Stellar populations in the Canis Major overdensity
- Autores
- Carraro, Giovanni; Moitinho, André; Vázquez, Rubén Ángel
- Año de publicación
- 2008
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We performed a photometric multicolour survey of the core of the Canis Major overdensity at l ≈ 244°, b ≈ —8°.0, reaching V ~ 22 and covering 0.3 x 1.0 arcmin2. 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 centred on the Canis Major overdensity. A large wavelength baseline, in the UBVRI 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 modelling. In agreement with our previous studies, in the same general region ofthe Milky Way, we recognize a young stellar population compatible with the expected structure and extension of the Local (Orion) and Outer (NormaCygnus) spiral arms in the Third Galactic Quadrant. Moreover, we interpret the conspicuous intermediate-age metal-poor population as belonging to the Galactic thick disc, distorted by the effect of strong disc warping at this latitude, and to the Galactic halo.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Galaxy: evolution
Galaxy: stellar content
Galaxy: structure - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/83524
Ver los metadatos del registro completo
id |
SEDICI_c6e3b213b87f8ae54dff9f8603ef6a6c |
---|---|
oai_identifier_str |
oai:sedici.unlp.edu.ar:10915/83524 |
network_acronym_str |
SEDICI |
repository_id_str |
1329 |
network_name_str |
SEDICI (UNLP) |
spelling |
Stellar populations in the Canis Major overdensityCarraro, GiovanniMoitinho, AndréVázquez, Rubén ÁngelCiencias AstronómicasGalaxy: evolutionGalaxy: stellar contentGalaxy: structureWe performed a photometric multicolour survey of the core of the Canis Major overdensity at l ≈ 244°, b ≈ —8°.0, reaching V ~ 22 and covering 0.3 x 1.0 arcmin2. 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 centred on the Canis Major overdensity. A large wavelength baseline, in the UBVRI 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 modelling. In agreement with our previous studies, in the same general region ofthe Milky Way, we recognize a young stellar population compatible with the expected structure and extension of the Local (Orion) and Outer (NormaCygnus) spiral arms in the Third Galactic Quadrant. Moreover, we interpret the conspicuous intermediate-age metal-poor population as belonging to the Galactic thick disc, distorted by the effect of strong disc warping at this latitude, and to the Galactic halo.Facultad de Ciencias Astronómicas y Geofísicas2008info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf1597-1604http://sedici.unlp.edu.ar/handle/10915/83524enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.12953.xinfo: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:UNLP2025-09-29T11:15:41Zoai:sedici.unlp.edu.ar:10915/83524Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:15:41.98SEDICI (UNLP) - Universidad Nacional de La Platafalse |
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 Ciencias Astronómicas Galaxy: evolution Galaxy: stellar content Galaxy: structure |
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 Vázquez, Rubén Ángel |
author |
Carraro, Giovanni |
author_facet |
Carraro, Giovanni Moitinho, André Vázquez, Rubén Ángel |
author_role |
author |
author2 |
Moitinho, André Vázquez, Rubén Ángel |
author2_role |
author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Galaxy: evolution Galaxy: stellar content Galaxy: structure |
topic |
Ciencias Astronómicas Galaxy: evolution Galaxy: stellar content Galaxy: structure |
dc.description.none.fl_txt_mv |
We performed a photometric multicolour survey of the core of the Canis Major overdensity at l ≈ 244°, b ≈ —8°.0, reaching V ~ 22 and covering 0.3 x 1.0 arcmin2. 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 centred on the Canis Major overdensity. A large wavelength baseline, in the UBVRI 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 modelling. In agreement with our previous studies, in the same general region ofthe Milky Way, we recognize a young stellar population compatible with the expected structure and extension of the Local (Orion) and Outer (NormaCygnus) spiral arms in the Third Galactic Quadrant. Moreover, we interpret the conspicuous intermediate-age metal-poor population as belonging to the Galactic thick disc, distorted by the effect of strong disc warping at this latitude, and to the Galactic halo. Facultad de Ciencias Astronómicas y Geofísicas |
description |
We performed a photometric multicolour survey of the core of the Canis Major overdensity at l ≈ 244°, b ≈ —8°.0, reaching V ~ 22 and covering 0.3 x 1.0 arcmin2. 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 centred on the Canis Major overdensity. A large wavelength baseline, in the UBVRI 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 modelling. In agreement with our previous studies, in the same general region ofthe Milky Way, we recognize a young stellar population compatible with the expected structure and extension of the Local (Orion) and Outer (NormaCygnus) spiral arms in the Third Galactic Quadrant. Moreover, we interpret the conspicuous intermediate-age metal-poor population as belonging to the Galactic thick disc, distorted by the effect of strong disc warping at this latitude, and to the Galactic halo. |
publishDate |
2008 |
dc.date.none.fl_str_mv |
2008 |
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/10915/83524 |
url |
http://sedici.unlp.edu.ar/handle/10915/83524 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/0035-8711 info:eu-repo/semantics/altIdentifier/doi/10.1111/j.1365-2966.2008.12953.x |
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 1597-1604 |
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_ |
1844616029255237632 |
score |
13.070432 |