The thickening of the thin disk in the third galactic quadrant

Autores
Carraro, Giovanni; Vázquez, Rubén Ángel; Acosta, Edgardo; Ahumada, Javier A.; Giorgi, Edgard Ervar Salvador
Año de publicación
2015
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
In the third Galactic quadrant (180° ≤ l ≤ 270°) of the Milky Way, the Galactic thin disk exhibits a significant Warp-shown both by gas and young stars-bending down a few kiloparsecs below the formal Galactic plane (b = 0°). This warp shows its maximum at l ∼ 240°, in the direction of the Canis Major constellation. In a series of papers, we have traced the detailed structure of this region using open star clusters, putting particular emphasis on the spiral structure of the outer disk. We noted a conspicuous accumulation of young star clusters within 2-3 kpc from the Sun and close to b = 0°, which we interpreted as the continuation of the Local (Orion) arm toward the outer disk. While most clusters (and young stars in their background) closely follow the warp of the disk, our decade-old survey of the spiral structure of this region led us to identify three clusters, Haffner 18 (1 and 2) and Haffner 19, which remain very close to b = 0° and lie at distances (4.5, ∼8.0, and 6.4 kpc) where most of the material is already significantly warped. Here, we report on a search for clusters that share the same properties as Haffner 18 and 19, and investigate the possible reasons for such an unexpected occurrence. We present UBVRI photometry of five young clusters, namely NGC 2345, NGC 2374, Trumpler 9, Haffner 20, and Haffner 21, which also lie close to the formal Galactic plane. With the exception of Haffner 20, in the background of these clusters we detected young stars that appear close to b = 0° and are located at distances up to ∼8 kpc from the Sun, thus deviating significantly from the warp. These populations define a structure that distributes over almost the entire third Galactic quadrant. We discuss this structure in the context of a possible thin disk flaring, similar to the Galactic thick disk.
Instituto de Astrofísica de La Plata
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Galaxy: disk
Galaxy: structure
Hertzsprung-Russell and C-M diagrams
open clusters and associations: general
open clusters and associations: individual (Haffner 20 Haffner 21 NGC 2345 NGC 2374 Trumpler 9)
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/86463

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repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling The thickening of the thin disk in the third galactic quadrantCarraro, GiovanniVázquez, Rubén ÁngelAcosta, EdgardoAhumada, Javier A.Giorgi, Edgard Ervar SalvadorCiencias AstronómicasGalaxy: diskGalaxy: structureHertzsprung-Russell and C-M diagramsopen clusters and associations: generalopen clusters and associations: individual (Haffner 20 Haffner 21 NGC 2345 NGC 2374 Trumpler 9)In the third Galactic quadrant (180° ≤ l ≤ 270°) of the Milky Way, the Galactic thin disk exhibits a significant Warp-shown both by gas and young stars-bending down a few kiloparsecs below the formal Galactic plane (b = 0°). This warp shows its maximum at l ∼ 240°, in the direction of the Canis Major constellation. In a series of papers, we have traced the detailed structure of this region using open star clusters, putting particular emphasis on the spiral structure of the outer disk. We noted a conspicuous accumulation of young star clusters within 2-3 kpc from the Sun and close to b = 0°, which we interpreted as the continuation of the Local (Orion) arm toward the outer disk. While most clusters (and young stars in their background) closely follow the warp of the disk, our decade-old survey of the spiral structure of this region led us to identify three clusters, Haffner 18 (1 and 2) and Haffner 19, which remain very close to b = 0° and lie at distances (4.5, ∼8.0, and 6.4 kpc) where most of the material is already significantly warped. Here, we report on a search for clusters that share the same properties as Haffner 18 and 19, and investigate the possible reasons for such an unexpected occurrence. We present UBVRI photometry of five young clusters, namely NGC 2345, NGC 2374, Trumpler 9, Haffner 20, and Haffner 21, which also lie close to the formal Galactic plane. With the exception of Haffner 20, in the background of these clusters we detected young stars that appear close to b = 0° and are located at distances up to ∼8 kpc from the Sun, thus deviating significantly from the warp. These populations define a structure that distributes over almost the entire third Galactic quadrant. We discuss this structure in the context of a possible thin disk flaring, similar to the Galactic thick disk.Instituto de Astrofísica de La PlataFacultad de Ciencias Astronómicas y Geofísicas2015info: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/10915/86463enginfo:eu-repo/semantics/altIdentifier/issn/0004-6256info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/149/1/12info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-09-29T11:16:59Zoai:sedici.unlp.edu.ar:10915/86463Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:59.479SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv The thickening of the thin disk in the third galactic quadrant
title The thickening of the thin disk in the third galactic quadrant
spellingShingle The thickening of the thin disk in the third galactic quadrant
Carraro, Giovanni
Ciencias Astronómicas
Galaxy: disk
Galaxy: structure
Hertzsprung-Russell and C-M diagrams
open clusters and associations: general
open clusters and associations: individual (Haffner 20 Haffner 21 NGC 2345 NGC 2374 Trumpler 9)
title_short The thickening of the thin disk in the third galactic quadrant
title_full The thickening of the thin disk in the third galactic quadrant
title_fullStr The thickening of the thin disk in the third galactic quadrant
title_full_unstemmed The thickening of the thin disk in the third galactic quadrant
title_sort The thickening of the thin disk in the third galactic quadrant
dc.creator.none.fl_str_mv Carraro, Giovanni
Vázquez, Rubén Ángel
Acosta, Edgardo
Ahumada, Javier A.
Giorgi, Edgard Ervar Salvador
author Carraro, Giovanni
author_facet Carraro, Giovanni
Vázquez, Rubén Ángel
Acosta, Edgardo
Ahumada, Javier A.
Giorgi, Edgard Ervar Salvador
author_role author
author2 Vázquez, Rubén Ángel
Acosta, Edgardo
Ahumada, Javier A.
Giorgi, Edgard Ervar Salvador
author2_role author
author
author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Galaxy: disk
Galaxy: structure
Hertzsprung-Russell and C-M diagrams
open clusters and associations: general
open clusters and associations: individual (Haffner 20 Haffner 21 NGC 2345 NGC 2374 Trumpler 9)
topic Ciencias Astronómicas
Galaxy: disk
Galaxy: structure
Hertzsprung-Russell and C-M diagrams
open clusters and associations: general
open clusters and associations: individual (Haffner 20 Haffner 21 NGC 2345 NGC 2374 Trumpler 9)
dc.description.none.fl_txt_mv In the third Galactic quadrant (180° ≤ l ≤ 270°) of the Milky Way, the Galactic thin disk exhibits a significant Warp-shown both by gas and young stars-bending down a few kiloparsecs below the formal Galactic plane (b = 0°). This warp shows its maximum at l ∼ 240°, in the direction of the Canis Major constellation. In a series of papers, we have traced the detailed structure of this region using open star clusters, putting particular emphasis on the spiral structure of the outer disk. We noted a conspicuous accumulation of young star clusters within 2-3 kpc from the Sun and close to b = 0°, which we interpreted as the continuation of the Local (Orion) arm toward the outer disk. While most clusters (and young stars in their background) closely follow the warp of the disk, our decade-old survey of the spiral structure of this region led us to identify three clusters, Haffner 18 (1 and 2) and Haffner 19, which remain very close to b = 0° and lie at distances (4.5, ∼8.0, and 6.4 kpc) where most of the material is already significantly warped. Here, we report on a search for clusters that share the same properties as Haffner 18 and 19, and investigate the possible reasons for such an unexpected occurrence. We present UBVRI photometry of five young clusters, namely NGC 2345, NGC 2374, Trumpler 9, Haffner 20, and Haffner 21, which also lie close to the formal Galactic plane. With the exception of Haffner 20, in the background of these clusters we detected young stars that appear close to b = 0° and are located at distances up to ∼8 kpc from the Sun, thus deviating significantly from the warp. These populations define a structure that distributes over almost the entire third Galactic quadrant. We discuss this structure in the context of a possible thin disk flaring, similar to the Galactic thick disk.
Instituto de Astrofísica de La Plata
Facultad de Ciencias Astronómicas y Geofísicas
description In the third Galactic quadrant (180° ≤ l ≤ 270°) of the Milky Way, the Galactic thin disk exhibits a significant Warp-shown both by gas and young stars-bending down a few kiloparsecs below the formal Galactic plane (b = 0°). This warp shows its maximum at l ∼ 240°, in the direction of the Canis Major constellation. In a series of papers, we have traced the detailed structure of this region using open star clusters, putting particular emphasis on the spiral structure of the outer disk. We noted a conspicuous accumulation of young star clusters within 2-3 kpc from the Sun and close to b = 0°, which we interpreted as the continuation of the Local (Orion) arm toward the outer disk. While most clusters (and young stars in their background) closely follow the warp of the disk, our decade-old survey of the spiral structure of this region led us to identify three clusters, Haffner 18 (1 and 2) and Haffner 19, which remain very close to b = 0° and lie at distances (4.5, ∼8.0, and 6.4 kpc) where most of the material is already significantly warped. Here, we report on a search for clusters that share the same properties as Haffner 18 and 19, and investigate the possible reasons for such an unexpected occurrence. We present UBVRI photometry of five young clusters, namely NGC 2345, NGC 2374, Trumpler 9, Haffner 20, and Haffner 21, which also lie close to the formal Galactic plane. With the exception of Haffner 20, in the background of these clusters we detected young stars that appear close to b = 0° and are located at distances up to ∼8 kpc from the Sun, thus deviating significantly from the warp. These populations define a structure that distributes over almost the entire third Galactic quadrant. We discuss this structure in the context of a possible thin disk flaring, similar to the Galactic thick disk.
publishDate 2015
dc.date.none.fl_str_mv 2015
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/10915/86463
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dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6256
info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-6256/149/1/12
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
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)
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instname_str Universidad Nacional de La Plata
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institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
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