Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group

Autores
Fang, Xuan; García-Benito, Rubén; Guerrero, Martín A.; Zhang, Yong; Liu, Xiaowei; Morisset, Christophe; Karakas, Amanda I.; Miller Bertolami, Marcelo Miguel; Yuan, Haibo; Cabrera Lavers, Antonio
Año de publicación
2018
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We report deep spectroscopy of 10 planetary nebulae (PNe) in the Andromeda Galaxy (M31) using the 10.4 m Gran Telescopio Canarias (GTC). Our targets reside in different regions of M31, including halo streams and the dwarf satellite M32, and kinematically deviate from the extended disk. The temperature-sensitive [O iii] λ4363 line is observed in all PNe. For four PNe, the GTC spectra extend beyond 1 μm, enabling the explicit detection of the [S iii] λ6312 and λλ9069, 9531 lines and thus determination of the [S iii] temperature. Abundance ratios are derived and generally consistent with AGB model predictions. Our PNe probably all evolved from low-mass (<2 M Ȯ) stars, as analyzed with the most up-to-date post-AGB evolutionary models, and their main-sequence ages are mostly ∼2-5 Gyr. Compared to the underlying, smooth, metal-poor halo of M31, our targets are uniformly metal rich ([O/H]-0.4), and seem to resemble the younger population in the stream. We thus speculate that our halo PNe formed in the Giant Stream's progenitor through extended star formation. Alternatively, they might have formed from the same metal-rich gas as did the outer-disk PNe but were displaced into their present locations as a result of galactic interactions. These interpretations are, although speculative, qualitatively in line with the current picture, as inferred from previous wide-field photometric surveys, that M31's halo is the result of complex interactions and merger processes. The behavior of the N/O of the combined sample of the outer-disk and our halo/substructure PNe signifies that hot bottom burning might actually occur at <3 M Ȯ but careful assessment is needed.
Fil: Fang, Xuan. Chinese Academy of Sciences; República de China
Fil: García-Benito, Rubén. Instituto de Astrofísica de Andalucía; España
Fil: Guerrero, Martín A.. Instituto de Astrofísica de Andalucía; España
Fil: Zhang, Yong. University of Hong Kong; China
Fil: Liu, Xiaowei. Peking University; China. Yunnan University; China
Fil: Morisset, Christophe. Universidad Nacional Autónoma de México; México
Fil: Karakas, Amanda I.. Monash University; Australia
Fil: Miller Bertolami, Marcelo Miguel. Instituto de Astrofísica de la Plata (conicet- Universidad Nacional de la Plata); Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Yuan, Haibo. Beijing Normal University; China
Fil: Cabrera Lavers, Antonio. Instituto Astrofisico de Canarias; España
Materia
GALAXIES: ABUNDANCES
GALAXIES: EVOLUTION
GALAXIES: INDIVIDUAL (M31)
ISM: ABUNDANCES
PLANETARY NEBULAE: GENERAL
STARS: EVOLUTION
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/82602
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/82602
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk GroupFang, XuanGarcía-Benito, RubénGuerrero, Martín A.Zhang, YongLiu, XiaoweiMorisset, ChristopheKarakas, Amanda I.Miller Bertolami, Marcelo MiguelYuan, HaiboCabrera Lavers, AntonioGALAXIES: ABUNDANCESGALAXIES: EVOLUTIONGALAXIES: INDIVIDUAL (M31)ISM: ABUNDANCESPLANETARY NEBULAE: GENERALSTARS: EVOLUTIONhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We report deep spectroscopy of 10 planetary nebulae (PNe) in the Andromeda Galaxy (M31) using the 10.4 m Gran Telescopio Canarias (GTC). Our targets reside in different regions of M31, including halo streams and the dwarf satellite M32, and kinematically deviate from the extended disk. The temperature-sensitive [O iii] λ4363 line is observed in all PNe. For four PNe, the GTC spectra extend beyond 1 μm, enabling the explicit detection of the [S iii] λ6312 and λλ9069, 9531 lines and thus determination of the [S iii] temperature. Abundance ratios are derived and generally consistent with AGB model predictions. Our PNe probably all evolved from low-mass (<2 M Ȯ) stars, as analyzed with the most up-to-date post-AGB evolutionary models, and their main-sequence ages are mostly ∼2-5 Gyr. Compared to the underlying, smooth, metal-poor halo of M31, our targets are uniformly metal rich ([O/H]-0.4), and seem to resemble the younger population in the stream. We thus speculate that our halo PNe formed in the Giant Stream's progenitor through extended star formation. Alternatively, they might have formed from the same metal-rich gas as did the outer-disk PNe but were displaced into their present locations as a result of galactic interactions. These interpretations are, although speculative, qualitatively in line with the current picture, as inferred from previous wide-field photometric surveys, that M31's halo is the result of complex interactions and merger processes. The behavior of the N/O of the combined sample of the outer-disk and our halo/substructure PNe signifies that hot bottom burning might actually occur at <3 M Ȯ but careful assessment is needed.Fil: Fang, Xuan. Chinese Academy of Sciences; República de ChinaFil: García-Benito, Rubén. Instituto de Astrofísica de Andalucía; EspañaFil: Guerrero, Martín A.. Instituto de Astrofísica de Andalucía; EspañaFil: Zhang, Yong. University of Hong Kong; ChinaFil: Liu, Xiaowei. Peking University; China. Yunnan University; ChinaFil: Morisset, Christophe. Universidad Nacional Autónoma de México; MéxicoFil: Karakas, Amanda I.. Monash University; AustraliaFil: Miller Bertolami, Marcelo Miguel. Instituto de Astrofísica de la Plata (conicet- Universidad Nacional de la Plata); Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Yuan, Haibo. Beijing Normal University; ChinaFil: Cabrera Lavers, Antonio. Instituto Astrofisico de Canarias; EspañaIOP Publishing2018-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/82602Fang, Xuan; García-Benito, Rubén; Guerrero, Martín A.; Zhang, Yong; Liu, Xiaowei; et al.; Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group; IOP Publishing; Astrophysical Journal; 853; 1; 1-20180004-637XCONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aaa1e5info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/0004-637X/853/1/50/info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:03:24Zoai:ri.conicet.gov.ar:11336/82602instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:03:24.741CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group
title Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group
spellingShingle Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group
Fang, Xuan
GALAXIES: ABUNDANCES
GALAXIES: EVOLUTION
GALAXIES: INDIVIDUAL (M31)
ISM: ABUNDANCES
PLANETARY NEBULAE: GENERAL
STARS: EVOLUTION
title_short Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group
title_full Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group
title_fullStr Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group
title_full_unstemmed Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group
title_sort Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group
dc.creator.none.fl_str_mv Fang, Xuan
García-Benito, Rubén
Guerrero, Martín A.
Zhang, Yong
Liu, Xiaowei
Morisset, Christophe
Karakas, Amanda I.
Miller Bertolami, Marcelo Miguel
Yuan, Haibo
Cabrera Lavers, Antonio
author Fang, Xuan
author_facet Fang, Xuan
García-Benito, Rubén
Guerrero, Martín A.
Zhang, Yong
Liu, Xiaowei
Morisset, Christophe
Karakas, Amanda I.
Miller Bertolami, Marcelo Miguel
Yuan, Haibo
Cabrera Lavers, Antonio
author_role author
author2 García-Benito, Rubén
Guerrero, Martín A.
Zhang, Yong
Liu, Xiaowei
Morisset, Christophe
Karakas, Amanda I.
Miller Bertolami, Marcelo Miguel
Yuan, Haibo
Cabrera Lavers, Antonio
author2_role author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv GALAXIES: ABUNDANCES
GALAXIES: EVOLUTION
GALAXIES: INDIVIDUAL (M31)
ISM: ABUNDANCES
PLANETARY NEBULAE: GENERAL
STARS: EVOLUTION
topic GALAXIES: ABUNDANCES
GALAXIES: EVOLUTION
GALAXIES: INDIVIDUAL (M31)
ISM: ABUNDANCES
PLANETARY NEBULAE: GENERAL
STARS: EVOLUTION
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv We report deep spectroscopy of 10 planetary nebulae (PNe) in the Andromeda Galaxy (M31) using the 10.4 m Gran Telescopio Canarias (GTC). Our targets reside in different regions of M31, including halo streams and the dwarf satellite M32, and kinematically deviate from the extended disk. The temperature-sensitive [O iii] λ4363 line is observed in all PNe. For four PNe, the GTC spectra extend beyond 1 μm, enabling the explicit detection of the [S iii] λ6312 and λλ9069, 9531 lines and thus determination of the [S iii] temperature. Abundance ratios are derived and generally consistent with AGB model predictions. Our PNe probably all evolved from low-mass (<2 M Ȯ) stars, as analyzed with the most up-to-date post-AGB evolutionary models, and their main-sequence ages are mostly ∼2-5 Gyr. Compared to the underlying, smooth, metal-poor halo of M31, our targets are uniformly metal rich ([O/H]-0.4), and seem to resemble the younger population in the stream. We thus speculate that our halo PNe formed in the Giant Stream's progenitor through extended star formation. Alternatively, they might have formed from the same metal-rich gas as did the outer-disk PNe but were displaced into their present locations as a result of galactic interactions. These interpretations are, although speculative, qualitatively in line with the current picture, as inferred from previous wide-field photometric surveys, that M31's halo is the result of complex interactions and merger processes. The behavior of the N/O of the combined sample of the outer-disk and our halo/substructure PNe signifies that hot bottom burning might actually occur at <3 M Ȯ but careful assessment is needed.
Fil: Fang, Xuan. Chinese Academy of Sciences; República de China
Fil: García-Benito, Rubén. Instituto de Astrofísica de Andalucía; España
Fil: Guerrero, Martín A.. Instituto de Astrofísica de Andalucía; España
Fil: Zhang, Yong. University of Hong Kong; China
Fil: Liu, Xiaowei. Peking University; China. Yunnan University; China
Fil: Morisset, Christophe. Universidad Nacional Autónoma de México; México
Fil: Karakas, Amanda I.. Monash University; Australia
Fil: Miller Bertolami, Marcelo Miguel. Instituto de Astrofísica de la Plata (conicet- Universidad Nacional de la Plata); Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Yuan, Haibo. Beijing Normal University; China
Fil: Cabrera Lavers, Antonio. Instituto Astrofisico de Canarias; España
description We report deep spectroscopy of 10 planetary nebulae (PNe) in the Andromeda Galaxy (M31) using the 10.4 m Gran Telescopio Canarias (GTC). Our targets reside in different regions of M31, including halo streams and the dwarf satellite M32, and kinematically deviate from the extended disk. The temperature-sensitive [O iii] λ4363 line is observed in all PNe. For four PNe, the GTC spectra extend beyond 1 μm, enabling the explicit detection of the [S iii] λ6312 and λλ9069, 9531 lines and thus determination of the [S iii] temperature. Abundance ratios are derived and generally consistent with AGB model predictions. Our PNe probably all evolved from low-mass (<2 M Ȯ) stars, as analyzed with the most up-to-date post-AGB evolutionary models, and their main-sequence ages are mostly ∼2-5 Gyr. Compared to the underlying, smooth, metal-poor halo of M31, our targets are uniformly metal rich ([O/H]-0.4), and seem to resemble the younger population in the stream. We thus speculate that our halo PNe formed in the Giant Stream's progenitor through extended star formation. Alternatively, they might have formed from the same metal-rich gas as did the outer-disk PNe but were displaced into their present locations as a result of galactic interactions. These interpretations are, although speculative, qualitatively in line with the current picture, as inferred from previous wide-field photometric surveys, that M31's halo is the result of complex interactions and merger processes. The behavior of the N/O of the combined sample of the outer-disk and our halo/substructure PNe signifies that hot bottom burning might actually occur at <3 M Ȯ but careful assessment is needed.
publishDate 2018
dc.date.none.fl_str_mv 2018-01
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/82602
Fang, Xuan; García-Benito, Rubén; Guerrero, Martín A.; Zhang, Yong; Liu, Xiaowei; et al.; Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group; IOP Publishing; Astrophysical Journal; 853; 1; 1-2018
0004-637X
CONICET Digital
CONICET
url http://hdl.handle.net/11336/82602
identifier_str_mv Fang, Xuan; García-Benito, Rubén; Guerrero, Martín A.; Zhang, Yong; Liu, Xiaowei; et al.; Chemical abundances of planetary nebulae in the substructures of M31. II. the extended sample and a comparison study with the Outer-disk Group; IOP Publishing; Astrophysical Journal; 853; 1; 1-2018
0004-637X
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aaa1e5
info:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/0004-637X/853/1/50/
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv IOP Publishing
publisher.none.fl_str_mv IOP Publishing
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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score 13.070432

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