Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines
- Autores
- Aidelman, Yael Judith; Cidale, Lydia Sonia
- Año de publicación
- 2023
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- The emission-line B-type stars constitute a heterogeneous group. Many of these stars show similar optical spectroscopic features and color indices, making it difficult to classify them adequately by means of photometric and spectroscopic techniques. Thus, it is relevant to deal with appropriate classification criteria to avoid as many selection effects as possible. For this purpose, we analyzed different reddening-free Q parameters, taking advantage of the Gaia and 2MASS photometric surveys, for both main sequence and emission-line B-type stars. Along with this work, we provided various criteria to search for normal and emission-line B-type stars, using different color–color, Q–color, and Q–Q diagrams. It was also possible to identify stars in different transition phases (i.e., (Formula presented.) vs. (Formula presented.) diagrams) and to classify them according to their NIR radiation excesses (i.e., the (Formula presented.) vs. (Formula presented.) diagram). Other diagrams, such as the (Formula presented.) vs. (Formula presented.) or (Formula presented.) vs. (Formula presented.), were very useful to search for and classify different classes of B-type stars with emission lines. These diagrams highlighted the presence of several stars, classified as CBe, with large color excesses that seemed to be caused by the presence of dust in their envelopes. Therefore, these stars would be misclassified. Three groups of HAeBe stars with different intrinsic dust properties were also distinguished. The amount of intrinsic dust emission in the diverse groups of emission-line stars was well-recognized via the (Formula presented.) vs. (Formula presented.) diagram. The different selection criteria are very important tools for automated designs of machine learning and optimal search algorithms.
Fil: Aidelman, Yael Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Cidale, Lydia Sonia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina - Materia
-
(STARS:) CIRCUMSTELLAR MATTER
STARS: EARLY-TYPE
STARS: EMISSION-LINE, BE
STARS: PECULIAR (EXCEPT CHEMICALLY PECULIAR) - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by/2.5/ar/
- Repositorio
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/233505
Ver los metadatos del registro completo
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oai:ri.conicet.gov.ar:11336/233505 |
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network_name_str |
CONICET Digital (CONICET) |
spelling |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission LinesAidelman, Yael JudithCidale, Lydia Sonia(STARS:) CIRCUMSTELLAR MATTERSTARS: EARLY-TYPESTARS: EMISSION-LINE, BESTARS: PECULIAR (EXCEPT CHEMICALLY PECULIAR)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1The emission-line B-type stars constitute a heterogeneous group. Many of these stars show similar optical spectroscopic features and color indices, making it difficult to classify them adequately by means of photometric and spectroscopic techniques. Thus, it is relevant to deal with appropriate classification criteria to avoid as many selection effects as possible. For this purpose, we analyzed different reddening-free Q parameters, taking advantage of the Gaia and 2MASS photometric surveys, for both main sequence and emission-line B-type stars. Along with this work, we provided various criteria to search for normal and emission-line B-type stars, using different color–color, Q–color, and Q–Q diagrams. It was also possible to identify stars in different transition phases (i.e., (Formula presented.) vs. (Formula presented.) diagrams) and to classify them according to their NIR radiation excesses (i.e., the (Formula presented.) vs. (Formula presented.) diagram). Other diagrams, such as the (Formula presented.) vs. (Formula presented.) or (Formula presented.) vs. (Formula presented.), were very useful to search for and classify different classes of B-type stars with emission lines. These diagrams highlighted the presence of several stars, classified as CBe, with large color excesses that seemed to be caused by the presence of dust in their envelopes. Therefore, these stars would be misclassified. Three groups of HAeBe stars with different intrinsic dust properties were also distinguished. The amount of intrinsic dust emission in the diverse groups of emission-line stars was well-recognized via the (Formula presented.) vs. (Formula presented.) diagram. The different selection criteria are very important tools for automated designs of machine learning and optimal search algorithms.Fil: Aidelman, Yael Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Cidale, Lydia Sonia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaMDPI2023-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/233505Aidelman, Yael Judith; Cidale, Lydia Sonia; Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines; MDPI; Galaxies; 11; 1; 2-2023; 1-222075-4434CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.3390/galaxies11010031info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:41:48Zoai:ri.conicet.gov.ar:11336/233505instacron: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 10:41:48.376CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
dc.title.none.fl_str_mv |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines |
title |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines |
spellingShingle |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines Aidelman, Yael Judith (STARS:) CIRCUMSTELLAR MATTER STARS: EARLY-TYPE STARS: EMISSION-LINE, BE STARS: PECULIAR (EXCEPT CHEMICALLY PECULIAR) |
title_short |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines |
title_full |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines |
title_fullStr |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines |
title_full_unstemmed |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines |
title_sort |
Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines |
dc.creator.none.fl_str_mv |
Aidelman, Yael Judith Cidale, Lydia Sonia |
author |
Aidelman, Yael Judith |
author_facet |
Aidelman, Yael Judith Cidale, Lydia Sonia |
author_role |
author |
author2 |
Cidale, Lydia Sonia |
author2_role |
author |
dc.subject.none.fl_str_mv |
(STARS:) CIRCUMSTELLAR MATTER STARS: EARLY-TYPE STARS: EMISSION-LINE, BE STARS: PECULIAR (EXCEPT CHEMICALLY PECULIAR) |
topic |
(STARS:) CIRCUMSTELLAR MATTER STARS: EARLY-TYPE STARS: EMISSION-LINE, BE STARS: PECULIAR (EXCEPT CHEMICALLY PECULIAR) |
purl_subject.fl_str_mv |
https://purl.org/becyt/ford/1.3 https://purl.org/becyt/ford/1 |
dc.description.none.fl_txt_mv |
The emission-line B-type stars constitute a heterogeneous group. Many of these stars show similar optical spectroscopic features and color indices, making it difficult to classify them adequately by means of photometric and spectroscopic techniques. Thus, it is relevant to deal with appropriate classification criteria to avoid as many selection effects as possible. For this purpose, we analyzed different reddening-free Q parameters, taking advantage of the Gaia and 2MASS photometric surveys, for both main sequence and emission-line B-type stars. Along with this work, we provided various criteria to search for normal and emission-line B-type stars, using different color–color, Q–color, and Q–Q diagrams. It was also possible to identify stars in different transition phases (i.e., (Formula presented.) vs. (Formula presented.) diagrams) and to classify them according to their NIR radiation excesses (i.e., the (Formula presented.) vs. (Formula presented.) diagram). Other diagrams, such as the (Formula presented.) vs. (Formula presented.) or (Formula presented.) vs. (Formula presented.), were very useful to search for and classify different classes of B-type stars with emission lines. These diagrams highlighted the presence of several stars, classified as CBe, with large color excesses that seemed to be caused by the presence of dust in their envelopes. Therefore, these stars would be misclassified. Three groups of HAeBe stars with different intrinsic dust properties were also distinguished. The amount of intrinsic dust emission in the diverse groups of emission-line stars was well-recognized via the (Formula presented.) vs. (Formula presented.) diagram. The different selection criteria are very important tools for automated designs of machine learning and optimal search algorithms. Fil: Aidelman, Yael Judith. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Cidale, Lydia Sonia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina |
description |
The emission-line B-type stars constitute a heterogeneous group. Many of these stars show similar optical spectroscopic features and color indices, making it difficult to classify them adequately by means of photometric and spectroscopic techniques. Thus, it is relevant to deal with appropriate classification criteria to avoid as many selection effects as possible. For this purpose, we analyzed different reddening-free Q parameters, taking advantage of the Gaia and 2MASS photometric surveys, for both main sequence and emission-line B-type stars. Along with this work, we provided various criteria to search for normal and emission-line B-type stars, using different color–color, Q–color, and Q–Q diagrams. It was also possible to identify stars in different transition phases (i.e., (Formula presented.) vs. (Formula presented.) diagrams) and to classify them according to their NIR radiation excesses (i.e., the (Formula presented.) vs. (Formula presented.) diagram). Other diagrams, such as the (Formula presented.) vs. (Formula presented.) or (Formula presented.) vs. (Formula presented.), were very useful to search for and classify different classes of B-type stars with emission lines. These diagrams highlighted the presence of several stars, classified as CBe, with large color excesses that seemed to be caused by the presence of dust in their envelopes. Therefore, these stars would be misclassified. Three groups of HAeBe stars with different intrinsic dust properties were also distinguished. The amount of intrinsic dust emission in the diverse groups of emission-line stars was well-recognized via the (Formula presented.) vs. (Formula presented.) diagram. The different selection criteria are very important tools for automated designs of machine learning and optimal search algorithms. |
publishDate |
2023 |
dc.date.none.fl_str_mv |
2023-02 |
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/11336/233505 Aidelman, Yael Judith; Cidale, Lydia Sonia; Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines; MDPI; Galaxies; 11; 1; 2-2023; 1-22 2075-4434 CONICET Digital CONICET |
url |
http://hdl.handle.net/11336/233505 |
identifier_str_mv |
Aidelman, Yael Judith; Cidale, Lydia Sonia; Reddening-Free Q Parameters to Classify B-Type Stars with Emission Lines; MDPI; Galaxies; 11; 1; 2-2023; 1-22 2075-4434 CONICET Digital CONICET |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.3390/galaxies11010031 |
dc.rights.none.fl_str_mv |
info:eu-repo/semantics/openAccess https://creativecommons.org/licenses/by/2.5/ar/ |
eu_rights_str_mv |
openAccess |
rights_invalid_str_mv |
https://creativecommons.org/licenses/by/2.5/ar/ |
dc.format.none.fl_str_mv |
application/pdf application/pdf |
dc.publisher.none.fl_str_mv |
MDPI |
publisher.none.fl_str_mv |
MDPI |
dc.source.none.fl_str_mv |
reponame:CONICET Digital (CONICET) instname:Consejo Nacional de Investigaciones Científicas y Técnicas |
reponame_str |
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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1844614449583882240 |
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13.070432 |