Hot Gas in the Wolf-Rayet Nebula NGC 3199

The Wolf-Rayet (WR) nebula NGC 3199 has been suggested to be a bow shock around its central star, WR 18, which is presumably a runaway star, because optical images of the nebula show a dominating arc of emission southwest of the star. We present the XMM-Newton detection of extended X-ray emission fr...

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Autores: Toalá, Jesús A., Marston, A. P., Guerrero, Martín A., Chu, Y. -H., Gruendl, R. A.
Formato: artículo
Estado:Versión aceptada para publicación
Fecha de publicación:2017
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/379696
Acesso em linha:http://hdl.handle.net/10261/379696
Access Level:acceso abierto
Palavra-chave:ISM: bubbles
Stars: Wolf–Rayet
X-rays: individual (NGC3199, WR18)
X-rays: ISM
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spelling Hot Gas in the Wolf-Rayet Nebula NGC 3199Toalá, Jesús A.Marston, A. P.Guerrero, Martín A.Chu, Y. -H.Gruendl, R. A.ISM: bubblesStars: Wolf–RayetX-rays: individual (NGC3199, WR18)X-rays: ISMThe Wolf-Rayet (WR) nebula NGC 3199 has been suggested to be a bow shock around its central star, WR 18, which is presumably a runaway star, because optical images of the nebula show a dominating arc of emission southwest of the star. We present the XMM-Newton detection of extended X-ray emission from NGC 3199, unveiling the powerful effect of the fast wind from WR 18. The X-ray emission is brighter in the region southeast of the star and an analysis of the spectral properties of the X-ray emission reveals abundance variations: (i) regions close to the optical arc present nitrogen-rich gas enhanced by the stellar wind from WR 18 and (ii) gas at the eastern region exhibits abundances close to those reported for the nebular abundances derived from optical studies, which is a signature of an efficient mixing of the nebular material with the stellar wind. The dominant plasma temperature and electron density are estimated to be T ≈ 1.2 ×10 K and n = 0.3 cm with an X-ray luminosity in the 0.3-3.0 keV energy range of L = 2.6 ×10 erg s. Combined with information derived from Herschel and the recent Gaia first data release, we conclude that WR 18 is not a runaway star and that the formation, chemical variations, and the shape of NGC 3199 depend on the initial configuration of the interstellar medium. © 2017. The American Astronomical SocietyWe would like to thank the anonymous referee for helpful suggestions that improved the presentation of our results. This work was based on observations obtained with XMM-Newton, Herschel, and Gaia satellites. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Herschel is an ESA space observatory with science instruments provided by Europeanled Principal Investigator consortia and with important participation from NASA. The Gaia data have been processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The authors thank Don Goldman (don@astrodon.com) for providing the narrowband [S II], Hα, and [O III] images of NGC 3199. We thank G. Ramos-Larios for helping process the optical images. M.A.G. acknowledges support from the grant AYA 2014-57280-P, cofunded with FEDER funds.American Astronomical SocietyEuropean CommissionConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2025202520172025info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/379696reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MINECO//AYA2014-57280-Phttp://dx.doi.org/10.3847/1538-4357/aa8554Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3796962026-05-22T06:33:51Z
dc.title.none.fl_str_mv Hot Gas in the Wolf-Rayet Nebula NGC 3199
title Hot Gas in the Wolf-Rayet Nebula NGC 3199
spellingShingle Hot Gas in the Wolf-Rayet Nebula NGC 3199
Toalá, Jesús A.
ISM: bubbles
Stars: Wolf–Rayet
X-rays: individual (NGC3199, WR18)
X-rays: ISM
title_short Hot Gas in the Wolf-Rayet Nebula NGC 3199
title_full Hot Gas in the Wolf-Rayet Nebula NGC 3199
title_fullStr Hot Gas in the Wolf-Rayet Nebula NGC 3199
title_full_unstemmed Hot Gas in the Wolf-Rayet Nebula NGC 3199
title_sort Hot Gas in the Wolf-Rayet Nebula NGC 3199
dc.creator.none.fl_str_mv Toalá, Jesús A.
Marston, A. P.
Guerrero, Martín A.
Chu, Y. -H.
Gruendl, R. A.
author Toalá, Jesús A.
author_facet Toalá, Jesús A.
Marston, A. P.
Guerrero, Martín A.
Chu, Y. -H.
Gruendl, R. A.
author_role author
author2 Marston, A. P.
Guerrero, Martín A.
Chu, Y. -H.
Gruendl, R. A.
author2_role author
author
author
author
dc.contributor.none.fl_str_mv European Commission
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv ISM: bubbles
Stars: Wolf–Rayet
X-rays: individual (NGC3199, WR18)
X-rays: ISM
topic ISM: bubbles
Stars: Wolf–Rayet
X-rays: individual (NGC3199, WR18)
X-rays: ISM
description The Wolf-Rayet (WR) nebula NGC 3199 has been suggested to be a bow shock around its central star, WR 18, which is presumably a runaway star, because optical images of the nebula show a dominating arc of emission southwest of the star. We present the XMM-Newton detection of extended X-ray emission from NGC 3199, unveiling the powerful effect of the fast wind from WR 18. The X-ray emission is brighter in the region southeast of the star and an analysis of the spectral properties of the X-ray emission reveals abundance variations: (i) regions close to the optical arc present nitrogen-rich gas enhanced by the stellar wind from WR 18 and (ii) gas at the eastern region exhibits abundances close to those reported for the nebular abundances derived from optical studies, which is a signature of an efficient mixing of the nebular material with the stellar wind. The dominant plasma temperature and electron density are estimated to be T ≈ 1.2 ×10 K and n = 0.3 cm with an X-ray luminosity in the 0.3-3.0 keV energy range of L = 2.6 ×10 erg s. Combined with information derived from Herschel and the recent Gaia first data release, we conclude that WR 18 is not a runaway star and that the formation, chemical variations, and the shape of NGC 3199 depend on the initial configuration of the interstellar medium. © 2017. The American Astronomical Society
publishDate 2017
dc.date.none.fl_str_mv 2017
2025
2025
2025
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Postprint
info:eu-repo/semantics/acceptedVersion
format article
status_str acceptedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/379696
url http://hdl.handle.net/10261/379696
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MINECO//AYA2014-57280-P
http://dx.doi.org/10.3847/1538-4357/aa8554
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv American Astronomical Society
publisher.none.fl_str_mv American 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 15,811543

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