Stellar populations in the Canis Major overdensity

Autores
Carraro, Giovanni; Moitinho, André; Vazquez, Ruben Angel
Año de publicación
2008
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We performed a photometric multicolor survey of the core of the Canis Major overdensity at l ≈ 244o, b ≈ −8.0o , reaching V ∼ 22 and covering 0 o . 3 × 1 o .0. The main aim is to unravel the complex mixture of stellar populations toward this Galactic direction, where in the recent past important signatures of an accretion event have been claimed to be detected. While our previous investigations were based on disjointed pointings aimed at revealing the large scale structure of the third Galactic Quadrant, we now focus on a complete coverage of a smaller field centered on the Canis Major overdensity. A large wave-length baseline, in the UBV RI bands, allows us to build up a suite of colour colour and colour magnitude diagrams, providing a much better diagnostic tool to disentangle the stellar populations of the region. In fact, the simple use of one colour magnitude diagram, widely employed in all the previous studies defending the existence of the Canis Major galaxy, does not allow one to separate the effects of the different parameters (reddening, age, metallicity, and distance) involved in the interpretation of data, forcing to rely on heavy modeling. In agreement with our previous studies in the same general region of the Milky Way, we recognize a young stellar population compatible with the expected structure and extension of the Local (Orion) and Outer (Norma-Cygnus) spiral arms in the Third Galactic Quadrant. Moreover we interpret the conspicuous intermediate-age metal poor population as belonging to the Galactic thick disk, distorted by the effect of strong disk warping at this latitude, and to the Galactic halo
Fil: Carraro, Giovanni. European Southern Observatory; Chile
Fil: Moitinho, André. Universidad de Lisboa; Portugal
Fil: Vazquez, Ruben Angel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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
Materia
Galaxy
Evolution
Structure
Galactic halo
Milky Way
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:11336/44320
Acceder
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network_name_str CONICET Digital (CONICET)
spelling Stellar populations in the Canis Major overdensityCarraro, GiovanniMoitinho, AndréVazquez, Ruben AngelGalaxyEvolutionStructureGalactic haloMilky Wayhttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1We performed a photometric multicolor survey of the core of the Canis Major overdensity at l ≈ 244o, b ≈ −8.0o , reaching V ∼ 22 and covering 0 o . 3 × 1 o .0. The main aim is to unravel the complex mixture of stellar populations toward this Galactic direction, where in the recent past important signatures of an accretion event have been claimed to be detected. While our previous investigations were based on disjointed pointings aimed at revealing the large scale structure of the third Galactic Quadrant, we now focus on a complete coverage of a smaller field centered on the Canis Major overdensity. A large wave-length baseline, in the UBV RI bands, allows us to build up a suite of colour colour and colour magnitude diagrams, providing a much better diagnostic tool to disentangle the stellar populations of the region. In fact, the simple use of one colour magnitude diagram, widely employed in all the previous studies defending the existence of the Canis Major galaxy, does not allow one to separate the effects of the different parameters (reddening, age, metallicity, and distance) involved in the interpretation of data, forcing to rely on heavy modeling. In agreement with our previous studies in the same general region of the Milky Way, we recognize a young stellar population compatible with the expected structure and extension of the Local (Orion) and Outer (Norma-Cygnus) spiral arms in the Third Galactic Quadrant. Moreover we interpret the conspicuous intermediate-age metal poor population as belonging to the Galactic thick disk, distorted by the effect of strong disk warping at this latitude, and to the Galactic haloFil: Carraro, Giovanni. European Southern Observatory; ChileFil: Moitinho, André. Universidad de Lisboa; PortugalFil: Vazquez, Ruben Angel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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; ArgentinaWiley Blackwell Publishing, Inc2008-12info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/44320Carraro, Giovanni; Moitinho, André; Vazquez, Ruben Angel; Stellar populations in the Canis Major overdensity; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 385; 12-2008; 1597-16040035-8711CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.12953.xinfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/385/3/1597/1013518info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-22T11:57:11Zoai:ri.conicet.gov.ar:11336/44320instacron: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:34982025-10-22 11:57:12.192CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Stellar populations in the Canis Major overdensity
title Stellar populations in the Canis Major overdensity
spellingShingle Stellar populations in the Canis Major overdensity
Carraro, Giovanni
Galaxy
Evolution
Structure
Galactic halo
Milky Way
title_short Stellar populations in the Canis Major overdensity
title_full Stellar populations in the Canis Major overdensity
title_fullStr Stellar populations in the Canis Major overdensity
title_full_unstemmed Stellar populations in the Canis Major overdensity
title_sort Stellar populations in the Canis Major overdensity
dc.creator.none.fl_str_mv Carraro, Giovanni
Moitinho, André
Vazquez, Ruben Angel
author Carraro, Giovanni
author_facet Carraro, Giovanni
Moitinho, André
Vazquez, Ruben Angel
author_role author
author2 Moitinho, André
Vazquez, Ruben Angel
author2_role author
author
dc.subject.none.fl_str_mv Galaxy
Evolution
Structure
Galactic halo
Milky Way
topic Galaxy
Evolution
Structure
Galactic halo
Milky Way
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 performed a photometric multicolor survey of the core of the Canis Major overdensity at l ≈ 244o, b ≈ −8.0o , reaching V ∼ 22 and covering 0 o . 3 × 1 o .0. The main aim is to unravel the complex mixture of stellar populations toward this Galactic direction, where in the recent past important signatures of an accretion event have been claimed to be detected. While our previous investigations were based on disjointed pointings aimed at revealing the large scale structure of the third Galactic Quadrant, we now focus on a complete coverage of a smaller field centered on the Canis Major overdensity. A large wave-length baseline, in the UBV RI bands, allows us to build up a suite of colour colour and colour magnitude diagrams, providing a much better diagnostic tool to disentangle the stellar populations of the region. In fact, the simple use of one colour magnitude diagram, widely employed in all the previous studies defending the existence of the Canis Major galaxy, does not allow one to separate the effects of the different parameters (reddening, age, metallicity, and distance) involved in the interpretation of data, forcing to rely on heavy modeling. In agreement with our previous studies in the same general region of the Milky Way, we recognize a young stellar population compatible with the expected structure and extension of the Local (Orion) and Outer (Norma-Cygnus) spiral arms in the Third Galactic Quadrant. Moreover we interpret the conspicuous intermediate-age metal poor population as belonging to the Galactic thick disk, distorted by the effect of strong disk warping at this latitude, and to the Galactic halo
Fil: Carraro, Giovanni. European Southern Observatory; Chile
Fil: Moitinho, André. Universidad de Lisboa; Portugal
Fil: Vazquez, Ruben Angel. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; 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
description We performed a photometric multicolor survey of the core of the Canis Major overdensity at l ≈ 244o, b ≈ −8.0o , reaching V ∼ 22 and covering 0 o . 3 × 1 o .0. The main aim is to unravel the complex mixture of stellar populations toward this Galactic direction, where in the recent past important signatures of an accretion event have been claimed to be detected. While our previous investigations were based on disjointed pointings aimed at revealing the large scale structure of the third Galactic Quadrant, we now focus on a complete coverage of a smaller field centered on the Canis Major overdensity. A large wave-length baseline, in the UBV RI bands, allows us to build up a suite of colour colour and colour magnitude diagrams, providing a much better diagnostic tool to disentangle the stellar populations of the region. In fact, the simple use of one colour magnitude diagram, widely employed in all the previous studies defending the existence of the Canis Major galaxy, does not allow one to separate the effects of the different parameters (reddening, age, metallicity, and distance) involved in the interpretation of data, forcing to rely on heavy modeling. In agreement with our previous studies in the same general region of the Milky Way, we recognize a young stellar population compatible with the expected structure and extension of the Local (Orion) and Outer (Norma-Cygnus) spiral arms in the Third Galactic Quadrant. Moreover we interpret the conspicuous intermediate-age metal poor population as belonging to the Galactic thick disk, distorted by the effect of strong disk warping at this latitude, and to the Galactic halo
publishDate 2008
dc.date.none.fl_str_mv 2008-12
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/11336/44320
Carraro, Giovanni; Moitinho, André; Vazquez, Ruben Angel; Stellar populations in the Canis Major overdensity; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 385; 12-2008; 1597-1604
0035-8711
CONICET Digital
CONICET
url http://hdl.handle.net/11336/44320
identifier_str_mv Carraro, Giovanni; Moitinho, André; Vazquez, Ruben Angel; Stellar populations in the Canis Major overdensity; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 385; 12-2008; 1597-1604
0035-8711
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.12953.x
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article/385/3/1597/1013518
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 Wiley Blackwell Publishing, Inc
publisher.none.fl_str_mv Wiley Blackwell Publishing, Inc
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 12.982451

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