Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton

CTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts a peculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observed in radio and lies towards the edge of the radio nebula. The putative pulsar, CXOU J201609.2+371110, was first resolved with Chandra and is surrounded...

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Autores: Guest, Benson T., Safi-Harb, Samar, MacMaster, A., Kothes, Roland, Olmi, Barbara, Amato, E., Bucciantini, Niccolò, Arzoumanian, Zaven
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2020
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/236780
Acceso en línea:http://hdl.handle.net/10261/236780
Access Level:acceso abierto
Palabra clave:ISM: individual (CTB 87 CXOU J201609.2+371110)
ISM: supernova remnants
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spelling Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-NewtonGuest, Benson T.Safi-Harb, SamarMacMaster, A.Kothes, RolandOlmi, BarbaraAmato, E.Bucciantini, NiccolòArzoumanian, ZavenISM: individual (CTB 87 CXOU J201609.2+371110)ISM: supernova remnantsCTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts a peculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observed in radio and lies towards the edge of the radio nebula. The putative pulsar, CXOU J201609.2+371110, was first resolved with Chandra and is surrounded by a compact and a more extended X-ray nebula. Here, we use a deep XMM-Newton observation to examine the morphology and evolutionary stage of the PWN and to search for thermal emission expected from a supernova shell or reverse shock interaction with supernova ejecta. We do not find evidence of thermal X-ray emission from the SNR and place an upper limit on the electron density of 0.05 cm for a plasma temperature kT ∼ 0.8 keV. The morphology and spectral properties are consistent with a ∼20-kyr-old relic PWN expanding into a stellar wind-blown bubble. We also present the first X-ray spectral index map from the PWN and show that we can reproduce its morphology by means of 2D axisymmetric relativistic hydrodynamical simulations.This research was supported by the Natural Sciences and Engineering Research Council of Canada (NSERC) through the Discovery Grants and the Canada Research Chairs Programs (SSH). BG acknowledges support from a University of Manitoba Graduate Scholarship. EA, NB, and BO wish to acknowledge financial support from the ‘Accordo attuativo ASI-INAF n. 2017-14-H.0, progetto: on the escape of cosmic rays and their impact on the background plasma’, the SKA-CTA-INAF and INAF-MAINSTREAM projects. We acknowledge an earlier contribution by H. Matheson towards the XMM proposal. We thank the referee for comments that helped improve the paper. This study used NASA’s Astrophysics Data System and ESA’s XMM–Newton facility.Blackwell PublishingRoyal Astronomical SocietyNational Research Council of CanadaCanada Research ChairsUniversity of ManitobaIstituto Nazionale di AstrofisicaNASAConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2021202120202021info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/236780reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Ingléshttp://doi.org/10.1093/mnras/stz3270Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/2367802026-05-22T06:33:51Z
dc.title.none.fl_str_mv Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton
title Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton
spellingShingle Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton
Guest, Benson T.
ISM: individual (CTB 87 CXOU J201609.2+371110)
ISM: supernova remnants
title_short Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton
title_full Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton
title_fullStr Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton
title_full_unstemmed Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton
title_sort Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton
dc.creator.none.fl_str_mv Guest, Benson T.
Safi-Harb, Samar
MacMaster, A.
Kothes, Roland
Olmi, Barbara
Amato, E.
Bucciantini, Niccolò
Arzoumanian, Zaven
author Guest, Benson T.
author_facet Guest, Benson T.
Safi-Harb, Samar
MacMaster, A.
Kothes, Roland
Olmi, Barbara
Amato, E.
Bucciantini, Niccolò
Arzoumanian, Zaven
author_role author
author2 Safi-Harb, Samar
MacMaster, A.
Kothes, Roland
Olmi, Barbara
Amato, E.
Bucciantini, Niccolò
Arzoumanian, Zaven
author2_role author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv National Research Council of Canada
Canada Research Chairs
University of Manitoba
Istituto Nazionale di Astrofisica
NASA
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv ISM: individual (CTB 87 CXOU J201609.2+371110)
ISM: supernova remnants
topic ISM: individual (CTB 87 CXOU J201609.2+371110)
ISM: supernova remnants
description CTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts a peculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observed in radio and lies towards the edge of the radio nebula. The putative pulsar, CXOU J201609.2+371110, was first resolved with Chandra and is surrounded by a compact and a more extended X-ray nebula. Here, we use a deep XMM-Newton observation to examine the morphology and evolutionary stage of the PWN and to search for thermal emission expected from a supernova shell or reverse shock interaction with supernova ejecta. We do not find evidence of thermal X-ray emission from the SNR and place an upper limit on the electron density of 0.05 cm for a plasma temperature kT ∼ 0.8 keV. The morphology and spectral properties are consistent with a ∼20-kyr-old relic PWN expanding into a stellar wind-blown bubble. We also present the first X-ray spectral index map from the PWN and show that we can reproduce its morphology by means of 2D axisymmetric relativistic hydrodynamical simulations.
publishDate 2020
dc.date.none.fl_str_mv 2020
2021
2021
2021
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/236780
url http://hdl.handle.net/10261/236780
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv http://doi.org/10.1093/mnras/stz3270
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv Blackwell Publishing
Royal Astronomical Society
publisher.none.fl_str_mv Blackwell Publishing
Royal Astronomical Society
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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score 15,81155

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