NGC 2849 and NGC 6134: two more BOCCE open clusters
- Autores
- Ahumada, Andrea Veronica; Cignoni, M.; Bragaglia, A.; Donati, P.; Tosi, M.; Marconi, G.
- Año de publicación
- 2013
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present CCD photometry of two southern open clusters. As part of the Bologna Open Cluster Chemical Evolution project we obtained BVI and UBVI imaging for NGC 2849 and NGC 6134, respectively. By means of the synthetic colour-magnitude diagram method and using various evolutionary sets of stellar evolution tracks with various metallicities, we determined at the same time age, distance and reddening. We also determined an approximate metallicity for NGC 2849, for which the information is not available from sounder methods like high-resolution spectroscopy. NGC 2849 turned to be 0.85-1.0 Gyr old with a solar metallicity. The foreground reddening is E(B - V) = 0.28 - 0.32, and the true distance modulus (m - M) 0 = 13.8-13.9. For NGC 6134 we did not obtain fully consistent answers from the V, B - V and V, V - I photometry, an unexpected problem, since both the metallicity and the reddening are known (from high-resolution spectroscopy and the U - B, B - V two colours diagram, respectively). This may either indicate a difficulty of current models (evolutionary tracks and/or models of atmosphere) to accurately reproduce colours, or be related to differences in the metal mixture assumed by the models and those of the clusters. Assuming the spectroscopic abundance and the colour excess [E(B - V) = 0.35] from the U - B, B - V plot, we derived a best age between 0.82 and 0.95 Gyr and a distance modulus 10.5. In agreement with previous studies, the NGC 6134 colour-magnitude diagram shows also a clear main sequence gap at V ˜ 15 and B-V ˜ 0.9-1.0 that is unexplained by canonical stellar evolution models.
Fil: Ahumada, Andrea Veronica. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina
Fil: Cignoni, M.. Universitá di Bologna. Dipartimento di Astronomia; Italia;
Fil: Bragaglia, A.. INAF-Osservatorio Astronomico di Bologna; Italia;
Fil: Donati, P.. Universitá di Bologna. Dipartimento di Astronomia; Italia;
Fil: Tosi, M.. INAF-Osservatorio Astronomico di Bologna; Italia;
Fil: Marconi, G.. European Southern Observatory (ESO); Chile; - Materia
-
STELLAR CLUSTERS
CMD - 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:11336/2500
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NGC 2849 and NGC 6134: two more BOCCE open clustersAhumada, Andrea VeronicaCignoni, M.Bragaglia, A.Donati, P.Tosi, M.Marconi, G.STELLAR CLUSTERSCMDWe present CCD photometry of two southern open clusters. As part of the Bologna Open Cluster Chemical Evolution project we obtained BVI and UBVI imaging for NGC 2849 and NGC 6134, respectively. By means of the synthetic colour-magnitude diagram method and using various evolutionary sets of stellar evolution tracks with various metallicities, we determined at the same time age, distance and reddening. We also determined an approximate metallicity for NGC 2849, for which the information is not available from sounder methods like high-resolution spectroscopy. NGC 2849 turned to be 0.85-1.0 Gyr old with a solar metallicity. The foreground reddening is E(B - V) = 0.28 - 0.32, and the true distance modulus (m - M) 0 = 13.8-13.9. For NGC 6134 we did not obtain fully consistent answers from the V, B - V and V, V - I photometry, an unexpected problem, since both the metallicity and the reddening are known (from high-resolution spectroscopy and the U - B, B - V two colours diagram, respectively). This may either indicate a difficulty of current models (evolutionary tracks and/or models of atmosphere) to accurately reproduce colours, or be related to differences in the metal mixture assumed by the models and those of the clusters. Assuming the spectroscopic abundance and the colour excess [E(B - V) = 0.35] from the U - B, B - V plot, we derived a best age between 0.82 and 0.95 Gyr and a distance modulus 10.5. In agreement with previous studies, the NGC 6134 colour-magnitude diagram shows also a clear main sequence gap at V ˜ 15 and B-V ˜ 0.9-1.0 that is unexplained by canonical stellar evolution models.Fil: Ahumada, Andrea Veronica. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; ArgentinaFil: Cignoni, M.. Universitá di Bologna. Dipartimento di Astronomia; Italia;Fil: Bragaglia, A.. INAF-Osservatorio Astronomico di Bologna; Italia;Fil: Donati, P.. Universitá di Bologna. Dipartimento di Astronomia; Italia;Fil: Tosi, M.. INAF-Osservatorio Astronomico di Bologna; Italia;Fil: Marconi, G.. European Southern Observatory (ESO); Chile;Wiley-blackwell Publishing, Inc2013-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/2500Ahumada, Andrea Veronica; Cignoni, M.; Bragaglia, A.; Donati, P.; Tosi, M.; et al.; NGC 2849 and NGC 6134: two more BOCCE open clusters; Wiley-blackwell Publishing, Inc; Monthly Notices Of The Royal Astronomical Society; 430; 3-2013; 221-2330035-8711enginfo:eu-repo/semantics/altIdentifier/url/http://mnras.oxfordjournals.org/content/430/1/221.abstractinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:01:36Zoai:ri.conicet.gov.ar:11336/2500instacron: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 10:01:36.843CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
NGC 2849 and NGC 6134: two more BOCCE open clusters |
title |
NGC 2849 and NGC 6134: two more BOCCE open clusters |
spellingShingle |
NGC 2849 and NGC 6134: two more BOCCE open clusters Ahumada, Andrea Veronica STELLAR CLUSTERS CMD |
title_short |
NGC 2849 and NGC 6134: two more BOCCE open clusters |
title_full |
NGC 2849 and NGC 6134: two more BOCCE open clusters |
title_fullStr |
NGC 2849 and NGC 6134: two more BOCCE open clusters |
title_full_unstemmed |
NGC 2849 and NGC 6134: two more BOCCE open clusters |
title_sort |
NGC 2849 and NGC 6134: two more BOCCE open clusters |
dc.creator.none.fl_str_mv |
Ahumada, Andrea Veronica Cignoni, M. Bragaglia, A. Donati, P. Tosi, M. Marconi, G. |
author |
Ahumada, Andrea Veronica |
author_facet |
Ahumada, Andrea Veronica Cignoni, M. Bragaglia, A. Donati, P. Tosi, M. Marconi, G. |
author_role |
author |
author2 |
Cignoni, M. Bragaglia, A. Donati, P. Tosi, M. Marconi, G. |
author2_role |
author author author author author |
dc.subject.none.fl_str_mv |
STELLAR CLUSTERS CMD |
topic |
STELLAR CLUSTERS CMD |
dc.description.none.fl_txt_mv |
We present CCD photometry of two southern open clusters. As part of the Bologna Open Cluster Chemical Evolution project we obtained BVI and UBVI imaging for NGC 2849 and NGC 6134, respectively. By means of the synthetic colour-magnitude diagram method and using various evolutionary sets of stellar evolution tracks with various metallicities, we determined at the same time age, distance and reddening. We also determined an approximate metallicity for NGC 2849, for which the information is not available from sounder methods like high-resolution spectroscopy. NGC 2849 turned to be 0.85-1.0 Gyr old with a solar metallicity. The foreground reddening is E(B - V) = 0.28 - 0.32, and the true distance modulus (m - M) 0 = 13.8-13.9. For NGC 6134 we did not obtain fully consistent answers from the V, B - V and V, V - I photometry, an unexpected problem, since both the metallicity and the reddening are known (from high-resolution spectroscopy and the U - B, B - V two colours diagram, respectively). This may either indicate a difficulty of current models (evolutionary tracks and/or models of atmosphere) to accurately reproduce colours, or be related to differences in the metal mixture assumed by the models and those of the clusters. Assuming the spectroscopic abundance and the colour excess [E(B - V) = 0.35] from the U - B, B - V plot, we derived a best age between 0.82 and 0.95 Gyr and a distance modulus 10.5. In agreement with previous studies, the NGC 6134 colour-magnitude diagram shows also a clear main sequence gap at V ˜ 15 and B-V ˜ 0.9-1.0 that is unexplained by canonical stellar evolution models. Fil: Ahumada, Andrea Veronica. Consejo Nacional de Investigaciones Científicas y Técnicas; Argentina. Universidad Nacional de Cordoba. Observatorio Astronomico de Cordoba. Departamento de Astrofisica Estelar; Argentina Fil: Cignoni, M.. Universitá di Bologna. Dipartimento di Astronomia; Italia; Fil: Bragaglia, A.. INAF-Osservatorio Astronomico di Bologna; Italia; Fil: Donati, P.. Universitá di Bologna. Dipartimento di Astronomia; Italia; Fil: Tosi, M.. INAF-Osservatorio Astronomico di Bologna; Italia; Fil: Marconi, G.. European Southern Observatory (ESO); Chile; |
description |
We present CCD photometry of two southern open clusters. As part of the Bologna Open Cluster Chemical Evolution project we obtained BVI and UBVI imaging for NGC 2849 and NGC 6134, respectively. By means of the synthetic colour-magnitude diagram method and using various evolutionary sets of stellar evolution tracks with various metallicities, we determined at the same time age, distance and reddening. We also determined an approximate metallicity for NGC 2849, for which the information is not available from sounder methods like high-resolution spectroscopy. NGC 2849 turned to be 0.85-1.0 Gyr old with a solar metallicity. The foreground reddening is E(B - V) = 0.28 - 0.32, and the true distance modulus (m - M) 0 = 13.8-13.9. For NGC 6134 we did not obtain fully consistent answers from the V, B - V and V, V - I photometry, an unexpected problem, since both the metallicity and the reddening are known (from high-resolution spectroscopy and the U - B, B - V two colours diagram, respectively). This may either indicate a difficulty of current models (evolutionary tracks and/or models of atmosphere) to accurately reproduce colours, or be related to differences in the metal mixture assumed by the models and those of the clusters. Assuming the spectroscopic abundance and the colour excess [E(B - V) = 0.35] from the U - B, B - V plot, we derived a best age between 0.82 and 0.95 Gyr and a distance modulus 10.5. In agreement with previous studies, the NGC 6134 colour-magnitude diagram shows also a clear main sequence gap at V ˜ 15 and B-V ˜ 0.9-1.0 that is unexplained by canonical stellar evolution models. |
publishDate |
2013 |
dc.date.none.fl_str_mv |
2013-03 |
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/11336/2500 Ahumada, Andrea Veronica; Cignoni, M.; Bragaglia, A.; Donati, P.; Tosi, M.; et al.; NGC 2849 and NGC 6134: two more BOCCE open clusters; Wiley-blackwell Publishing, Inc; Monthly Notices Of The Royal Astronomical Society; 430; 3-2013; 221-233 0035-8711 |
url |
http://hdl.handle.net/11336/2500 |
identifier_str_mv |
Ahumada, Andrea Veronica; Cignoni, M.; Bragaglia, A.; Donati, P.; Tosi, M.; et al.; NGC 2849 and NGC 6134: two more BOCCE open clusters; Wiley-blackwell Publishing, Inc; Monthly Notices Of The Royal Astronomical Society; 430; 3-2013; 221-233 0035-8711 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/url/http://mnras.oxfordjournals.org/content/430/1/221.abstract |
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 |
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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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1844613811738247168 |
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13.070432 |