Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020
- Autores
- Morgado, B.E.; Sicardy, Bruno; Braga Ribas, Felipe; Desmars, Josselin; Gomes Júnior, Altair Ramos; Bérard, D.; Leiva, Rodrigo; Vieira Martins, Roberto; Benedetti Rossi, G.; Santos Sanz, Pablo; Camargo, Julio Ignacio Bueno; Duffard, R.; Rommel, F.L.; Assafin, M.; Boufleur, R.C.; Colas, F.; Kretlow, Mike; Beisker, W.; Sfair, Rafael; Snodgrass, Colin; Morales, N.; Fernández Valenzuela, E.; Amaral, L.S.; Amarante, A.; Artola, R.A.; Backes, M.; Bath, K. L.; Bouley, S.; Garcia Lambas, Diego Rodolfo; Schneiter, Ernesto Matías
- Año de publicación
- 2021
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- Context. The Centaur (10199) Chariklo has the first ring system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow sizes and shapes to be determined with kilometre accuracy, and provide the characteristics of the occulting object and its vicinity. Aims. Using stellar occultations observed between 2017 and 2020, our aim is to constrain the physical parameters of Chariklo and its rings. We also determine the structure of the rings, and obtain precise astrometrical positions of Chariklo. Methods. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the datasets, from which ingress and egress times, and the ring widths and opacity values were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and ring structure. Results. We characterise Chariklo's ring system (C1R and C2R), and obtain radii and pole orientations that are consistent with, but more accurate than, results from previous occultations. We confirm the detection of W-shaped structures within C1R and an evident variation in radial width. The observed width ranges between 4.8 and 9.1 km with a mean value of 6.5 km. One dual observation (visible and red) does not reveal any differences in the C1R opacity profiles, indicating a ring particle size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3σ), and its width variations may indicate an eccentricity higher than ~0.005. We fit a tri-axial shape to Chariklo's detections over 11 occultations, and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8-1.5+1.4, 135.2-2.8+1.4, and 99.1-2.7+5.4 km. Ultimately, we provided seven astrometric positions at a milliarcsecond accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris.
Fil: Morgado, B.E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Sicardy, Bruno. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Braga Ribas, Felipe. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Universidade Tecnologia Federal do Parana; Brasil
Fil: Desmars, Josselin. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Gomes Júnior, Altair Ramos. Universidade de Sao Paulo; Brasil
Fil: Bérard, D.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Leiva, Rodrigo. Universidad de Chile; Chile. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Vieira Martins, Roberto. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil. Universidade Federal do Rio de Janeiro; Brasil
Fil: Benedetti Rossi, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Universidade Federal de Sao Paulo; Brasil
Fil: Santos Sanz, Pablo. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Camargo, Julio Ignacio Bueno. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Duffard, R.. Universidade Federal do Rio de Janeiro; Brasil
Fil: Rommel, F.L.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Assafin, M.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Boufleur, R.C.. Universidad Nacional de Córdoba; Argentina
Fil: Colas, F.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Kretlow, Mike. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Beisker, W.. University of North Carolina; Estados Unidos
Fil: Sfair, Rafael. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Snodgrass, Colin. University of Edinburgh; Reino Unido
Fil: Morales, N.. Pontificia Universidad Católica de Chile; Chile. Universidad Católica de Chile; Chile
Fil: Fernández Valenzuela, E.. Pontificia Universidad Católica de Chile; Chile. Universidad Católica de Chile; Chile
Fil: Amaral, L.S.. Massachusetts Institute of Technology; Estados Unidos
Fil: Amarante, A.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil
Fil: Artola, R.A.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Backes, M.. Universidad Nacional de Córdoba; Argentina
Fil: Bath, K. L.. University of North Carolina; Estados Unidos
Fil: Bouley, S.. University of St. Andrews; Reino Unido
Fil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina
Fil: Schneiter, Ernesto Matías. Universidad Nacional de Córdoba. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Ingeniería Económica y Legal; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina - Materia
-
ASTEROIDS: INDIVIDUAL: CHARIKLO
METHODS: DATA ANALYSIS
METHODS: OBSERVATIONAL
MINOR PLANETS
OCCULTATIONS
PLANETS AND SATELLITES: RINGS - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- https://creativecommons.org/licenses/by/2.5/ar/
- Repositorio
.jpg)
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/173040
Ver los metadatos del registro completo
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Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020Morgado, B.E.Sicardy, BrunoBraga Ribas, FelipeDesmars, JosselinGomes Júnior, Altair RamosBérard, D.Leiva, RodrigoVieira Martins, RobertoBenedetti Rossi, G.Santos Sanz, PabloCamargo, Julio Ignacio BuenoDuffard, R.Rommel, F.L.Assafin, M.Boufleur, R.C.Colas, F.Kretlow, MikeBeisker, W.Sfair, RafaelSnodgrass, ColinMorales, N.Fernández Valenzuela, E.Amaral, L.S.Amarante, A.Artola, R.A.Backes, M.Bath, K. L.Bouley, S.Garcia Lambas, Diego RodolfoSchneiter, Ernesto MatíasASTEROIDS: INDIVIDUAL: CHARIKLOMETHODS: DATA ANALYSISMETHODS: OBSERVATIONALMINOR PLANETSOCCULTATIONSPLANETS AND SATELLITES: RINGShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Context. The Centaur (10199) Chariklo has the first ring system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow sizes and shapes to be determined with kilometre accuracy, and provide the characteristics of the occulting object and its vicinity. Aims. Using stellar occultations observed between 2017 and 2020, our aim is to constrain the physical parameters of Chariklo and its rings. We also determine the structure of the rings, and obtain precise astrometrical positions of Chariklo. Methods. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the datasets, from which ingress and egress times, and the ring widths and opacity values were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and ring structure. Results. We characterise Chariklo's ring system (C1R and C2R), and obtain radii and pole orientations that are consistent with, but more accurate than, results from previous occultations. We confirm the detection of W-shaped structures within C1R and an evident variation in radial width. The observed width ranges between 4.8 and 9.1 km with a mean value of 6.5 km. One dual observation (visible and red) does not reveal any differences in the C1R opacity profiles, indicating a ring particle size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3σ), and its width variations may indicate an eccentricity higher than ~0.005. We fit a tri-axial shape to Chariklo's detections over 11 occultations, and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8-1.5+1.4, 135.2-2.8+1.4, and 99.1-2.7+5.4 km. Ultimately, we provided seven astrometric positions at a milliarcsecond accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris.Fil: Morgado, B.E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Sicardy, Bruno. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Braga Ribas, Felipe. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Universidade Tecnologia Federal do Parana; BrasilFil: Desmars, Josselin. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Gomes Júnior, Altair Ramos. Universidade de Sao Paulo; BrasilFil: Bérard, D.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Leiva, Rodrigo. Universidad de Chile; Chile. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Vieira Martins, Roberto. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil. Universidade Federal do Rio de Janeiro; BrasilFil: Benedetti Rossi, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Universidade Federal de Sao Paulo; BrasilFil: Santos Sanz, Pablo. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Camargo, Julio Ignacio Bueno. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Duffard, R.. Universidade Federal do Rio de Janeiro; BrasilFil: Rommel, F.L.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Assafin, M.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Boufleur, R.C.. Universidad Nacional de Córdoba; ArgentinaFil: Colas, F.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Kretlow, Mike. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Beisker, W.. University of North Carolina; Estados UnidosFil: Sfair, Rafael. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Snodgrass, Colin. University of Edinburgh; Reino UnidoFil: Morales, N.. Pontificia Universidad Católica de Chile; Chile. Universidad Católica de Chile; ChileFil: Fernández Valenzuela, E.. Pontificia Universidad Católica de Chile; Chile. Universidad Católica de Chile; ChileFil: Amaral, L.S.. Massachusetts Institute of Technology; Estados UnidosFil: Amarante, A.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; BrasilFil: Artola, R.A.. Centre National de la Recherche Scientifique. Observatoire de Paris; FranciaFil: Backes, M.. Universidad Nacional de Córdoba; ArgentinaFil: Bath, K. L.. University of North Carolina; Estados UnidosFil: Bouley, S.. University of St. Andrews; Reino UnidoFil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaFil: Schneiter, Ernesto Matías. Universidad Nacional de Córdoba. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Ingeniería Económica y Legal; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; ArgentinaEDP Sciences2021-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/173040Morgado, B.E.; Sicardy, Bruno; Braga Ribas, Felipe; Desmars, Josselin; Gomes Júnior, Altair Ramos; et al.; Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020; EDP Sciences; Astronomy and Astrophysics; 652; A141; 8-2021; 1-290004-63611432-0746CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202141543info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2021/08/aa41543-21/aa41543-21.htmlinfo:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-11-05T09:36:55Zoai:ri.conicet.gov.ar:11336/173040instacron: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:34982025-11-05 09:36:55.436CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse |
| dc.title.none.fl_str_mv |
Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020 |
| title |
Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020 |
| spellingShingle |
Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020 Morgado, B.E. ASTEROIDS: INDIVIDUAL: CHARIKLO METHODS: DATA ANALYSIS METHODS: OBSERVATIONAL MINOR PLANETS OCCULTATIONS PLANETS AND SATELLITES: RINGS |
| title_short |
Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020 |
| title_full |
Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020 |
| title_fullStr |
Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020 |
| title_full_unstemmed |
Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020 |
| title_sort |
Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020 |
| dc.creator.none.fl_str_mv |
Morgado, B.E. Sicardy, Bruno Braga Ribas, Felipe Desmars, Josselin Gomes Júnior, Altair Ramos Bérard, D. Leiva, Rodrigo Vieira Martins, Roberto Benedetti Rossi, G. Santos Sanz, Pablo Camargo, Julio Ignacio Bueno Duffard, R. Rommel, F.L. Assafin, M. Boufleur, R.C. Colas, F. Kretlow, Mike Beisker, W. Sfair, Rafael Snodgrass, Colin Morales, N. Fernández Valenzuela, E. Amaral, L.S. Amarante, A. Artola, R.A. Backes, M. Bath, K. L. Bouley, S. Garcia Lambas, Diego Rodolfo Schneiter, Ernesto Matías |
| author |
Morgado, B.E. |
| author_facet |
Morgado, B.E. Sicardy, Bruno Braga Ribas, Felipe Desmars, Josselin Gomes Júnior, Altair Ramos Bérard, D. Leiva, Rodrigo Vieira Martins, Roberto Benedetti Rossi, G. Santos Sanz, Pablo Camargo, Julio Ignacio Bueno Duffard, R. Rommel, F.L. Assafin, M. Boufleur, R.C. Colas, F. Kretlow, Mike Beisker, W. Sfair, Rafael Snodgrass, Colin Morales, N. Fernández Valenzuela, E. Amaral, L.S. Amarante, A. Artola, R.A. Backes, M. Bath, K. L. Bouley, S. Garcia Lambas, Diego Rodolfo Schneiter, Ernesto Matías |
| author_role |
author |
| author2 |
Sicardy, Bruno Braga Ribas, Felipe Desmars, Josselin Gomes Júnior, Altair Ramos Bérard, D. Leiva, Rodrigo Vieira Martins, Roberto Benedetti Rossi, G. Santos Sanz, Pablo Camargo, Julio Ignacio Bueno Duffard, R. Rommel, F.L. Assafin, M. Boufleur, R.C. Colas, F. Kretlow, Mike Beisker, W. Sfair, Rafael Snodgrass, Colin Morales, N. Fernández Valenzuela, E. Amaral, L.S. Amarante, A. Artola, R.A. Backes, M. Bath, K. L. Bouley, S. Garcia Lambas, Diego Rodolfo Schneiter, Ernesto Matías |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
ASTEROIDS: INDIVIDUAL: CHARIKLO METHODS: DATA ANALYSIS METHODS: OBSERVATIONAL MINOR PLANETS OCCULTATIONS PLANETS AND SATELLITES: RINGS |
| topic |
ASTEROIDS: INDIVIDUAL: CHARIKLO METHODS: DATA ANALYSIS METHODS: OBSERVATIONAL MINOR PLANETS OCCULTATIONS PLANETS AND SATELLITES: RINGS |
| 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. The Centaur (10199) Chariklo has the first ring system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow sizes and shapes to be determined with kilometre accuracy, and provide the characteristics of the occulting object and its vicinity. Aims. Using stellar occultations observed between 2017 and 2020, our aim is to constrain the physical parameters of Chariklo and its rings. We also determine the structure of the rings, and obtain precise astrometrical positions of Chariklo. Methods. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the datasets, from which ingress and egress times, and the ring widths and opacity values were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and ring structure. Results. We characterise Chariklo's ring system (C1R and C2R), and obtain radii and pole orientations that are consistent with, but more accurate than, results from previous occultations. We confirm the detection of W-shaped structures within C1R and an evident variation in radial width. The observed width ranges between 4.8 and 9.1 km with a mean value of 6.5 km. One dual observation (visible and red) does not reveal any differences in the C1R opacity profiles, indicating a ring particle size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3σ), and its width variations may indicate an eccentricity higher than ~0.005. We fit a tri-axial shape to Chariklo's detections over 11 occultations, and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8-1.5+1.4, 135.2-2.8+1.4, and 99.1-2.7+5.4 km. Ultimately, we provided seven astrometric positions at a milliarcsecond accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris. Fil: Morgado, B.E.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil Fil: Sicardy, Bruno. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Braga Ribas, Felipe. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Universidade Tecnologia Federal do Parana; Brasil Fil: Desmars, Josselin. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Gomes Júnior, Altair Ramos. Universidade de Sao Paulo; Brasil Fil: Bérard, D.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Leiva, Rodrigo. Universidad de Chile; Chile. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Vieira Martins, Roberto. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil. Universidade Federal do Rio de Janeiro; Brasil Fil: Benedetti Rossi, G.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia. Universidade Federal de Sao Paulo; Brasil Fil: Santos Sanz, Pablo. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil Fil: Camargo, Julio Ignacio Bueno. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil Fil: Duffard, R.. Universidade Federal do Rio de Janeiro; Brasil Fil: Rommel, F.L.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil Fil: Assafin, M.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Boufleur, R.C.. Universidad Nacional de Córdoba; Argentina Fil: Colas, F.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil Fil: Kretlow, Mike. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil Fil: Beisker, W.. University of North Carolina; Estados Unidos Fil: Sfair, Rafael. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Snodgrass, Colin. University of Edinburgh; Reino Unido Fil: Morales, N.. Pontificia Universidad Católica de Chile; Chile. Universidad Católica de Chile; Chile Fil: Fernández Valenzuela, E.. Pontificia Universidad Católica de Chile; Chile. Universidad Católica de Chile; Chile Fil: Amaral, L.S.. Massachusetts Institute of Technology; Estados Unidos Fil: Amarante, A.. Ministério de Ciencia, Tecnologia e Innovacao. Observatorio Nacional; Brasil Fil: Artola, R.A.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Backes, M.. Universidad Nacional de Córdoba; Argentina Fil: Bath, K. L.. University of North Carolina; Estados Unidos Fil: Bouley, S.. University of St. Andrews; Reino Unido Fil: Garcia Lambas, Diego Rodolfo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina Fil: Schneiter, Ernesto Matías. Universidad Nacional de Córdoba. Facultad de Ciencias Exactas, Físicas y Naturales. Departamento de Ingeniería Económica y Legal; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina |
| description |
Context. The Centaur (10199) Chariklo has the first ring system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow sizes and shapes to be determined with kilometre accuracy, and provide the characteristics of the occulting object and its vicinity. Aims. Using stellar occultations observed between 2017 and 2020, our aim is to constrain the physical parameters of Chariklo and its rings. We also determine the structure of the rings, and obtain precise astrometrical positions of Chariklo. Methods. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the datasets, from which ingress and egress times, and the ring widths and opacity values were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and ring structure. Results. We characterise Chariklo's ring system (C1R and C2R), and obtain radii and pole orientations that are consistent with, but more accurate than, results from previous occultations. We confirm the detection of W-shaped structures within C1R and an evident variation in radial width. The observed width ranges between 4.8 and 9.1 km with a mean value of 6.5 km. One dual observation (visible and red) does not reveal any differences in the C1R opacity profiles, indicating a ring particle size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3σ), and its width variations may indicate an eccentricity higher than ~0.005. We fit a tri-axial shape to Chariklo's detections over 11 occultations, and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8-1.5+1.4, 135.2-2.8+1.4, and 99.1-2.7+5.4 km. Ultimately, we provided seven astrometric positions at a milliarcsecond accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris. |
| publishDate |
2021 |
| dc.date.none.fl_str_mv |
2021-08 |
| 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/11336/173040 Morgado, B.E.; Sicardy, Bruno; Braga Ribas, Felipe; Desmars, Josselin; Gomes Júnior, Altair Ramos; et al.; Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020; EDP Sciences; Astronomy and Astrophysics; 652; A141; 8-2021; 1-29 0004-6361 1432-0746 CONICET Digital CONICET |
| url |
http://hdl.handle.net/11336/173040 |
| identifier_str_mv |
Morgado, B.E.; Sicardy, Bruno; Braga Ribas, Felipe; Desmars, Josselin; Gomes Júnior, Altair Ramos; et al.; Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020; EDP Sciences; Astronomy and Astrophysics; 652; A141; 8-2021; 1-29 0004-6361 1432-0746 CONICET Digital CONICET |
| dc.language.none.fl_str_mv |
eng |
| language |
eng |
| dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/doi/10.1051/0004-6361/202141543 info:eu-repo/semantics/altIdentifier/url/https://www.aanda.org/articles/aa/full_html/2021/08/aa41543-21/aa41543-21.html |
| 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 |
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_ |
1847976831444058112 |
| score |
13.087074 |