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
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/85526

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/85526
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repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling 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/doi/10.1051/0004-6361/201220743
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
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Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
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rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
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