Photometric study of the young open cluster NGC 3293
- Autores
- Baume, Gustavo Luis; Vázquez, Rubén Ángel; Carraro, G.; Feinstein, Alejandro
- Año de publicación
- 2003
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Deep and extensive CCD photometric observations at UBV(RI)cHα were carried out in the area of the open cluster NGC 3293. The new data set allows to see the entire cluster sequence down to Mv ≈ +4.5, revealing that stars with Mv < -2 are evolving off the main sequence; stars with -2 < Mv < +2 are located on the main sequence and stars with Mv > +2 are placed above it. According to our analysis, the cluster distance is d = 2750 ± 250 pc (V0 - Mv = 12.2 ± 0.2) and its nuclear age is 8 ± 1 Myr. NGC 3293 contains an important fraction of pre-main sequence (PMS) stars distributed along a parallel band to the ZAMS with masses from 1 to 2.5 M⊙ and a mean contraction age of 10 Myr. This last value does not differ too much from the nuclear age estimate. If we take into account the many factors that may affect the PMS star positions on the colour-magnitude diagram, both ages can be perfectly reconciled. The star formation rate, on the other hand, suggests that NGC 3293 stars formed surely in one single event, therefore favouring a coeval process of star formation. Using the Hα data, we detected nineteen stars with signs of Hα emission in the region of NGC 3293, another indication that the star formation process is still active in the region. The computed initial mass function for the cluster has a slope of x = 1.2 ± 0.2. a bit flatter than the typical slope for field stars and similar to the values found for other young open clusters.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Galaxy: open clusters and associations: individual: NGC 3293
Stars: imaging
Stars: luminosity function, mass function - 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:10915/84700
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Photometric study of the young open cluster NGC 3293Baume, Gustavo LuisVázquez, Rubén ÁngelCarraro, G.Feinstein, AlejandroCiencias AstronómicasGalaxy: open clusters and associations: individual: NGC 3293Stars: imagingStars: luminosity function, mass functionDeep and extensive CCD photometric observations at UBV(RI)cHα were carried out in the area of the open cluster NGC 3293. The new data set allows to see the entire cluster sequence down to Mv ≈ +4.5, revealing that stars with Mv < -2 are evolving off the main sequence; stars with -2 < Mv < +2 are located on the main sequence and stars with Mv > +2 are placed above it. According to our analysis, the cluster distance is d = 2750 ± 250 pc (V0 - Mv = 12.2 ± 0.2) and its nuclear age is 8 ± 1 Myr. NGC 3293 contains an important fraction of pre-main sequence (PMS) stars distributed along a parallel band to the ZAMS with masses from 1 to 2.5 M⊙ and a mean contraction age of 10 Myr. This last value does not differ too much from the nuclear age estimate. If we take into account the many factors that may affect the PMS star positions on the colour-magnitude diagram, both ages can be perfectly reconciled. The star formation rate, on the other hand, suggests that NGC 3293 stars formed surely in one single event, therefore favouring a coeval process of star formation. Using the Hα data, we detected nineteen stars with signs of Hα emission in the region of NGC 3293, another indication that the star formation process is still active in the region. The computed initial mass function for the cluster has a slope of x = 1.2 ± 0.2. a bit flatter than the typical slope for field stars and similar to the values found for other young open clusters.Facultad de Ciencias Astronómicas y Geofísicas2003info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf549-564http://sedici.unlp.edu.ar/handle/10915/84700enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20030223info: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:UNLP2025-09-29T11:16:15Zoai:sedici.unlp.edu.ar:10915/84700Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:16.211SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Photometric study of the young open cluster NGC 3293 |
title |
Photometric study of the young open cluster NGC 3293 |
spellingShingle |
Photometric study of the young open cluster NGC 3293 Baume, Gustavo Luis Ciencias Astronómicas Galaxy: open clusters and associations: individual: NGC 3293 Stars: imaging Stars: luminosity function, mass function |
title_short |
Photometric study of the young open cluster NGC 3293 |
title_full |
Photometric study of the young open cluster NGC 3293 |
title_fullStr |
Photometric study of the young open cluster NGC 3293 |
title_full_unstemmed |
Photometric study of the young open cluster NGC 3293 |
title_sort |
Photometric study of the young open cluster NGC 3293 |
dc.creator.none.fl_str_mv |
Baume, Gustavo Luis Vázquez, Rubén Ángel Carraro, G. Feinstein, Alejandro |
author |
Baume, Gustavo Luis |
author_facet |
Baume, Gustavo Luis Vázquez, Rubén Ángel Carraro, G. Feinstein, Alejandro |
author_role |
author |
author2 |
Vázquez, Rubén Ángel Carraro, G. Feinstein, Alejandro |
author2_role |
author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Galaxy: open clusters and associations: individual: NGC 3293 Stars: imaging Stars: luminosity function, mass function |
topic |
Ciencias Astronómicas Galaxy: open clusters and associations: individual: NGC 3293 Stars: imaging Stars: luminosity function, mass function |
dc.description.none.fl_txt_mv |
Deep and extensive CCD photometric observations at UBV(RI)cHα were carried out in the area of the open cluster NGC 3293. The new data set allows to see the entire cluster sequence down to Mv ≈ +4.5, revealing that stars with Mv < -2 are evolving off the main sequence; stars with -2 < Mv < +2 are located on the main sequence and stars with Mv > +2 are placed above it. According to our analysis, the cluster distance is d = 2750 ± 250 pc (V0 - Mv = 12.2 ± 0.2) and its nuclear age is 8 ± 1 Myr. NGC 3293 contains an important fraction of pre-main sequence (PMS) stars distributed along a parallel band to the ZAMS with masses from 1 to 2.5 M⊙ and a mean contraction age of 10 Myr. This last value does not differ too much from the nuclear age estimate. If we take into account the many factors that may affect the PMS star positions on the colour-magnitude diagram, both ages can be perfectly reconciled. The star formation rate, on the other hand, suggests that NGC 3293 stars formed surely in one single event, therefore favouring a coeval process of star formation. Using the Hα data, we detected nineteen stars with signs of Hα emission in the region of NGC 3293, another indication that the star formation process is still active in the region. The computed initial mass function for the cluster has a slope of x = 1.2 ± 0.2. a bit flatter than the typical slope for field stars and similar to the values found for other young open clusters. Facultad de Ciencias Astronómicas y Geofísicas |
description |
Deep and extensive CCD photometric observations at UBV(RI)cHα were carried out in the area of the open cluster NGC 3293. The new data set allows to see the entire cluster sequence down to Mv ≈ +4.5, revealing that stars with Mv < -2 are evolving off the main sequence; stars with -2 < Mv < +2 are located on the main sequence and stars with Mv > +2 are placed above it. According to our analysis, the cluster distance is d = 2750 ± 250 pc (V0 - Mv = 12.2 ± 0.2) and its nuclear age is 8 ± 1 Myr. NGC 3293 contains an important fraction of pre-main sequence (PMS) stars distributed along a parallel band to the ZAMS with masses from 1 to 2.5 M⊙ and a mean contraction age of 10 Myr. This last value does not differ too much from the nuclear age estimate. If we take into account the many factors that may affect the PMS star positions on the colour-magnitude diagram, both ages can be perfectly reconciled. The star formation rate, on the other hand, suggests that NGC 3293 stars formed surely in one single event, therefore favouring a coeval process of star formation. Using the Hα data, we detected nineteen stars with signs of Hα emission in the region of NGC 3293, another indication that the star formation process is still active in the region. The computed initial mass function for the cluster has a slope of x = 1.2 ± 0.2. a bit flatter than the typical slope for field stars and similar to the values found for other young open clusters. |
publishDate |
2003 |
dc.date.none.fl_str_mv |
2003 |
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/10915/84700 |
url |
http://sedici.unlp.edu.ar/handle/10915/84700 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/0004-6361 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361:20030223 |
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 |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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application/pdf 549-564 |
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