Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance

Aims: This work aims to disentangle the morphological, kinematic, and chemical components of the nebula M1-67 to shed light on its process of formation around the central Wolf-Rayet (WR) star WR124. Methods: We have carried out integral field spectroscopy observations over two regions of M1-67, cove...

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Detalles Bibliográficos
Autores: Fernández-Martín, Alba, Vílchez Medina, José Manuel, Pérez-Montero, E., Candian, A., Sánchez, S. F., Martín-Gordón, D., Riera, A.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2013
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/408884
Acceso en línea:http://hdl.handle.net/10261/408884
Access Level:acceso abierto
Palabra clave:ISM: abundances
ISM: bubbles
ISM: individual objects: M1-67
ISM: kinematics and dynamics
Stars: Wolf-Rayet
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spelling Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearanceFernández-Martín, AlbaVílchez Medina, José ManuelPérez-Montero, E.Candian, A.Sánchez, S. F.Martín-Gordón, D.Riera, A.ISM: abundancesISM: bubblesISM: individual objects: M1-67ISM: kinematics and dynamicsStars: Wolf-RayetAims: This work aims to disentangle the morphological, kinematic, and chemical components of the nebula M1-67 to shed light on its process of formation around the central Wolf-Rayet (WR) star WR124. Methods: We have carried out integral field spectroscopy observations over two regions of M1-67, covering most of the nebula in the optical range. Maps of electron density, line ratios, and radial velocity were created to perform a detailed analysis of the two-dimensional structure. We studied the physical and chemical properties by means of integrated spectra selected over the whole nebula. Photoionization models were performed to confirm the empirical chemical results theoretically. In addition, we obtained and analysed infrared spectroscopic data and the MIPS 24 μm image of M1-67 from Spitzer. Results: We find that the ionized gas of M1-67 is condensed in knots aligned in a preferred axis along the NE-SW direction, like a bipolar structure. Both electron density and radial velocity decrease in this direction when moving away from the central star. From the derived electron temperature, Te ∼ 8200 K, we have estimated chemical abundances, obtaining that nitrogen appears strongly enriched and oxygen depleted. From the last two results, we infer that this bipolarity is the consequence of an ejection of an evolved stage of WR124 with material processed in the CNO cycle. Furthermore, we find two regions placed outside of the bipolar structure with different spectral and chemical properties. The infrared study has revealed that the bipolar axis is composed of ionized gas with a low ionization degree that is well mixed with warm dust and of a spherical bubble surrounding the ejection at 24 μm. Taking the evolution of a 60 M star and the temporal scale of the bipolar ejection into account, we propose that the observed gas was ejected during an eruption in the luminous blue variable stage. The star has entered the WR phase recently without apparent signs of interaction between WR-winds and interstellar material. © 2013 ESO.This work is supported by the Spanish Ministry of Science and Innovation (MICINN) under the grant BES-2008-008120. This work has been partially funded by the projects: AYA2010-21887-C04-01 of the Spanish PNAYA and CSD2006 - 00070 "1st Science with GTC from the CONSOLIDER 2010 programme of the Spanish MICINN and TIC114 of the Junta de Andalucía. We thank J. Toalá for providing estimations for the initial mass of the WR star and for useful suggestions. We are also very grateful to M. Fernández-Lorenzo, A. Monreal-Ibero, K. Weis, and the ESTALLIDOS collaboration for their useful comments and scientific support.Peer reviewedEDP SciencesMinisterio de Ciencia e Innovación (España)Ministerio de Educación y Ciencia (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252013info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/408884reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//BES-2008-008120info:eu-repo/grantAgreement/MICINN//AYA2010-21887-C04-01info:eu-repo/grantAgreement/MEC//CSD2006-00070http://dx.doi.org/10.1051/0004-6361/201220773Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/4088842026-05-22T06:33:51Z
dc.title.none.fl_str_mv Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance
title Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance
spellingShingle Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance
Fernández-Martín, Alba
ISM: abundances
ISM: bubbles
ISM: individual objects: M1-67
ISM: kinematics and dynamics
Stars: Wolf-Rayet
title_short Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance
title_full Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance
title_fullStr Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance
title_full_unstemmed Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance
title_sort Integral field spectroscopy of M1-67. A Wolf-Rayet nebula with luminous blue variable nebula appearance
dc.creator.none.fl_str_mv Fernández-Martín, Alba
Vílchez Medina, José Manuel
Pérez-Montero, E.
Candian, A.
Sánchez, S. F.
Martín-Gordón, D.
Riera, A.
author Fernández-Martín, Alba
author_facet Fernández-Martín, Alba
Vílchez Medina, José Manuel
Pérez-Montero, E.
Candian, A.
Sánchez, S. F.
Martín-Gordón, D.
Riera, A.
author_role author
author2 Vílchez Medina, José Manuel
Pérez-Montero, E.
Candian, A.
Sánchez, S. F.
Martín-Gordón, D.
Riera, A.
author2_role author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
Ministerio de Educación y Ciencia (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv ISM: abundances
ISM: bubbles
ISM: individual objects: M1-67
ISM: kinematics and dynamics
Stars: Wolf-Rayet
topic ISM: abundances
ISM: bubbles
ISM: individual objects: M1-67
ISM: kinematics and dynamics
Stars: Wolf-Rayet
description Aims: This work aims to disentangle the morphological, kinematic, and chemical components of the nebula M1-67 to shed light on its process of formation around the central Wolf-Rayet (WR) star WR124. Methods: We have carried out integral field spectroscopy observations over two regions of M1-67, covering most of the nebula in the optical range. Maps of electron density, line ratios, and radial velocity were created to perform a detailed analysis of the two-dimensional structure. We studied the physical and chemical properties by means of integrated spectra selected over the whole nebula. Photoionization models were performed to confirm the empirical chemical results theoretically. In addition, we obtained and analysed infrared spectroscopic data and the MIPS 24 μm image of M1-67 from Spitzer. Results: We find that the ionized gas of M1-67 is condensed in knots aligned in a preferred axis along the NE-SW direction, like a bipolar structure. Both electron density and radial velocity decrease in this direction when moving away from the central star. From the derived electron temperature, Te ∼ 8200 K, we have estimated chemical abundances, obtaining that nitrogen appears strongly enriched and oxygen depleted. From the last two results, we infer that this bipolarity is the consequence of an ejection of an evolved stage of WR124 with material processed in the CNO cycle. Furthermore, we find two regions placed outside of the bipolar structure with different spectral and chemical properties. The infrared study has revealed that the bipolar axis is composed of ionized gas with a low ionization degree that is well mixed with warm dust and of a spherical bubble surrounding the ejection at 24 μm. Taking the evolution of a 60 M star and the temporal scale of the bipolar ejection into account, we propose that the observed gas was ejected during an eruption in the luminous blue variable stage. The star has entered the WR phase recently without apparent signs of interaction between WR-winds and interstellar material. © 2013 ESO.
publishDate 2013
dc.date.none.fl_str_mv 2013
2025
2025
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/10261/408884
url http://hdl.handle.net/10261/408884
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MICINN//BES-2008-008120
info:eu-repo/grantAgreement/MICINN//AYA2010-21887-C04-01
info:eu-repo/grantAgreement/MEC//CSD2006-00070
http://dx.doi.org/10.1051/0004-6361/201220773
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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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