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⊙) 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⊙ but careful assessment is needed.
Instituto de Astrofísica de La Plata
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Astronomía
galaxies: abundances
galaxies: evolution
galaxies: individual (M31)
ISM: abundances
planetary nebulae: general
stars: evolution
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by/3.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/93569

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network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
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, AntonioAstronomíagalaxies: abundancesgalaxies: evolutiongalaxies: individual (M31)ISM: abundancesplanetary nebulae: generalstars: evolutionWe 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⊙) 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⊙ but careful assessment is needed.Instituto de Astrofísica de La PlataFacultad de Ciencias Astronómicas y Geofísicas2018-01info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/93569enginfo:eu-repo/semantics/altIdentifier/url/https://iopscience.iop.org/0004-637X/853/1/50/info:eu-repo/semantics/altIdentifier/url/https://ri.conicet.gov.ar/handle/11336/82602info:eu-repo/semantics/altIdentifier/issn/0004-637Xinfo:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aaa1e5info:eu-repo/semantics/altIdentifier/hdl/11336/82602info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by/3.0/Creative Commons Attribution 3.0 Unported (CC BY 3.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:19:26Zoai:sedici.unlp.edu.ar:10915/93569Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:19:27.019SEDICI (UNLP) - Universidad Nacional de La Platafalse
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
Astronomía
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 Astronomía
galaxies: abundances
galaxies: evolution
galaxies: individual (M31)
ISM: abundances
planetary nebulae: general
stars: evolution
topic Astronomía
galaxies: abundances
galaxies: evolution
galaxies: individual (M31)
ISM: abundances
planetary nebulae: general
stars: evolution
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⊙) 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⊙ but careful assessment is needed.
Instituto de Astrofísica de La Plata
Facultad de Ciencias Astronómicas y Geofísicas
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⊙) 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⊙ 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
Articulo
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info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://sedici.unlp.edu.ar/handle/10915/93569
url http://sedici.unlp.edu.ar/handle/10915/93569
dc.language.none.fl_str_mv eng
language eng
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info:eu-repo/semantics/altIdentifier/url/https://ri.conicet.gov.ar/handle/11336/82602
info:eu-repo/semantics/altIdentifier/issn/0004-637X
info:eu-repo/semantics/altIdentifier/doi/10.3847/1538-4357/aaa1e5
info:eu-repo/semantics/altIdentifier/hdl/11336/82602
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/3.0/
Creative Commons Attribution 3.0 Unported (CC BY 3.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by/3.0/
Creative Commons Attribution 3.0 Unported (CC BY 3.0)
dc.format.none.fl_str_mv application/pdf
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
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reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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