THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA

“Water fountains” (WFs) are evolved objects showing high-velocity, collimated jets traced by water maser emission. Most of them are in the post-asymptotic giant branch (post-AGB) and they may represent one of the first manifestations of collimated mass loss in evolved stars. We present water maser,...

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Authors: Gómez, José F., Suárez, Olga, Bendjoya, Philippe, Rizzo, J. Ricardo, Miranda, Luis F., Green, James A., Uscanga, Lucero, García-García, Enrique, Lagadec, Eric, Guerrero, Martín A., Ramos-Larios, Gerardo
Format: article
Status:Versión aceptada para publicación
Publication Date:2015
Country:España
Institution:Consejo Superior de Investigaciones Científicas (CSIC)
Repository:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/397631
Online Access:http://hdl.handle.net/10261/397631
Access Level:Open access
Keyword:Masers
Planetary nebulae: general
Planetary nebulae: individual (IRAS 15103-5754)
Stars: AGB and post-AGB
Stars: mass-loss
Stars: winds, outflows
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oai_identifier_str oai:digital.csic.es:10261/397631
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network_name_str España
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dc.title.none.fl_str_mv THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA
title THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA
spellingShingle THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA
Gómez, José F.
Masers
Planetary nebulae: general
Planetary nebulae: individual (IRAS 15103-5754)
Stars: AGB and post-AGB
Stars: mass-loss
Stars: winds, outflows
title_short THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA
title_full THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA
title_fullStr THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA
title_full_unstemmed THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA
title_sort THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULA
dc.creator.none.fl_str_mv Gómez, José F.
Suárez, Olga
Bendjoya, Philippe
Rizzo, J. Ricardo
Miranda, Luis F.
Green, James A.
Uscanga, Lucero
García-García, Enrique
Lagadec, Eric
Guerrero, Martín A.
Ramos-Larios, Gerardo
author Gómez, José F.
author_facet Gómez, José F.
Suárez, Olga
Bendjoya, Philippe
Rizzo, J. Ricardo
Miranda, Luis F.
Green, James A.
Uscanga, Lucero
García-García, Enrique
Lagadec, Eric
Guerrero, Martín A.
Ramos-Larios, Gerardo
author_role author
author2 Suárez, Olga
Bendjoya, Philippe
Rizzo, J. Ricardo
Miranda, Luis F.
Green, James A.
Uscanga, Lucero
García-García, Enrique
Lagadec, Eric
Guerrero, Martín A.
Ramos-Larios, Gerardo
author2_role author
author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
European Commission
Universidad de Vigo
Consejo Nacional de Ciencia y Tecnología (México)
Science and Technology Facilities Council (UK)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Masers
Planetary nebulae: general
Planetary nebulae: individual (IRAS 15103-5754)
Stars: AGB and post-AGB
Stars: mass-loss
Stars: winds, outflows
topic Masers
Planetary nebulae: general
Planetary nebulae: individual (IRAS 15103-5754)
Stars: AGB and post-AGB
Stars: mass-loss
Stars: winds, outflows
description “Water fountains” (WFs) are evolved objects showing high-velocity, collimated jets traced by water maser emission. Most of them are in the post-asymptotic giant branch (post-AGB) and they may represent one of the first manifestations of collimated mass loss in evolved stars. We present water maser, carbon monoxide, and mid-infrared spectroscopic data (obtained with the Australia Telescope Compact Array, Herschel Space Observatory, and the Very Large Telescope, respectively) toward IRAS 15103−5754, a possible planetary nebula (PN) with WF characteristics. Carbon monoxide observations show that IRAS 15103−5754 is an evolved object, while the mid-IR spectrum displays unambiguous [Ne ii] emission, indicating that photoionization has started and thus, its nature as a PN is confirmed. Water maser spectra show several components spreading over a large velocity range (≃ 75 km s−1) and tracing a collimated jet. This indicates that the object is a WF, the first WF known that has already entered the PN phase. However, the spatial and kinematical distribution of the maser emission in this object are significantly different from those in other WFs. Moreover, the velocity distribution of the maser emission shows a “Hubble-like” flow (higher velocities at larger distances from the central star), consistent with a short-lived, explosive mass-loss event. This velocity pattern is not seen in other WFs (which are presumably in earlier evolutionary stages). We therefore suggest that we are witnessing a fundamental change of mass-loss processes in WFs, with water masers being pumped by steady jets in post-AGB stars, but tracing explosive/ballistic events as the object enters the PN phase. © 2015. The American Astronomical Society. All rights reserved.
publishDate 2015
dc.date.none.fl_str_mv 2015
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/10261/397631
url http://hdl.handle.net/10261/397631
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
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http://dx.doi.org/10.1088/0004-637X/799/2/186
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dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
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)
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spelling THE FIRST “WATER FOUNTAIN” COLLIMATED OUTFLOW IN A PLANETARY NEBULAGómez, José F.Suárez, OlgaBendjoya, PhilippeRizzo, J. RicardoMiranda, Luis F.Green, James A.Uscanga, LuceroGarcía-García, EnriqueLagadec, EricGuerrero, Martín A.Ramos-Larios, GerardoMasersPlanetary nebulae: generalPlanetary nebulae: individual (IRAS 15103-5754)Stars: AGB and post-AGBStars: mass-lossStars: winds, outflows“Water fountains” (WFs) are evolved objects showing high-velocity, collimated jets traced by water maser emission. Most of them are in the post-asymptotic giant branch (post-AGB) and they may represent one of the first manifestations of collimated mass loss in evolved stars. We present water maser, carbon monoxide, and mid-infrared spectroscopic data (obtained with the Australia Telescope Compact Array, Herschel Space Observatory, and the Very Large Telescope, respectively) toward IRAS 15103−5754, a possible planetary nebula (PN) with WF characteristics. Carbon monoxide observations show that IRAS 15103−5754 is an evolved object, while the mid-IR spectrum displays unambiguous [Ne ii] emission, indicating that photoionization has started and thus, its nature as a PN is confirmed. Water maser spectra show several components spreading over a large velocity range (≃ 75 km s−1) and tracing a collimated jet. This indicates that the object is a WF, the first WF known that has already entered the PN phase. However, the spatial and kinematical distribution of the maser emission in this object are significantly different from those in other WFs. Moreover, the velocity distribution of the maser emission shows a “Hubble-like” flow (higher velocities at larger distances from the central star), consistent with a short-lived, explosive mass-loss event. This velocity pattern is not seen in other WFs (which are presumably in earlier evolutionary stages). We therefore suggest that we are witnessing a fundamental change of mass-loss processes in WFs, with water masers being pumped by steady jets in post-AGB stars, but tracing explosive/ballistic events as the object enters the PN phase. © 2015. The American Astronomical Society. All rights reserved..F.G. wishes to express his gratitude to CSIRO Astronomy and Space Science, and the Observatoire de la Côte d'Azur for their support and hospitality during the preparation of this paper. J.F.G., O.S., and L.F.M. are supported by MICINN (Spain) grant AYA2011-30228-C03-01, while M.A.G. is supported by grant AYA2011-29754-C03-02 (both grants include FEDER funds). J.R.R. acknowledges support from MICINN grants CSD2009-00038, AYA2009-07304, and AYA2012-32032. L.F.M. acknowledges partial support from grant 12VI20 of the Universidad de Vigo. L.U. is supported by grant PE9-1160 of the Greek General Secretariat for Research and Technology in the framework of the program Support of Postdoctoral Researchers. G.R.L. acknowledges support from CONACyT and PROMEP (Mexico). This paper made use of information from the Red MSX Source survey database at http://rms.leeds.ac.uk/cgi-bin/public/RMS_DATABASE.cgi, which was constructed with support from the Science and Technology Facilities Council of the UK.Peer reviewedIOP PublishingMinisterio de Ciencia e Innovación (España)European CommissionUniversidad de VigoConsejo Nacional de Ciencia y Tecnología (México)Science and Technology Facilities Council (UK)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202520252015info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Postprintinfo:eu-repo/semantics/acceptedVersionhttp://hdl.handle.net/10261/397631reponame: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##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MICINN//AYA2011-30228-C03-01info:eu-repo/grantAgreement/MICINN//AYA2011-29754-C03-02info:eu-repo/grantAgreement/MICINN//CSD2009-00038info:eu-repo/grantAgreement/MICINN//AYA2009-07304info:eu-repo/grantAgreement/MINECO//AYA2012-32032http://dx.doi.org/10.1088/0004-637X/799/2/186Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3976312026-05-22T06:33:51Z
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