Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies
- Autores
- Corti, Mariela Alejandra; Orellana, Rosa Beatriz
- Año de publicación
- 2013
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. An OB association is a gravitationally unbound group of stars. The identification of the members of the association is an important aspect of its study. There are few astrometric membership studies for OB associations, but the combination of these studies with astrophysical techniques becomes a very powerful tool for this type of research. Aims. We perform new spectroscopic and astrometric studies of the members of the association Centaurus OB1 (Cen OB1) and the open cluster NGC 4755. Methods. To carry out this study we used new spectroscopic optical observations obtained at CASLEO, and proper motion and photometric data from the Tycho-2 Catalogue and other databases available via the Internet. Results. With this investigation we found 52 members of Cen OB1 (l = 303º.7, b = 0º.4) and four members of NGC 4755 (l = 303º.2, b = 2º.5), an open cluster integrated into the Cen OB1 stellar association. The distance, heliocentric radial velocity, proper motion, and age of Cen OB1 are 2.6 ± 0.5 kpc, ~-20 km s-1, μαcosδ = -4.78 ± 0.10 mas yr-1, μδ = -0.93 ± 0.10 mas yr-1, and ~20 × 106 years old, respectively. The same parameters found for NGC 4755 are 1.9 ± 0.5 kpc, -18 ± 2 km s-1, μαcosδ = -4.14 ± 0.19 mas yr-1, μδ = -1.09 ± 0.12 mas yr-1, and ~15 × 106 years old. The pulsars PSR J1253-5820 and PSR J1254-6150 could have been born as the result of supernovae explosions that occurred in the past by massive members of Cen OB1. We have seen Infrared Astronomical Satellite (IRAS) sources near Cen OB1, that show that star formation is still occurring. The age gradient observed between the different members of Cen OB1 makes it likely that the stellar association and IRAS sources represent different stages of a sequential formation process.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
Open clusters and associations: individual: Centaurus OB1
Open clusters and associations: individual: NGC 4755
Proper motions
Stars: early-type - 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:10915/85526
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Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studiesCorti, Mariela AlejandraOrellana, Rosa BeatrizCiencias AstronómicasOpen clusters and associations: individual: Centaurus OB1Open clusters and associations: individual: NGC 4755Proper motionsStars: early-typeContext. An OB association is a gravitationally unbound group of stars. The identification of the members of the association is an important aspect of its study. There are few astrometric membership studies for OB associations, but the combination of these studies with astrophysical techniques becomes a very powerful tool for this type of research. Aims. We perform new spectroscopic and astrometric studies of the members of the association Centaurus OB1 (Cen OB1) and the open cluster NGC 4755. Methods. To carry out this study we used new spectroscopic optical observations obtained at CASLEO, and proper motion and photometric data from the Tycho-2 Catalogue and other databases available via the Internet. Results. With this investigation we found 52 members of Cen OB1 (l = 303º.7, b = 0º.4) and four members of NGC 4755 (l = 303º.2, b = 2º.5), an open cluster integrated into the Cen OB1 stellar association. The distance, heliocentric radial velocity, proper motion, and age of Cen OB1 are 2.6 ± 0.5 kpc, ~-20 km s<SUP>-1</SUP>, μ<SUB>α</SUB>cosδ = -4.78 ± 0.10 mas yr<SUP>-1</SUP>, μ<SUB>δ</SUB> = -0.93 ± 0.10 mas yr<SUP>-1</SUP>, and ~20 × 10<SUP>6</SUP> years old, respectively. The same parameters found for NGC 4755 are 1.9 ± 0.5 kpc, -18 ± 2 km s<SUP>-1</SUP>, μ<SUB>α</SUB>cosδ = -4.14 ± 0.19 mas yr<SUP>-1</SUP>, μ<SUB>δ</SUB> = -1.09 ± 0.12 mas yr<SUP>-1</SUP>, and ~15 × 10<SUP>6</SUP> years old. The pulsars PSR J1253-5820 and PSR J1254-6150 could have been born as the result of supernovae explosions that occurred in the past by massive members of Cen OB1. We have seen Infrared Astronomical Satellite (IRAS) sources near Cen OB1, that show that star formation is still occurring. The age gradient observed between the different members of Cen OB1 makes it likely that the stellar association and IRAS sources represent different stages of a sequential formation process.Facultad de Ciencias Astronómicas y GeofísicasInstituto Argentino de RadioastronomíaInstituto de Astrofísica de La Plata2013info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/85526enginfo:eu-repo/semantics/altIdentifier/issn/0004-6361info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201220743info: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:UNLP2025-09-29T11:16:30Zoai:sedici.unlp.edu.ar:10915/85526Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:31.019SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies |
title |
Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies |
spellingShingle |
Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies Corti, Mariela Alejandra Ciencias Astronómicas Open clusters and associations: individual: Centaurus OB1 Open clusters and associations: individual: NGC 4755 Proper motions Stars: early-type |
title_short |
Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies |
title_full |
Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies |
title_fullStr |
Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies |
title_full_unstemmed |
Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies |
title_sort |
Members of Centaurus OB1 and NGC 4755: new spectroscopic and astrometric studies |
dc.creator.none.fl_str_mv |
Corti, Mariela Alejandra Orellana, Rosa Beatriz |
author |
Corti, Mariela Alejandra |
author_facet |
Corti, Mariela Alejandra Orellana, Rosa Beatriz |
author_role |
author |
author2 |
Orellana, Rosa Beatriz |
author2_role |
author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Open clusters and associations: individual: Centaurus OB1 Open clusters and associations: individual: NGC 4755 Proper motions Stars: early-type |
topic |
Ciencias Astronómicas Open clusters and associations: individual: Centaurus OB1 Open clusters and associations: individual: NGC 4755 Proper motions Stars: early-type |
dc.description.none.fl_txt_mv |
Context. An OB association is a gravitationally unbound group of stars. The identification of the members of the association is an important aspect of its study. There are few astrometric membership studies for OB associations, but the combination of these studies with astrophysical techniques becomes a very powerful tool for this type of research. Aims. We perform new spectroscopic and astrometric studies of the members of the association Centaurus OB1 (Cen OB1) and the open cluster NGC 4755. Methods. To carry out this study we used new spectroscopic optical observations obtained at CASLEO, and proper motion and photometric data from the Tycho-2 Catalogue and other databases available via the Internet. Results. With this investigation we found 52 members of Cen OB1 (l = 303º.7, b = 0º.4) and four members of NGC 4755 (l = 303º.2, b = 2º.5), an open cluster integrated into the Cen OB1 stellar association. The distance, heliocentric radial velocity, proper motion, and age of Cen OB1 are 2.6 ± 0.5 kpc, ~-20 km s<SUP>-1</SUP>, μ<SUB>α</SUB>cosδ = -4.78 ± 0.10 mas yr<SUP>-1</SUP>, μ<SUB>δ</SUB> = -0.93 ± 0.10 mas yr<SUP>-1</SUP>, and ~20 × 10<SUP>6</SUP> years old, respectively. The same parameters found for NGC 4755 are 1.9 ± 0.5 kpc, -18 ± 2 km s<SUP>-1</SUP>, μ<SUB>α</SUB>cosδ = -4.14 ± 0.19 mas yr<SUP>-1</SUP>, μ<SUB>δ</SUB> = -1.09 ± 0.12 mas yr<SUP>-1</SUP>, and ~15 × 10<SUP>6</SUP> years old. The pulsars PSR J1253-5820 and PSR J1254-6150 could have been born as the result of supernovae explosions that occurred in the past by massive members of Cen OB1. We have seen Infrared Astronomical Satellite (IRAS) sources near Cen OB1, that show that star formation is still occurring. The age gradient observed between the different members of Cen OB1 makes it likely that the stellar association and IRAS sources represent different stages of a sequential formation process. Facultad de Ciencias Astronómicas y Geofísicas Instituto Argentino de Radioastronomía Instituto de Astrofísica de La Plata |
description |
Context. An OB association is a gravitationally unbound group of stars. The identification of the members of the association is an important aspect of its study. There are few astrometric membership studies for OB associations, but the combination of these studies with astrophysical techniques becomes a very powerful tool for this type of research. Aims. We perform new spectroscopic and astrometric studies of the members of the association Centaurus OB1 (Cen OB1) and the open cluster NGC 4755. Methods. To carry out this study we used new spectroscopic optical observations obtained at CASLEO, and proper motion and photometric data from the Tycho-2 Catalogue and other databases available via the Internet. Results. With this investigation we found 52 members of Cen OB1 (l = 303º.7, b = 0º.4) and four members of NGC 4755 (l = 303º.2, b = 2º.5), an open cluster integrated into the Cen OB1 stellar association. The distance, heliocentric radial velocity, proper motion, and age of Cen OB1 are 2.6 ± 0.5 kpc, ~-20 km s<SUP>-1</SUP>, μ<SUB>α</SUB>cosδ = -4.78 ± 0.10 mas yr<SUP>-1</SUP>, μ<SUB>δ</SUB> = -0.93 ± 0.10 mas yr<SUP>-1</SUP>, and ~20 × 10<SUP>6</SUP> years old, respectively. The same parameters found for NGC 4755 are 1.9 ± 0.5 kpc, -18 ± 2 km s<SUP>-1</SUP>, μ<SUB>α</SUB>cosδ = -4.14 ± 0.19 mas yr<SUP>-1</SUP>, μ<SUB>δ</SUB> = -1.09 ± 0.12 mas yr<SUP>-1</SUP>, and ~15 × 10<SUP>6</SUP> years old. The pulsars PSR J1253-5820 and PSR J1254-6150 could have been born as the result of supernovae explosions that occurred in the past by massive members of Cen OB1. We have seen Infrared Astronomical Satellite (IRAS) sources near Cen OB1, that show that star formation is still occurring. The age gradient observed between the different members of Cen OB1 makes it likely that the stellar association and IRAS sources represent different stages of a sequential formation process. |
publishDate |
2013 |
dc.date.none.fl_str_mv |
2013 |
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info:eu-repo/semantics/altIdentifier/issn/0004-6361 info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201220743 |
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