Polarimetry in the outskirts of NGC 6611

Autores
Orsatti, Ana María; Vega, Ema Irene; Marraco, Hugo Gustavo
Año de publicación
2006
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We present new polarimetric UBVRI observations of 25 stars in the direction of the halo of NGC 6611, the rich stellar open cluster embedded in an ionized hydrogen complex (M16). Our plan is to characterize the interstellar material (ISM) associated with halo stars in order to make a comparison with the ISM dusty core characteristics that resulted from a previous investigation by the same authors. Of the halo stars, 47% (8 out of 17) show indications of intrinsic polarization in their light, similar to what was found for core stars (50%). We have identified the presence of nearby dust clouds located on the Local arm that produce a mean polarization of about 1%; a value λmax = 0.61 ± 0.07 μm, which is slightly larger than that of the average ISM; and a mean direction of the polarization vectors of θV = 81.°9 ± 1.°8. The ISM associated with the halo region has λmax similar to the general interstellar medium (0.55 ± 0.07 μm). The observed polarizations show a gradual increase from halo (Pmax = 1.93% ± 0.3%) to core (Pmax = 3.19% ± 0.63%). Position angles of the e-vector for both groups are generally similar, but there exists a slight difference in mean direction between them that is within the errors. We have also found that the halo stars are possibly represented by Whittet & van Breda's relationship, while in the cluster's core the dust does not fulfill the above-mentioned relationship. As a conclusion, we cannot find any clear difference between core and halo dust characteristics, with the exception of λmax, which may suggest a change in dust size.
Facultad de Ciencias Astronómicas y Geofísicas
Materia
Ciencias Astronómicas
Dust, extinction
Open clusters and associations: individual (NGC 6611)
Techniques: polarimetric Online material: machine-readable table
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:10915/83135

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/83135
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Polarimetry in the outskirts of NGC 6611Orsatti, Ana MaríaVega, Ema IreneMarraco, Hugo GustavoCiencias AstronómicasDust, extinctionOpen clusters and associations: individual (NGC 6611)Techniques: polarimetric Online material: machine-readable tableWe present new polarimetric UBVRI observations of 25 stars in the direction of the halo of NGC 6611, the rich stellar open cluster embedded in an ionized hydrogen complex (M16). Our plan is to characterize the interstellar material (ISM) associated with halo stars in order to make a comparison with the ISM dusty core characteristics that resulted from a previous investigation by the same authors. Of the halo stars, 47% (8 out of 17) show indications of intrinsic polarization in their light, similar to what was found for core stars (50%). We have identified the presence of nearby dust clouds located on the Local arm that produce a mean polarization of about 1%; a value λmax = 0.61 ± 0.07 μm, which is slightly larger than that of the average ISM; and a mean direction of the polarization vectors of θV = 81.°9 ± 1.°8. The ISM associated with the halo region has λmax similar to the general interstellar medium (0.55 ± 0.07 μm). The observed polarizations show a gradual increase from halo (Pmax = 1.93% ± 0.3%) to core (Pmax = 3.19% ± 0.63%). Position angles of the e-vector for both groups are generally similar, but there exists a slight difference in mean direction between them that is within the errors. We have also found that the halo stars are possibly represented by Whittet & van Breda's relationship, while in the cluster's core the dust does not fulfill the above-mentioned relationship. As a conclusion, we cannot find any clear difference between core and halo dust characteristics, with the exception of λmax, which may suggest a change in dust size.Facultad de Ciencias Astronómicas y Geofísicas2006-10-28info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf1783-1788http://sedici.unlp.edu.ar/handle/10915/83135enginfo:eu-repo/semantics/altIdentifier/issn/0004-6256info:eu-repo/semantics/altIdentifier/doi/10.1086/507674info: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:UNLP2025-09-29T11:15:45Zoai:sedici.unlp.edu.ar:10915/83135Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:15:45.989SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Polarimetry in the outskirts of NGC 6611
title Polarimetry in the outskirts of NGC 6611
spellingShingle Polarimetry in the outskirts of NGC 6611
Orsatti, Ana María
Ciencias Astronómicas
Dust, extinction
Open clusters and associations: individual (NGC 6611)
Techniques: polarimetric Online material: machine-readable table
title_short Polarimetry in the outskirts of NGC 6611
title_full Polarimetry in the outskirts of NGC 6611
title_fullStr Polarimetry in the outskirts of NGC 6611
title_full_unstemmed Polarimetry in the outskirts of NGC 6611
title_sort Polarimetry in the outskirts of NGC 6611
dc.creator.none.fl_str_mv Orsatti, Ana María
Vega, Ema Irene
Marraco, Hugo Gustavo
author Orsatti, Ana María
author_facet Orsatti, Ana María
Vega, Ema Irene
Marraco, Hugo Gustavo
author_role author
author2 Vega, Ema Irene
Marraco, Hugo Gustavo
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
Dust, extinction
Open clusters and associations: individual (NGC 6611)
Techniques: polarimetric Online material: machine-readable table
topic Ciencias Astronómicas
Dust, extinction
Open clusters and associations: individual (NGC 6611)
Techniques: polarimetric Online material: machine-readable table
dc.description.none.fl_txt_mv We present new polarimetric UBVRI observations of 25 stars in the direction of the halo of NGC 6611, the rich stellar open cluster embedded in an ionized hydrogen complex (M16). Our plan is to characterize the interstellar material (ISM) associated with halo stars in order to make a comparison with the ISM dusty core characteristics that resulted from a previous investigation by the same authors. Of the halo stars, 47% (8 out of 17) show indications of intrinsic polarization in their light, similar to what was found for core stars (50%). We have identified the presence of nearby dust clouds located on the Local arm that produce a mean polarization of about 1%; a value λmax = 0.61 ± 0.07 μm, which is slightly larger than that of the average ISM; and a mean direction of the polarization vectors of θV = 81.°9 ± 1.°8. The ISM associated with the halo region has λmax similar to the general interstellar medium (0.55 ± 0.07 μm). The observed polarizations show a gradual increase from halo (Pmax = 1.93% ± 0.3%) to core (Pmax = 3.19% ± 0.63%). Position angles of the e-vector for both groups are generally similar, but there exists a slight difference in mean direction between them that is within the errors. We have also found that the halo stars are possibly represented by Whittet & van Breda's relationship, while in the cluster's core the dust does not fulfill the above-mentioned relationship. As a conclusion, we cannot find any clear difference between core and halo dust characteristics, with the exception of λmax, which may suggest a change in dust size.
Facultad de Ciencias Astronómicas y Geofísicas
description We present new polarimetric UBVRI observations of 25 stars in the direction of the halo of NGC 6611, the rich stellar open cluster embedded in an ionized hydrogen complex (M16). Our plan is to characterize the interstellar material (ISM) associated with halo stars in order to make a comparison with the ISM dusty core characteristics that resulted from a previous investigation by the same authors. Of the halo stars, 47% (8 out of 17) show indications of intrinsic polarization in their light, similar to what was found for core stars (50%). We have identified the presence of nearby dust clouds located on the Local arm that produce a mean polarization of about 1%; a value λmax = 0.61 ± 0.07 μm, which is slightly larger than that of the average ISM; and a mean direction of the polarization vectors of θV = 81.°9 ± 1.°8. The ISM associated with the halo region has λmax similar to the general interstellar medium (0.55 ± 0.07 μm). The observed polarizations show a gradual increase from halo (Pmax = 1.93% ± 0.3%) to core (Pmax = 3.19% ± 0.63%). Position angles of the e-vector for both groups are generally similar, but there exists a slight difference in mean direction between them that is within the errors. We have also found that the halo stars are possibly represented by Whittet & van Breda's relationship, while in the cluster's core the dust does not fulfill the above-mentioned relationship. As a conclusion, we cannot find any clear difference between core and halo dust characteristics, with the exception of λmax, which may suggest a change in dust size.
publishDate 2006
dc.date.none.fl_str_mv 2006-10-28
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/10915/83135
url http://sedici.unlp.edu.ar/handle/10915/83135
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6256
info:eu-repo/semantics/altIdentifier/doi/10.1086/507674
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
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
1783-1788
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
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instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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