Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes

Abstract B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to...

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Veröffentlicht in:Monthly Notices of the Royal Astronomical Society 2017-10, Vol.470 (4), p.4608-4617
Hauptverfasser: Ansoldi, S, Antonelli, L. A, Banerjee, B, de Almeida, U. Barres, González, J. Becerra, Berti, A, Biasuzzi, B, Biland, A, Blanch, O, Bonnefoy, S, Bonnoli, G, Borracci, F, Bretz, T, Carosi, A, Chatterjee, A, Colin, P, Colombo, E, Da Vela, P, Dazzi, F, De Angelis, A, Wilhelmi, E. de Oña, Pierro, F. Di, Doert, M, Domínguez, A, Dorner, D, Doro, M, Einecke, S, Glawion, D. Eisenacher, Elsaesser, D, Engelkemeier, M, Ramazani, V. Fallah, Fernández-Barral, A, Fonseca, M. V, Font, L, Fruck, C, Galindo, D, Gaug, M, Giammaria, P, Godinović, N, Gora, D, Griffiths, S, Hadasch, D, Hassan, T, Hughes, G, Ishio, K, Konno, Y, Kushida, J, Kuveždić, D, Lindfors, E, Majumdar, P, Makariev, M, Maneva, G, Manganaro, M, Maraschi, L, Mariotti, M, Mazin, D, Menzel, U, Mirzoyan, R, Moralejo, A, Moreno, V, Moretti, E, Neustroev, V, Niedzwiecki, A, Rosillo, M. Nievas, Nilsson, K, Noda, K, Nogués, L, Paiano, S, Palacio, J, Paneque, D, Paoletti, R, Paredes-Fortuny, X, Pedaletti, G, Perri, L, Persic, M, Poutanen, J, Moroni, P. G. Prada, Prandini, E, Garcia, J. R, Reichardt, I, Rhode, W, Ribó, M, Rico, J, Saito, T, Schroeder, S, Šnidarić, I, Sobczynska, D, Takalo, L, Tavecchio, F, Temnikov, P, Terzić, T, Teshima, M, Torres-Albà, N, Vanzo, G, Ward, J. E, Wu, M. H, Zarić, D, Collaboration), (MAGIC, Cognard, I, Guillemot, L
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container_title Monthly Notices of the Royal Astronomical Society
container_volume 470
creator Ansoldi, S
Antonelli, L. A
Banerjee, B
de Almeida, U. Barres
González, J. Becerra
Berti, A
Biasuzzi, B
Biland, A
Blanch, O
Bonnefoy, S
Bonnoli, G
Borracci, F
Bretz, T
Carosi, A
Chatterjee, A
Colin, P
Colombo, E
Da Vela, P
Dazzi, F
De Angelis, A
Wilhelmi, E. de Oña
Pierro, F. Di
Doert, M
Domínguez, A
Dorner, D
Doro, M
Einecke, S
Glawion, D. Eisenacher
Elsaesser, D
Engelkemeier, M
Ramazani, V. Fallah
Fernández-Barral, A
Fonseca, M. V
Font, L
Fruck, C
Galindo, D
Gaug, M
Giammaria, P
Godinović, N
Gora, D
Griffiths, S
Hadasch, D
Hassan, T
Hughes, G
Ishio, K
Konno, Y
Kushida, J
Kuveždić, D
Lindfors, E
Majumdar, P
Makariev, M
Maneva, G
Manganaro, M
Maraschi, L
Mariotti, M
Mazin, D
Menzel, U
Mirzoyan, R
Moralejo, A
Moreno, V
Moretti, E
Neustroev, V
Niedzwiecki, A
Rosillo, M. Nievas
Nilsson, K
Noda, K
Nogués, L
Paiano, S
Palacio, J
Paneque, D
Paoletti, R
Paredes-Fortuny, X
Pedaletti, G
Perri, L
Persic, M
Poutanen, J
Moroni, P. G. Prada
Prandini, E
Garcia, J. R
Reichardt, I
Rhode, W
Ribó, M
Rico, J
Saito, T
Schroeder, S
Šnidarić, I
Sobczynska, D
Takalo, L
Tavecchio, F
Temnikov, P
Terzić, T
Teshima, M
Torres-Albà, N
Vanzo, G
Ward, J. E
Wu, M. H
Zarić, D
Collaboration), (MAGIC
Cognard, I
Guillemot, L
description Abstract B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to TeV energies and subsequent production of very high-energy γ-rays in the inverse Compton process. We performed extensive observations with the Major Atmospheric Gamma Imaging Cherenkov Telescopes (MAGIC) telescopes of B1957+20. We interpret results in the framework of a few different models, namely emission from the vicinity of the millisecond pulsar, the interaction of the pulsar and stellar companion wind region or bow shock nebula. No significant steady very high-energy γ-ray emission was found. We derived a 95 per cent confidence level upper limit of 3.0 × 10−12 cm−2 s−1 on the average γ-ray emission from the binary system above 200 GeV. The upper limits obtained with the MAGIC constrain, for the first time, different models of the high-energy emission in B1957+20. In particular, in the inner mixed wind nebula model with mono-energetic injection of electrons, the acceleration efficiency of electrons is constrained to be below ∼2–10 per cent of the pulsar spin-down power. For the pulsar emission, the obtained upper limits for each emission peak are well above the exponential cut-off fits to the Fermi-LAT data, extrapolated to energies above 50 GeV. The MAGIC upper limits can rule out a simple power-law tail extension through the sub-TeV energy range for the main peak seen at radio frequencies.
doi_str_mv 10.1093/mnras/stx1405
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Fallah ; Fernández-Barral, A ; Fonseca, M. V ; Font, L ; Fruck, C ; Galindo, D ; Gaug, M ; Giammaria, P ; Godinović, N ; Gora, D ; Griffiths, S ; Hadasch, D ; Hassan, T ; Hughes, G ; Ishio, K ; Konno, Y ; Kushida, J ; Kuveždić, D ; Lindfors, E ; Majumdar, P ; Makariev, M ; Maneva, G ; Manganaro, M ; Maraschi, L ; Mariotti, M ; Mazin, D ; Menzel, U ; Mirzoyan, R ; Moralejo, A ; Moreno, V ; Moretti, E ; Neustroev, V ; Niedzwiecki, A ; Rosillo, M. Nievas ; Nilsson, K ; Noda, K ; Nogués, L ; Paiano, S ; Palacio, J ; Paneque, D ; Paoletti, R ; Paredes-Fortuny, X ; Pedaletti, G ; Perri, L ; Persic, M ; Poutanen, J ; Moroni, P. G. Prada ; Prandini, E ; Garcia, J. R ; Reichardt, I ; Rhode, W ; Ribó, M ; Rico, J ; Saito, T ; Schroeder, S ; Šnidarić, I ; Sobczynska, D ; Takalo, L ; Tavecchio, F ; Temnikov, P ; Terzić, T ; Teshima, M ; Torres-Albà, N ; Vanzo, G ; Ward, J. E ; Wu, M. 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We derived a 95 per cent confidence level upper limit of 3.0 × 10−12 cm−2 s−1 on the average γ-ray emission from the binary system above 200 GeV. The upper limits obtained with the MAGIC constrain, for the first time, different models of the high-energy emission in B1957+20. In particular, in the inner mixed wind nebula model with mono-energetic injection of electrons, the acceleration efficiency of electrons is constrained to be below ∼2–10 per cent of the pulsar spin-down power. For the pulsar emission, the obtained upper limits for each emission peak are well above the exponential cut-off fits to the Fermi-LAT data, extrapolated to energies above 50 GeV. 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H</creatorcontrib><creatorcontrib>Zarić, D</creatorcontrib><creatorcontrib>Collaboration), (MAGIC</creatorcontrib><creatorcontrib>Cognard, I</creatorcontrib><creatorcontrib>Guillemot, L</creatorcontrib><title>Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes</title><title>Monthly Notices of the Royal Astronomical Society</title><description>Abstract B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to TeV energies and subsequent production of very high-energy γ-rays in the inverse Compton process. We performed extensive observations with the Major Atmospheric Gamma Imaging Cherenkov Telescopes (MAGIC) telescopes of B1957+20. We interpret results in the framework of a few different models, namely emission from the vicinity of the millisecond pulsar, the interaction of the pulsar and stellar companion wind region or bow shock nebula. No significant steady very high-energy γ-ray emission was found. We derived a 95 per cent confidence level upper limit of 3.0 × 10−12 cm−2 s−1 on the average γ-ray emission from the binary system above 200 GeV. The upper limits obtained with the MAGIC constrain, for the first time, different models of the high-energy emission in B1957+20. In particular, in the inner mixed wind nebula model with mono-energetic injection of electrons, the acceleration efficiency of electrons is constrained to be below ∼2–10 per cent of the pulsar spin-down power. For the pulsar emission, the obtained upper limits for each emission peak are well above the exponential cut-off fits to the Fermi-LAT data, extrapolated to energies above 50 GeV. The MAGIC upper limits can rule out a simple power-law tail extension through the sub-TeV energy range for the main peak seen at radio frequencies.</description><subject>Astrophysics</subject><subject>Sciences of the Universe</subject><subject>Solar and Stellar Astrophysics</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNqF0M9LwzAUB_AgCs7p0XuOotQlTZM2xznUCZNd9Bxe0pRF06Y03eb-e7sfePX04PF5jy9fhG4peaREsknddBAnsf-hGeFnaESZ4EkqhThHI0IYT4qc0kt0FeMXISRjqRghvdTRdhvoXWhwqHC_slh7MN9468qwxU9U8vwhJbh23rtoTWhK3K59hA5r10C3w3EXe1sPvl8dzt-nr28z3FtvowmtjdfoogIf7c1pjtHny_PHbJ4slgOcLhLDsqxPhNCE5wCa23SIx6WQJUtlWpIhNZhyWEowacEBoDAZUKormRVFqatKlpKyMbo__l2BV23n6iGcCuDUfLpQrolrRahggmT5Zo-TIzZdiLGz1d8FJWrfpjq0qU5tDv7u6MO6_Yf-Agi0dxM</recordid><startdate>20171001</startdate><enddate>20171001</enddate><creator>Ansoldi, S</creator><creator>Antonelli, L. 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H</creator><creator>Zarić, D</creator><creator>Collaboration), (MAGIC</creator><creator>Cognard, I</creator><creator>Guillemot, L</creator><general>Oxford University Press</general><general>Oxford University Press (OUP): Policy P - Oxford Open Option A</general><scope>AAYXX</scope><scope>CITATION</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0002-2830-0502</orcidid><orcidid>https://orcid.org/0000-0001-8442-7877</orcidid><orcidid>https://orcid.org/0000-0002-0965-0259</orcidid><orcidid>https://orcid.org/0000-0003-1397-6478</orcidid><orcidid>https://orcid.org/0000-0001-7387-3812</orcidid><orcidid>https://orcid.org/0000-0002-5959-4179</orcidid><orcidid>https://orcid.org/0000-0003-1539-3268</orcidid><orcidid>https://orcid.org/0000-0002-6336-865X</orcidid><orcidid>https://orcid.org/0000-0002-1775-9692</orcidid><orcidid>https://orcid.org/0000-0001-6796-3205</orcidid><orcidid>https://orcid.org/0000-0003-0163-7233</orcidid><orcidid>https://orcid.org/0000-0003-2636-5000</orcidid><orcidid>https://orcid.org/0000-0003-4137-1134</orcidid><orcidid>https://orcid.org/0000-0002-9430-5264</orcidid><orcidid>https://orcid.org/0000-0002-1622-3116</orcidid><orcidid>https://orcid.org/0000-0002-5481-5040</orcidid><orcidid>https://orcid.org/0000-0001-9159-9853</orcidid><orcidid>https://orcid.org/0000-0002-1445-8683</orcidid><orcidid>https://orcid.org/0000-0002-1566-9044</orcidid><orcidid>https://orcid.org/0000-0003-3444-3830</orcidid><orcidid>https://orcid.org/0000-0003-0605-108X</orcidid><orcidid>https://orcid.org/0000-0001-5880-7518</orcidid><orcidid>https://orcid.org/0000-0002-7669-266X</orcidid><orcidid>https://orcid.org/0000-0002-2950-6641</orcidid><orcidid>https://orcid.org/0000-0002-1830-4251</orcidid><orcidid>https://orcid.org/0000-0001-6201-3761</orcidid><orcidid>https://orcid.org/0000-0001-8823-479X</orcidid><orcidid>https://orcid.org/0000-0002-4758-9196</orcidid><orcidid>https://orcid.org/0000-0003-1853-4900</orcidid><orcidid>https://orcid.org/0000-0003-2501-2270</orcidid><orcidid>https://orcid.org/0000-0001-8663-6461</orcidid><orcidid>https://orcid.org/0000-0002-3771-4918</orcidid><orcidid>https://orcid.org/0000-0002-8269-5760</orcidid><orcidid>https://orcid.org/0000-0002-9931-4557</orcidid><orcidid>https://orcid.org/0000-0002-1288-833X</orcidid><orcidid>https://orcid.org/0000-0003-3108-1141</orcidid><orcidid>https://orcid.org/0000-0002-4137-4370</orcidid><orcidid>https://orcid.org/0000-0002-7504-2083</orcidid><orcidid>https://orcid.org/0000-0003-0256-0995</orcidid><orcidid>https://orcid.org/0000-0001-5409-6544</orcidid><orcidid>https://orcid.org/0000-0002-8380-1633</orcidid><orcidid>https://orcid.org/0000-0002-2239-3373</orcidid><orcidid>https://orcid.org/0000-0003-0158-2826</orcidid><orcidid>https://orcid.org/0000-0002-8002-8585</orcidid><orcidid>https://orcid.org/0000-0002-9155-6199</orcidid><orcidid>https://orcid.org/0000-0002-3700-3745</orcidid><orcidid>https://orcid.org/0000-0001-7909-588X</orcidid><orcidid>https://orcid.org/0000-0002-5613-7693</orcidid><orcidid>https://orcid.org/0000-0002-1344-9080</orcidid><orcidid>https://orcid.org/0000-0002-9559-3384</orcidid><orcidid>https://orcid.org/0000-0003-2109-5961</orcidid><orcidid>https://orcid.org/0000-0002-0445-4566</orcidid><orcidid>https://orcid.org/0000-0003-4576-0452</orcidid><orcidid>https://orcid.org/0000-0003-3624-4480</orcidid><orcidid>https://orcid.org/0000-0002-7027-5021</orcidid><orcidid>https://orcid.org/0000-0003-0396-4190</orcidid><orcidid>https://orcid.org/0000-0002-2010-4005</orcidid><orcidid>https://orcid.org/0000-0001-9687-8237</orcidid><orcidid>https://orcid.org/0000-0002-1998-9707</orcidid><orcidid>https://orcid.org/0000-0001-9104-3214</orcidid><orcidid>https://orcid.org/0000-0002-8358-2098</orcidid><orcidid>https://orcid.org/0000-0003-4502-9053</orcidid><orcidid>https://orcid.org/0000-0001-9078-5507</orcidid><orcidid>https://orcid.org/0000-0003-0827-5642</orcidid><orcidid>https://orcid.org/0000-0003-1530-3031</orcidid><orcidid>https://orcid.org/0000-0003-4772-595X</orcidid><orcidid>https://orcid.org/0000-0003-2464-9077</orcidid><orcidid>https://orcid.org/0000-0003-3297-4128</orcidid><orcidid>https://orcid.org/0000-0001-5049-1045</orcidid></search><sort><creationdate>20171001</creationdate><title>Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes</title><author>Ansoldi, S ; Antonelli, L. A ; Banerjee, B ; de Almeida, U. Barres ; González, J. Becerra ; Berti, A ; Biasuzzi, B ; Biland, A ; Blanch, O ; Bonnefoy, S ; Bonnoli, G ; Borracci, F ; Bretz, T ; Carosi, A ; Chatterjee, A ; Colin, P ; Colombo, E ; Da Vela, P ; Dazzi, F ; De Angelis, A ; Wilhelmi, E. de Oña ; Pierro, F. Di ; Doert, M ; Domínguez, A ; Dorner, D ; Doro, M ; Einecke, S ; Glawion, D. Eisenacher ; Elsaesser, D ; Engelkemeier, M ; Ramazani, V. Fallah ; Fernández-Barral, A ; Fonseca, M. V ; Font, L ; Fruck, C ; Galindo, D ; Gaug, M ; Giammaria, P ; Godinović, N ; Gora, D ; Griffiths, S ; Hadasch, D ; Hassan, T ; Hughes, G ; Ishio, K ; Konno, Y ; Kushida, J ; Kuveždić, D ; Lindfors, E ; Majumdar, P ; Makariev, M ; Maneva, G ; Manganaro, M ; Maraschi, L ; Mariotti, M ; Mazin, D ; Menzel, U ; Mirzoyan, R ; Moralejo, A ; Moreno, V ; Moretti, E ; Neustroev, V ; Niedzwiecki, A ; Rosillo, M. Nievas ; Nilsson, K ; Noda, K ; Nogués, L ; Paiano, S ; Palacio, J ; Paneque, D ; Paoletti, R ; Paredes-Fortuny, X ; Pedaletti, G ; Perri, L ; Persic, M ; Poutanen, J ; Moroni, P. G. Prada ; Prandini, E ; Garcia, J. R ; Reichardt, I ; Rhode, W ; Ribó, M ; Rico, J ; Saito, T ; Schroeder, S ; Šnidarić, I ; Sobczynska, D ; Takalo, L ; Tavecchio, F ; Temnikov, P ; Terzić, T ; Teshima, M ; Torres-Albà, N ; Vanzo, G ; Ward, J. E ; Wu, M. H ; Zarić, D ; Collaboration), (MAGIC ; Cognard, I ; Guillemot, L</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c344t-66b057aab5e20005969d3292d0711acd2009ac285aaa8c4a11bf9488dbff9d913</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Astrophysics</topic><topic>Sciences of the Universe</topic><topic>Solar and Stellar Astrophysics</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Ansoldi, S</creatorcontrib><creatorcontrib>Antonelli, L. A</creatorcontrib><creatorcontrib>Banerjee, B</creatorcontrib><creatorcontrib>de Almeida, U. Barres</creatorcontrib><creatorcontrib>González, J. 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Di</creatorcontrib><creatorcontrib>Doert, M</creatorcontrib><creatorcontrib>Domínguez, A</creatorcontrib><creatorcontrib>Dorner, D</creatorcontrib><creatorcontrib>Doro, M</creatorcontrib><creatorcontrib>Einecke, S</creatorcontrib><creatorcontrib>Glawion, D. Eisenacher</creatorcontrib><creatorcontrib>Elsaesser, D</creatorcontrib><creatorcontrib>Engelkemeier, M</creatorcontrib><creatorcontrib>Ramazani, V. Fallah</creatorcontrib><creatorcontrib>Fernández-Barral, A</creatorcontrib><creatorcontrib>Fonseca, M. 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Nievas</creatorcontrib><creatorcontrib>Nilsson, K</creatorcontrib><creatorcontrib>Noda, K</creatorcontrib><creatorcontrib>Nogués, L</creatorcontrib><creatorcontrib>Paiano, S</creatorcontrib><creatorcontrib>Palacio, J</creatorcontrib><creatorcontrib>Paneque, D</creatorcontrib><creatorcontrib>Paoletti, R</creatorcontrib><creatorcontrib>Paredes-Fortuny, X</creatorcontrib><creatorcontrib>Pedaletti, G</creatorcontrib><creatorcontrib>Perri, L</creatorcontrib><creatorcontrib>Persic, M</creatorcontrib><creatorcontrib>Poutanen, J</creatorcontrib><creatorcontrib>Moroni, P. G. Prada</creatorcontrib><creatorcontrib>Prandini, E</creatorcontrib><creatorcontrib>Garcia, J. R</creatorcontrib><creatorcontrib>Reichardt, I</creatorcontrib><creatorcontrib>Rhode, W</creatorcontrib><creatorcontrib>Ribó, M</creatorcontrib><creatorcontrib>Rico, J</creatorcontrib><creatorcontrib>Saito, T</creatorcontrib><creatorcontrib>Schroeder, S</creatorcontrib><creatorcontrib>Šnidarić, I</creatorcontrib><creatorcontrib>Sobczynska, D</creatorcontrib><creatorcontrib>Takalo, L</creatorcontrib><creatorcontrib>Tavecchio, F</creatorcontrib><creatorcontrib>Temnikov, P</creatorcontrib><creatorcontrib>Terzić, T</creatorcontrib><creatorcontrib>Teshima, M</creatorcontrib><creatorcontrib>Torres-Albà, N</creatorcontrib><creatorcontrib>Vanzo, G</creatorcontrib><creatorcontrib>Ward, J. E</creatorcontrib><creatorcontrib>Wu, M. H</creatorcontrib><creatorcontrib>Zarić, D</creatorcontrib><creatorcontrib>Collaboration), (MAGIC</creatorcontrib><creatorcontrib>Cognard, I</creatorcontrib><creatorcontrib>Guillemot, L</creatorcontrib><collection>CrossRef</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Monthly Notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Ansoldi, S</au><au>Antonelli, L. A</au><au>Banerjee, B</au><au>de Almeida, U. Barres</au><au>González, J. Becerra</au><au>Berti, A</au><au>Biasuzzi, B</au><au>Biland, A</au><au>Blanch, O</au><au>Bonnefoy, S</au><au>Bonnoli, G</au><au>Borracci, F</au><au>Bretz, T</au><au>Carosi, A</au><au>Chatterjee, A</au><au>Colin, P</au><au>Colombo, E</au><au>Da Vela, P</au><au>Dazzi, F</au><au>De Angelis, A</au><au>Wilhelmi, E. de Oña</au><au>Pierro, F. Di</au><au>Doert, M</au><au>Domínguez, A</au><au>Dorner, D</au><au>Doro, M</au><au>Einecke, S</au><au>Glawion, D. Eisenacher</au><au>Elsaesser, D</au><au>Engelkemeier, M</au><au>Ramazani, V. Fallah</au><au>Fernández-Barral, A</au><au>Fonseca, M. V</au><au>Font, L</au><au>Fruck, C</au><au>Galindo, D</au><au>Gaug, M</au><au>Giammaria, P</au><au>Godinović, N</au><au>Gora, D</au><au>Griffiths, S</au><au>Hadasch, D</au><au>Hassan, T</au><au>Hughes, G</au><au>Ishio, K</au><au>Konno, Y</au><au>Kushida, J</au><au>Kuveždić, D</au><au>Lindfors, E</au><au>Majumdar, P</au><au>Makariev, M</au><au>Maneva, G</au><au>Manganaro, M</au><au>Maraschi, L</au><au>Mariotti, M</au><au>Mazin, D</au><au>Menzel, U</au><au>Mirzoyan, R</au><au>Moralejo, A</au><au>Moreno, V</au><au>Moretti, E</au><au>Neustroev, V</au><au>Niedzwiecki, A</au><au>Rosillo, M. Nievas</au><au>Nilsson, K</au><au>Noda, K</au><au>Nogués, L</au><au>Paiano, S</au><au>Palacio, J</au><au>Paneque, D</au><au>Paoletti, R</au><au>Paredes-Fortuny, X</au><au>Pedaletti, G</au><au>Perri, L</au><au>Persic, M</au><au>Poutanen, J</au><au>Moroni, P. G. Prada</au><au>Prandini, E</au><au>Garcia, J. R</au><au>Reichardt, I</au><au>Rhode, W</au><au>Ribó, M</au><au>Rico, J</au><au>Saito, T</au><au>Schroeder, S</au><au>Šnidarić, I</au><au>Sobczynska, D</au><au>Takalo, L</au><au>Tavecchio, F</au><au>Temnikov, P</au><au>Terzić, T</au><au>Teshima, M</au><au>Torres-Albà, N</au><au>Vanzo, G</au><au>Ward, J. E</au><au>Wu, M. H</au><au>Zarić, D</au><au>Collaboration), (MAGIC</au><au>Cognard, I</au><au>Guillemot, L</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes</atitle><jtitle>Monthly Notices of the Royal Astronomical Society</jtitle><date>2017-10-01</date><risdate>2017</risdate><volume>470</volume><issue>4</issue><spage>4608</spage><epage>4617</epage><pages>4608-4617</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>Abstract B1957+20 is a millisecond pulsar located in a black-widow-type compact binary system with a low-mass stellar companion. The interaction of the pulsar wind with the companion star wind and/or the interstellar plasma is expected to create plausible conditions for acceleration of electrons to TeV energies and subsequent production of very high-energy γ-rays in the inverse Compton process. We performed extensive observations with the Major Atmospheric Gamma Imaging Cherenkov Telescopes (MAGIC) telescopes of B1957+20. We interpret results in the framework of a few different models, namely emission from the vicinity of the millisecond pulsar, the interaction of the pulsar and stellar companion wind region or bow shock nebula. No significant steady very high-energy γ-ray emission was found. We derived a 95 per cent confidence level upper limit of 3.0 × 10−12 cm−2 s−1 on the average γ-ray emission from the binary system above 200 GeV. The upper limits obtained with the MAGIC constrain, for the first time, different models of the high-energy emission in B1957+20. In particular, in the inner mixed wind nebula model with mono-energetic injection of electrons, the acceleration efficiency of electrons is constrained to be below ∼2–10 per cent of the pulsar spin-down power. For the pulsar emission, the obtained upper limits for each emission peak are well above the exponential cut-off fits to the Fermi-LAT data, extrapolated to energies above 50 GeV. The MAGIC upper limits can rule out a simple power-law tail extension through the sub-TeV energy range for the main peak seen at radio frequencies.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stx1405</doi><tpages>10</tpages><orcidid>https://orcid.org/0000-0002-2830-0502</orcidid><orcidid>https://orcid.org/0000-0001-8442-7877</orcidid><orcidid>https://orcid.org/0000-0002-0965-0259</orcidid><orcidid>https://orcid.org/0000-0003-1397-6478</orcidid><orcidid>https://orcid.org/0000-0001-7387-3812</orcidid><orcidid>https://orcid.org/0000-0002-5959-4179</orcidid><orcidid>https://orcid.org/0000-0003-1539-3268</orcidid><orcidid>https://orcid.org/0000-0002-6336-865X</orcidid><orcidid>https://orcid.org/0000-0002-1775-9692</orcidid><orcidid>https://orcid.org/0000-0001-6796-3205</orcidid><orcidid>https://orcid.org/0000-0003-0163-7233</orcidid><orcidid>https://orcid.org/0000-0003-2636-5000</orcidid><orcidid>https://orcid.org/0000-0003-4137-1134</orcidid><orcidid>https://orcid.org/0000-0002-9430-5264</orcidid><orcidid>https://orcid.org/0000-0002-1622-3116</orcidid><orcidid>https://orcid.org/0000-0002-5481-5040</orcidid><orcidid>https://orcid.org/0000-0001-9159-9853</orcidid><orcidid>https://orcid.org/0000-0002-1445-8683</orcidid><orcidid>https://orcid.org/0000-0002-1566-9044</orcidid><orcidid>https://orcid.org/0000-0003-3444-3830</orcidid><orcidid>https://orcid.org/0000-0003-0605-108X</orcidid><orcidid>https://orcid.org/0000-0001-5880-7518</orcidid><orcidid>https://orcid.org/0000-0002-7669-266X</orcidid><orcidid>https://orcid.org/0000-0002-2950-6641</orcidid><orcidid>https://orcid.org/0000-0002-1830-4251</orcidid><orcidid>https://orcid.org/0000-0001-6201-3761</orcidid><orcidid>https://orcid.org/0000-0001-8823-479X</orcidid><orcidid>https://orcid.org/0000-0002-4758-9196</orcidid><orcidid>https://orcid.org/0000-0003-1853-4900</orcidid><orcidid>https://orcid.org/0000-0003-2501-2270</orcidid><orcidid>https://orcid.org/0000-0001-8663-6461</orcidid><orcidid>https://orcid.org/0000-0002-3771-4918</orcidid><orcidid>https://orcid.org/0000-0002-8269-5760</orcidid><orcidid>https://orcid.org/0000-0002-9931-4557</orcidid><orcidid>https://orcid.org/0000-0002-1288-833X</orcidid><orcidid>https://orcid.org/0000-0003-3108-1141</orcidid><orcidid>https://orcid.org/0000-0002-4137-4370</orcidid><orcidid>https://orcid.org/0000-0002-7504-2083</orcidid><orcidid>https://orcid.org/0000-0003-0256-0995</orcidid><orcidid>https://orcid.org/0000-0001-5409-6544</orcidid><orcidid>https://orcid.org/0000-0002-8380-1633</orcidid><orcidid>https://orcid.org/0000-0002-2239-3373</orcidid><orcidid>https://orcid.org/0000-0003-0158-2826</orcidid><orcidid>https://orcid.org/0000-0002-8002-8585</orcidid><orcidid>https://orcid.org/0000-0002-9155-6199</orcidid><orcidid>https://orcid.org/0000-0002-3700-3745</orcidid><orcidid>https://orcid.org/0000-0001-7909-588X</orcidid><orcidid>https://orcid.org/0000-0002-5613-7693</orcidid><orcidid>https://orcid.org/0000-0002-1344-9080</orcidid><orcidid>https://orcid.org/0000-0002-9559-3384</orcidid><orcidid>https://orcid.org/0000-0003-2109-5961</orcidid><orcidid>https://orcid.org/0000-0002-0445-4566</orcidid><orcidid>https://orcid.org/0000-0003-4576-0452</orcidid><orcidid>https://orcid.org/0000-0003-3624-4480</orcidid><orcidid>https://orcid.org/0000-0002-7027-5021</orcidid><orcidid>https://orcid.org/0000-0003-0396-4190</orcidid><orcidid>https://orcid.org/0000-0002-2010-4005</orcidid><orcidid>https://orcid.org/0000-0001-9687-8237</orcidid><orcidid>https://orcid.org/0000-0002-1998-9707</orcidid><orcidid>https://orcid.org/0000-0001-9104-3214</orcidid><orcidid>https://orcid.org/0000-0002-8358-2098</orcidid><orcidid>https://orcid.org/0000-0003-4502-9053</orcidid><orcidid>https://orcid.org/0000-0001-9078-5507</orcidid><orcidid>https://orcid.org/0000-0003-0827-5642</orcidid><orcidid>https://orcid.org/0000-0003-1530-3031</orcidid><orcidid>https://orcid.org/0000-0003-4772-595X</orcidid><orcidid>https://orcid.org/0000-0003-2464-9077</orcidid><orcidid>https://orcid.org/0000-0003-3297-4128</orcidid><orcidid>https://orcid.org/0000-0001-5049-1045</orcidid><oa>free_for_read</oa></addata></record>
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identifier ISSN: 0035-8711
ispartof Monthly Notices of the Royal Astronomical Society, 2017-10, Vol.470 (4), p.4608-4617
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1365-2966
language eng
recordid cdi_hal_primary_oai_HAL_insu_01636047v1
source Oxford Journals Open Access Collection
subjects Astrophysics
Sciences of the Universe
Solar and Stellar Astrophysics
title Observation of the black widow B1957+20 millisecond pulsar binary system with the MAGIC telescopes
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