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
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/233505
Acceder
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oai_identifier_str oai:ri.conicet.gov.ar:11336/233505
network_acronym_str CONICETDig
repository_id_str 3498
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 Técnicas2025-10-22T12:14:27Zoai: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:34982025-10-22 12:14:27.573CONICET 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
_version_ 1846782552324440064
score 12.982451

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