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
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/93569
Ver los metadatos del registro completo
id |
SEDICI_5460ed50ed3cb9863385bce054a58c7e |
---|---|
oai_identifier_str |
oai:sedici.unlp.edu.ar:10915/93569 |
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 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://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 |
dc.relation.none.fl_str_mv |
info: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/11336/82602 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 instacron:UNLP |
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 |
_version_ |
1844616068145872896 |
score |
13.070432 |