herrera, J.19,20; Hose, J.16; Hrupec, D.10,11,12,13,14; Ishio, K.16; Konno, Y.4,5,6; Kubo, H.4,5,6; Kushida, J.4,5,6; Kuvezdic, D.10,11,12,13,14; Lelas, D.10,11,12,13,14; Lewandowska, N.29,36,37; Lindfors, E.30,31,32; Lombardi, S.7; Longo, F.2,3,24; Lopez, M.18; Maggio, C.33,34; Majumdar, P.15; Makariev, M.38; Maneva, G.38; Manganaro, M.10,11,12,13,14; Mannheim, K.29; Maraschi, L.7; Mariotti, M.8,9; Martinez, M.25; Mazin, D.4,5,6,16; Menzel, U.16; Minev, M.38; Miranda, J. M.26,27; Mirzoyan, R.16; Moralejo, A.25; Moreno, V33,34; Moretti, E.16; Nagayoshi, T.4,5,6; Neustroev, V30,31,32; Niedzwiecki, A.21; Nievas Rosillo, M.18; Nigro, C.22; Nilsson, K.30,31,32; Ninci, D.25; Nishijima, K.4,5,6; Noda, K.25; Nogues, L.25; Paiano, S.8,9; Palacio, J.25; Paneque, D.16; Paoletti, R.26,27; Paredes, J. M.35; Pedaletti, G.22; Peresano, M.2,3; Perri, L.7; Persic, M.2,3,39,40; Moroni, P. G. Prada41,42; Prandini, E.8,9; Puljak, I10,11,12,13,14; Garcia, J. R.16; Reichardt, I8,9; Rhode, W.28; Ribo, M.35; Rico, J.25; Righi, C.7; Rugliancich, A.26,27; Saito, T.4,5,6; Satalecka, K.22; Schroeder, S.28; Schweizer, T.16; Shore, S. N.41,42; Sitarek, J.21; Snidaric, I10,11,12,13,14; Sobczynska, D.21; Stamerra, A.7; Strzys, M.16; Suric, T.10,11,12,13,14; Takalo, L.30,31,32; Tavecchio, F.7; Temnikov, P.38; Terzic, T.10,11,12,13,14; Teshima, M.4,5,6,16; Torres-Alba, N.35; Treves, A.2,3; Tsujimoto, S.4,5,6; Vanzo, G.19,20; Vazquez Acosta, M.19,20; Vovk, I16; Ward, J. E.25; Will, M.16; Zaric, D.10,11,12,13,14; Smits, R.43
Organizations: 1Swiss Fed Inst Technol, CH-8093 Zurich, Switzerland.
2Univ Udine, I-33100 Udine, Italy.
3INFN Trieste, I-33100 Udine, Italy.
4Univ Tokyo, Japanese Mag Consortium ICRR, Chiba 2778582, Japan.
5Kyoto Univ, Dept Phys, Kyoto 6068502, Japan.
6Tokai Univ, Tokai, Kanagawa 2591292, Japan.
7Natl Inst Astrophys INAF, I-00136 Rome, Italy.
8Univ Padua, I-35131 Padua, Italy.
9Ist Nazl Fis Nucl, I-35131 Padua, Italy.
10Univ Rijeka, Dept Phys, Croatian Mag Consortium, Rijeka 51000, Croatia.
11Univ Split, FESB, Split 21000, Croatia.
12Univ Zagreb, FER, Zagreb 10000, Croatia.
13Univ Osijek, Osijek 31000, Croatia.
14Rudjer Boskovic Inst, Zagreb 10000, Croatia.
15HBNI, Saha Inst Nucl Phys, 1-AF Bidhannagar,Sect 1, Kolkata 700064, India.
16Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany.
17Urca, CBPF, BR-22290180 Rio De Janeiro, RJ, Brazil.
18Univ Complutense, E-28040 Madrid, Spain.
19Inst Astrofis Canarias, E-38200 Tenerife, Spain.
20Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain.
21Univ Lodz, Dept Astrophys, PL-90236 Lodz, Poland.
22DESY, D-15738 Zeuthen, Germany.
23Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany.
24Universit Trieste, Dipartimento Fis, I-34127 Trieste, Italy.
25BIST, IFAE, Barcelona 08193, Spain.
26Univ Siena, I-53100 Siena, Italy.
27INFN Pisa, I-53100 Siena, Italy.
28Tech Univ Dortmund, D-44221 Dortmund, Germany.
29Univ Wurzburg, D-97074 Wurzburg, Germany.
30Univ Turku, Finnish MAG Consortium, Tuorla Observ, Vaisalantie 20, Piikkio 21500, Finland.
31Univ Turku, Finnish Ctr Astron, ESO FINCA, Vaisalantie 20, Piikkio 21500, Finland.
32Univ Oulu, Astron Div, Oulu 90014, Finland.
33Univ Autonoma Barcelona, Dept Fis, Bellaterra 08193, Spain.
34Univ Autonoma Barcelona, CERES IEEC, Bellaterra 08193, Spain.
35Univ Barcelona, ICC, IEEC UB, E-08028 Barcelona, Spain.
36West Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
37West Virginia Univ, Ctr Gravitat Waves & Cosmol, Chestnut Ridge Res Bldg, Morgantown, WV 26505 USA.
38Bulgarian Acad Sci, Inst Nucl Res & Nucl Energy, BU-1784 Sofia, Bulgaria.
39Univ Bologna, INAF Trieste, Bologna, Italy.
40Univ Bologna, Dept Phys & Astron, Bologna, Italy.
41Univ Pisa, I-56126 Pisa, Italy.
42INFN Pisa, I-56126 Pisa, Italy.
43ASTRON, POB 2, NL-7990 Dwingeloo, Netherlands.
Format: article
Version: published version
Access: open
Online Access: PDF Full Text (PDF, 0.6 MB)
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Language: English
Published: EDP Sciences, 2020
Publish Date: 2020-06-18


Aims: The aim of this study is to search for evidence of a common emission engine between radio giant pulses (GPs) and very-high-energy (VHE, E > 100 GeV) γ-rays from the Crab pulsar.

Methods: We performed 16 h of simultaneous observations of the Crab pulsar at 1.4 GHz with the Effelsberg radio telescope and the Westerbork Synthesis Radio Telescope (WSRT), and at energies above 60 GeV we used the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes. We searched for a statistical correlation between the radio and VHE γ-ray emission with search windows of different lengths and different time lags to the arrival times of a radio GP. A dedicated search for an enhancement in the number of VHE γ-rays correlated with the occurrence of radio GPs was carried out separately for the P1 and P2 phase ranges, respectively.

Results: In the radio data sample, 99444 radio GPs were detected. We find no significant correlation between the GPs and VHE photons in any of the search windows. Depending on phase cuts and the chosen search windows, we find upper limits at a 95% confidence level on an increase in VHE γ-ray events correlated with radio GPs between 7% and 61% of the average Crab pulsar VHE flux for the P1 and P2 phase ranges, respectively. This puts upper limits on the flux increase during a radio GP between 12% and 2900% of the pulsed VHE flux, depending on the search window duration and phase cuts. This is the most stringent upper limit on a correlation between γ-ray emission and radio GPs reported so far.

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Series: Astronomy and astrophysics
ISSN: 0004-6361
ISSN-E: 1432-0746
ISSN-L: 0004-6361
Volume: 634
Article number: A25
DOI: 10.1051/0004-6361/201833555
Type of Publication: A1 Journal article – refereed
Field of Science: 115 Astronomy and space science
Funding: The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064),and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ.
Copyright information: © ESO 2020.