Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC
The pulsar wind nebula (PWN) 3C 58 is one of the historical very high-energy (VHE; E> 100 GeV) γ-ray source candidates. It is energized by one of the highest spin-down power pulsars known (5% of Crab pulsar) and it has been compared with the Crab nebula because of their morphological similarities...
| Autores: | , , , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión aceptada para publicación |
| Fecha de publicación: | 2014 |
| País: | España |
| Institución: | Universidad de Barcelona |
| Repositorio: | Dipòsit Digital de la UB |
| OAI Identifier: | oai:diposit.ub.edu:2445/58586 |
| Acceso en línea: | https://hdl.handle.net/2445/58586 |
| Access Level: | acceso abierto |
| Palabra clave: | Raigs gamma Púlsars Astrofísica Gamma rays Pulsars Astrophysics |
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Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGICGalindo Fernández, DanielMarcote Martin, BenitoMunar i Adrover, PereParedes i Poy, Josep MariaParedes Fortuny, XavierRibó Gomis, MarcZanin, RobertaMAGIC CollaborationRaigs gammaPúlsarsAstrofísicaGamma raysPulsarsAstrophysicsThe pulsar wind nebula (PWN) 3C 58 is one of the historical very high-energy (VHE; E> 100 GeV) γ-ray source candidates. It is energized by one of the highest spin-down power pulsars known (5% of Crab pulsar) and it has been compared with the Crab nebula because of their morphological similarities. This object was previously observed by imaging atmospheric Cherenkov telescopes (Whipple, VERITAS and MAGIC), although it was not detected, with an upper limit of 2.3% Crab unit (C.U.) at VHE. It was detected by the Fermi Large Area Telescope (LAT) with a spectrum extending beyond 100 GeV. Aims: We aim to extend the spectrum of 3C 58 beyond the energies reported by the Fermi Collaboration and probe acceleration of particles in the PWN up to energies of a few tens of TeV. Methods: We analyzed 81 h of 3C 58 data taken in the period between August 2013 and January 2014 with the MAGIC telescopes. Results: We detected VHE γ-ray emission from 3C 58 with a significance of 5.7σ and an integral flux of 0.65% C.U. above 1 TeV. According to our results, 3C 58 is the least luminous VHE γ-ray PWN ever detected at VHE and has the lowest flux at VHE to date. The differential energy spectrum between 400 GeV and 10 TeV is well described by a power-law function dφ/dE = f0(E/1 TeV)-Γ with f0 = (2.0 ± 0.4stat ± 0.6sys) × 10-13 cm-2 s-1 TeV-1 and Γ = 2.4 ± 0.2stat ± 0.2sys. The skymap is compatible with an unresolved source. Conclusions: We report the first significant detection of PWN 3C 58 at TeV energies. We compare our results with the expectations of time-dependent models in which electrons upscatter photon fields. The best representation favors a distance to the PWN of 2 kpc and far-infrared (FIR) values similar to cosmic microwave background photon fields. If we consider an unexpectedly high FIR density, the data can also be reproduced by models assuming a 3.2 kpc distance. A low magnetic field, far from equipartition, is required to explain the VHE data. Hadronic contribution from the hosting supernova remnant (SNR) requires an unrealistic energy budget given the density of the medium, disfavoring cosmic-ray acceleration in the SNR as origin of the VHE γ-ray emission.Springer Verlag2014info:eu-repo/semantics/articleinfo:eu-repo/semantics/acceptedVersionapplication/pdfhttps://hdl.handle.net/2445/58586Articles publicats en revistes (Física Quàntica i Astrofísica)reponame:Dipòsit Digital de la UBinstname:Universidad de BarcelonaInglésVersió postprint del document publicat a: http://dx.doi.org/10.1051/0004-6361/201424261Astronomy and Astrophysics, 2014, vol. 567, num. L8, p. 1-5http://dx.doi.org/10.1051/0004-6361/201424261(c) Springer Verlag, 2014info:eu-repo/semantics/openAccessoai:diposit.ub.edu:2445/585862026-05-27T06:46:51Z |
| dc.title.none.fl_str_mv |
Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC |
| title |
Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC |
| spellingShingle |
Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC Galindo Fernández, Daniel Raigs gamma Púlsars Astrofísica Gamma rays Pulsars Astrophysics |
| title_short |
Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC |
| title_full |
Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC |
| title_fullStr |
Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC |
| title_full_unstemmed |
Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC |
| title_sort |
Discovery of TeV γ-ray emission from the pulsar wind nebula 3C 58 by MAGIC |
| dc.creator.none.fl_str_mv |
Galindo Fernández, Daniel Marcote Martin, Benito Munar i Adrover, Pere Paredes i Poy, Josep Maria Paredes Fortuny, Xavier Ribó Gomis, Marc Zanin, Roberta MAGIC Collaboration |
| author |
Galindo Fernández, Daniel |
| author_facet |
Galindo Fernández, Daniel Marcote Martin, Benito Munar i Adrover, Pere Paredes i Poy, Josep Maria Paredes Fortuny, Xavier Ribó Gomis, Marc Zanin, Roberta MAGIC Collaboration |
| author_role |
author |
| author2 |
Marcote Martin, Benito Munar i Adrover, Pere Paredes i Poy, Josep Maria Paredes Fortuny, Xavier Ribó Gomis, Marc Zanin, Roberta MAGIC Collaboration |
| author2_role |
author author author author author author author |
| dc.subject.none.fl_str_mv |
Raigs gamma Púlsars Astrofísica Gamma rays Pulsars Astrophysics |
| topic |
Raigs gamma Púlsars Astrofísica Gamma rays Pulsars Astrophysics |
| description |
The pulsar wind nebula (PWN) 3C 58 is one of the historical very high-energy (VHE; E> 100 GeV) γ-ray source candidates. It is energized by one of the highest spin-down power pulsars known (5% of Crab pulsar) and it has been compared with the Crab nebula because of their morphological similarities. This object was previously observed by imaging atmospheric Cherenkov telescopes (Whipple, VERITAS and MAGIC), although it was not detected, with an upper limit of 2.3% Crab unit (C.U.) at VHE. It was detected by the Fermi Large Area Telescope (LAT) with a spectrum extending beyond 100 GeV. Aims: We aim to extend the spectrum of 3C 58 beyond the energies reported by the Fermi Collaboration and probe acceleration of particles in the PWN up to energies of a few tens of TeV. Methods: We analyzed 81 h of 3C 58 data taken in the period between August 2013 and January 2014 with the MAGIC telescopes. Results: We detected VHE γ-ray emission from 3C 58 with a significance of 5.7σ and an integral flux of 0.65% C.U. above 1 TeV. According to our results, 3C 58 is the least luminous VHE γ-ray PWN ever detected at VHE and has the lowest flux at VHE to date. The differential energy spectrum between 400 GeV and 10 TeV is well described by a power-law function dφ/dE = f0(E/1 TeV)-Γ with f0 = (2.0 ± 0.4stat ± 0.6sys) × 10-13 cm-2 s-1 TeV-1 and Γ = 2.4 ± 0.2stat ± 0.2sys. The skymap is compatible with an unresolved source. Conclusions: We report the first significant detection of PWN 3C 58 at TeV energies. We compare our results with the expectations of time-dependent models in which electrons upscatter photon fields. The best representation favors a distance to the PWN of 2 kpc and far-infrared (FIR) values similar to cosmic microwave background photon fields. If we consider an unexpectedly high FIR density, the data can also be reproduced by models assuming a 3.2 kpc distance. A low magnetic field, far from equipartition, is required to explain the VHE data. Hadronic contribution from the hosting supernova remnant (SNR) requires an unrealistic energy budget given the density of the medium, disfavoring cosmic-ray acceleration in the SNR as origin of the VHE γ-ray emission. |
| publishDate |
2014 |
| dc.date.none.fl_str_mv |
2014 |
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info:eu-repo/semantics/article info:eu-repo/semantics/acceptedVersion |
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article |
| status_str |
acceptedVersion |
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https://hdl.handle.net/2445/58586 |
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https://hdl.handle.net/2445/58586 |
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Inglés |
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Inglés |
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Versió postprint del document publicat a: http://dx.doi.org/10.1051/0004-6361/201424261 Astronomy and Astrophysics, 2014, vol. 567, num. L8, p. 1-5 http://dx.doi.org/10.1051/0004-6361/201424261 |
| dc.rights.none.fl_str_mv |
(c) Springer Verlag, 2014 info:eu-repo/semantics/openAccess |
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(c) Springer Verlag, 2014 |
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openAccess |
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application/pdf |
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Springer Verlag |
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Springer Verlag |
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Articles publicats en revistes (Física Quàntica i Astrofísica) reponame:Dipòsit Digital de la UB instname:Universidad de Barcelona |
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Universidad de Barcelona |
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Dipòsit Digital de la UB |
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