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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/44320
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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 Técnicas2025-09-29T10:24:26Zoai: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:34982025-09-29 10:24:26.303CONICET 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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1844614240932986880 |
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13.070432 |