Differences between the Pallas collisional family and similarly sized B-type asteroids ?

Autores
Alí Lagoa, V.; Licandro, J.; Gil Hutton, Ricardo Alfredo; Cañada Assandri, Marcela Inés; Delbon, Marisa Ester; De León, J.; Campins, H.; Pinilla Alonso, N.; Kelley, M. S. P.; Hanus, J.
Año de publicación
2016
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Context. B-type asteroids constitute a peculiar spectral class within the C-complex. Previous work has pointed out the difference between the visible geometric albedos of B-types and those of the Pallas collisional family (PCF), whose few members with observed spectra are B-types (one exception out of eight objects). This has been interpreted as being due to compositional differences. However, the PCF members are typically smaller than the spectroscopically classified B-types, and the following possibilities have not been ruled out: the albedo differences might be related to a size-albedo dependence and/or to the generally larger errors of the WISE data and best-fitting values of the derived parameters expected for smaller objects. Aims. We compare albedos and beaming parameters of PCF members and B-types of similar sizes and re-examine our conclusion on the different composition of the PCF. Methods. By modelling their WISE/NEOWISE data, we derived sizes and albedos of all objects whose Sloan Digital Sky Survey reflectances are similar to the typical B-type reflectance spectra. In particular, we derived the so-called infrared beaming parameters (η), effective diameters (D), and corresponding visible geometric albedos (pV), and studied their value distributions. Results. We obtained the effective diameter and geometric visible albedo for ~600 B-type asteroids whose sizes range between 2 and 100 km, approximately half of which have fitted η-values that are inversely correlated to size. We found that the albedo distributions of the PCF is significantly different from that of other B-types in the same size range (2-20 km), and we rule out any size-albedo dependency or biases related to the lower quality of the pV-values of smaller objects. In addition, we also found differences between the η-value distribution of the PCF and the other similarly-sized B-types. Conclusions. The differences in the visible albedos of PCF members and the other B-types of similar sizes is a strong indication that their compositions are different. The trend between beaming parameter and size of the B-types (excluding the PCF) is consistent with the expectation that the surfaces of smaller asteroids have coarser rocks than do those of larger objects (D> 40 km), which are thought to be covered by a finer, more insulating layer of dust.
Fil: Alí Lagoa, V.. Université de la Côte d’Azur; Francia. Instituto de Astrofísica de Canaria; España. Universidad de La Laguna; España
Fil: Licandro, J.. Universidad de La Laguna; España. Instituto de Astrofísica de Canaria; España
Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina. Universidad Nacional de San Juan; Argentina
Fil: Cañada Assandri, Marcela Inés. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina. Universidad Nacional de San Juan; Argentina
Fil: Delbon, Marisa Ester. Université de la Côte d’Azur; Francia
Fil: De León, J.. Instituto de Astrofísica de Canaria; España. Universidad de La Laguna; España
Fil: Campins, H.. University of Central Florida; Estados Unidos
Fil: Pinilla Alonso, N.. University of Tennessee; Estados Unidos. University of Central Florida; Estados Unidos
Fil: Kelley, M. S. P.. University of Maryland; Estados Unidos
Fil: Hanus, J.. Université de la Côte d’Azur; Francia
Materia
INFRARED: PLANETARY SYSTEMS
MINOR PLANETS, ASTEROIDS: GENERAL
SURVEYS
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/63614
Acceder
id CONICETDig_c98b3cfaa1c025f110e8417300bf558d
oai_identifier_str oai:ri.conicet.gov.ar:11336/63614
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling Differences between the Pallas collisional family and similarly sized B-type asteroids ?Alí Lagoa, V.Licandro, J.Gil Hutton, Ricardo AlfredoCañada Assandri, Marcela InésDelbon, Marisa EsterDe León, J.Campins, H.Pinilla Alonso, N.Kelley, M. S. P.Hanus, J.INFRARED: PLANETARY SYSTEMSMINOR PLANETS, ASTEROIDS: GENERALSURVEYShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. B-type asteroids constitute a peculiar spectral class within the C-complex. Previous work has pointed out the difference between the visible geometric albedos of B-types and those of the Pallas collisional family (PCF), whose few members with observed spectra are B-types (one exception out of eight objects). This has been interpreted as being due to compositional differences. However, the PCF members are typically smaller than the spectroscopically classified B-types, and the following possibilities have not been ruled out: the albedo differences might be related to a size-albedo dependence and/or to the generally larger errors of the WISE data and best-fitting values of the derived parameters expected for smaller objects. Aims. We compare albedos and beaming parameters of PCF members and B-types of similar sizes and re-examine our conclusion on the different composition of the PCF. Methods. By modelling their WISE/NEOWISE data, we derived sizes and albedos of all objects whose Sloan Digital Sky Survey reflectances are similar to the typical B-type reflectance spectra. In particular, we derived the so-called infrared beaming parameters (η), effective diameters (D), and corresponding visible geometric albedos (pV), and studied their value distributions. Results. We obtained the effective diameter and geometric visible albedo for ~600 B-type asteroids whose sizes range between 2 and 100 km, approximately half of which have fitted η-values that are inversely correlated to size. We found that the albedo distributions of the PCF is significantly different from that of other B-types in the same size range (2-20 km), and we rule out any size-albedo dependency or biases related to the lower quality of the pV-values of smaller objects. In addition, we also found differences between the η-value distribution of the PCF and the other similarly-sized B-types. Conclusions. The differences in the visible albedos of PCF members and the other B-types of similar sizes is a strong indication that their compositions are different. The trend between beaming parameter and size of the B-types (excluding the PCF) is consistent with the expectation that the surfaces of smaller asteroids have coarser rocks than do those of larger objects (D> 40 km), which are thought to be covered by a finer, more insulating layer of dust.Fil: Alí Lagoa, V.. Université de la Côte d’Azur; Francia. Instituto de Astrofísica de Canaria; España. Universidad de La Laguna; EspañaFil: Licandro, J.. Universidad de La Laguna; España. Instituto de Astrofísica de Canaria; EspañaFil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina. Universidad Nacional de San Juan; ArgentinaFil: Cañada Assandri, Marcela Inés. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina. Universidad Nacional de San Juan; ArgentinaFil: Delbon, Marisa Ester. Université de la Côte d’Azur; FranciaFil: De León, J.. Instituto de Astrofísica de Canaria; España. Universidad de La Laguna; EspañaFil: Campins, H.. University of Central Florida; Estados UnidosFil: Pinilla Alonso, N.. University of Tennessee; Estados Unidos. University of Central Florida; Estados UnidosFil: Kelley, M. S. P.. University of Maryland; Estados UnidosFil: Hanus, J.. Université de la Côte d’Azur; FranciaEDP Sciences2016-07info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/63614Alí Lagoa, V.; Licandro, J.; Gil Hutton, Ricardo Alfredo; Cañada Assandri, Marcela Inés; Delbon, Marisa Ester; et al.; Differences between the Pallas collisional family and similarly sized B-type asteroids ?; EDP Sciences; Astronomy and Astrophysics; 591; A14; 7-2016; 1-110004-6361CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527660info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/07/aa27660-15/aa27660-15.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:18:59Zoai:ri.conicet.gov.ar:11336/63614instacron: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 10:18:59.558CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Differences between the Pallas collisional family and similarly sized B-type asteroids ?
title Differences between the Pallas collisional family and similarly sized B-type asteroids ?
spellingShingle Differences between the Pallas collisional family and similarly sized B-type asteroids ?
Alí Lagoa, V.
INFRARED: PLANETARY SYSTEMS
MINOR PLANETS, ASTEROIDS: GENERAL
SURVEYS
title_short Differences between the Pallas collisional family and similarly sized B-type asteroids ?
title_full Differences between the Pallas collisional family and similarly sized B-type asteroids ?
title_fullStr Differences between the Pallas collisional family and similarly sized B-type asteroids ?
title_full_unstemmed Differences between the Pallas collisional family and similarly sized B-type asteroids ?
title_sort Differences between the Pallas collisional family and similarly sized B-type asteroids ?
dc.creator.none.fl_str_mv Alí Lagoa, V.
Licandro, J.
Gil Hutton, Ricardo Alfredo
Cañada Assandri, Marcela Inés
Delbon, Marisa Ester
De León, J.
Campins, H.
Pinilla Alonso, N.
Kelley, M. S. P.
Hanus, J.
author Alí Lagoa, V.
author_facet Alí Lagoa, V.
Licandro, J.
Gil Hutton, Ricardo Alfredo
Cañada Assandri, Marcela Inés
Delbon, Marisa Ester
De León, J.
Campins, H.
Pinilla Alonso, N.
Kelley, M. S. P.
Hanus, J.
author_role author
author2 Licandro, J.
Gil Hutton, Ricardo Alfredo
Cañada Assandri, Marcela Inés
Delbon, Marisa Ester
De León, J.
Campins, H.
Pinilla Alonso, N.
Kelley, M. S. P.
Hanus, J.
author2_role author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv INFRARED: PLANETARY SYSTEMS
MINOR PLANETS, ASTEROIDS: GENERAL
SURVEYS
topic INFRARED: PLANETARY SYSTEMS
MINOR PLANETS, ASTEROIDS: GENERAL
SURVEYS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Context. B-type asteroids constitute a peculiar spectral class within the C-complex. Previous work has pointed out the difference between the visible geometric albedos of B-types and those of the Pallas collisional family (PCF), whose few members with observed spectra are B-types (one exception out of eight objects). This has been interpreted as being due to compositional differences. However, the PCF members are typically smaller than the spectroscopically classified B-types, and the following possibilities have not been ruled out: the albedo differences might be related to a size-albedo dependence and/or to the generally larger errors of the WISE data and best-fitting values of the derived parameters expected for smaller objects. Aims. We compare albedos and beaming parameters of PCF members and B-types of similar sizes and re-examine our conclusion on the different composition of the PCF. Methods. By modelling their WISE/NEOWISE data, we derived sizes and albedos of all objects whose Sloan Digital Sky Survey reflectances are similar to the typical B-type reflectance spectra. In particular, we derived the so-called infrared beaming parameters (η), effective diameters (D), and corresponding visible geometric albedos (pV), and studied their value distributions. Results. We obtained the effective diameter and geometric visible albedo for ~600 B-type asteroids whose sizes range between 2 and 100 km, approximately half of which have fitted η-values that are inversely correlated to size. We found that the albedo distributions of the PCF is significantly different from that of other B-types in the same size range (2-20 km), and we rule out any size-albedo dependency or biases related to the lower quality of the pV-values of smaller objects. In addition, we also found differences between the η-value distribution of the PCF and the other similarly-sized B-types. Conclusions. The differences in the visible albedos of PCF members and the other B-types of similar sizes is a strong indication that their compositions are different. The trend between beaming parameter and size of the B-types (excluding the PCF) is consistent with the expectation that the surfaces of smaller asteroids have coarser rocks than do those of larger objects (D> 40 km), which are thought to be covered by a finer, more insulating layer of dust.
Fil: Alí Lagoa, V.. Université de la Côte d’Azur; Francia. Instituto de Astrofísica de Canaria; España. Universidad de La Laguna; España
Fil: Licandro, J.. Universidad de La Laguna; España. Instituto de Astrofísica de Canaria; España
Fil: Gil Hutton, Ricardo Alfredo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina. Universidad Nacional de San Juan; Argentina
Fil: Cañada Assandri, Marcela Inés. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Complejo Astronómico "El Leoncito". Universidad Nacional de Córdoba. Complejo Astronómico "El Leoncito". Universidad Nacional de la Plata. Complejo Astronómico "El Leoncito". Universidad Nacional de San Juan. Complejo Astronómico "El Leoncito"; Argentina. Universidad Nacional de San Juan; Argentina
Fil: Delbon, Marisa Ester. Université de la Côte d’Azur; Francia
Fil: De León, J.. Instituto de Astrofísica de Canaria; España. Universidad de La Laguna; España
Fil: Campins, H.. University of Central Florida; Estados Unidos
Fil: Pinilla Alonso, N.. University of Tennessee; Estados Unidos. University of Central Florida; Estados Unidos
Fil: Kelley, M. S. P.. University of Maryland; Estados Unidos
Fil: Hanus, J.. Université de la Côte d’Azur; Francia
description Context. B-type asteroids constitute a peculiar spectral class within the C-complex. Previous work has pointed out the difference between the visible geometric albedos of B-types and those of the Pallas collisional family (PCF), whose few members with observed spectra are B-types (one exception out of eight objects). This has been interpreted as being due to compositional differences. However, the PCF members are typically smaller than the spectroscopically classified B-types, and the following possibilities have not been ruled out: the albedo differences might be related to a size-albedo dependence and/or to the generally larger errors of the WISE data and best-fitting values of the derived parameters expected for smaller objects. Aims. We compare albedos and beaming parameters of PCF members and B-types of similar sizes and re-examine our conclusion on the different composition of the PCF. Methods. By modelling their WISE/NEOWISE data, we derived sizes and albedos of all objects whose Sloan Digital Sky Survey reflectances are similar to the typical B-type reflectance spectra. In particular, we derived the so-called infrared beaming parameters (η), effective diameters (D), and corresponding visible geometric albedos (pV), and studied their value distributions. Results. We obtained the effective diameter and geometric visible albedo for ~600 B-type asteroids whose sizes range between 2 and 100 km, approximately half of which have fitted η-values that are inversely correlated to size. We found that the albedo distributions of the PCF is significantly different from that of other B-types in the same size range (2-20 km), and we rule out any size-albedo dependency or biases related to the lower quality of the pV-values of smaller objects. In addition, we also found differences between the η-value distribution of the PCF and the other similarly-sized B-types. Conclusions. The differences in the visible albedos of PCF members and the other B-types of similar sizes is a strong indication that their compositions are different. The trend between beaming parameter and size of the B-types (excluding the PCF) is consistent with the expectation that the surfaces of smaller asteroids have coarser rocks than do those of larger objects (D> 40 km), which are thought to be covered by a finer, more insulating layer of dust.
publishDate 2016
dc.date.none.fl_str_mv 2016-07
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/11336/63614
Alí Lagoa, V.; Licandro, J.; Gil Hutton, Ricardo Alfredo; Cañada Assandri, Marcela Inés; Delbon, Marisa Ester; et al.; Differences between the Pallas collisional family and similarly sized B-type asteroids ?; EDP Sciences; Astronomy and Astrophysics; 591; A14; 7-2016; 1-11
0004-6361
CONICET Digital
CONICET
url http://hdl.handle.net/11336/63614
identifier_str_mv Alí Lagoa, V.; Licandro, J.; Gil Hutton, Ricardo Alfredo; Cañada Assandri, Marcela Inés; Delbon, Marisa Ester; et al.; Differences between the Pallas collisional family and similarly sized B-type asteroids ?; EDP Sciences; Astronomy and Astrophysics; 591; A14; 7-2016; 1-11
0004-6361
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/201527660
info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/abs/2016/07/aa27660-15/aa27660-15.html
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
application/pdf
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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_ 1844614156945195008
score 13.070432

Publicaciones similares