Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020

B. E. Morgado; B. Sicardy; F. Braga-Ribas; J. Desmars; A. R. Gomes-Júnior; D. Bérard; R. Leiva; J. L. Ortiz; R. Vieira-Martins; G. Benedetti-Rossi; P. Santos-Sanz; J. I. B. Camargo; R. Duffard; F. L. Rommel; M. Assafin; R. C. Boufleur; F. Colas; M. Kretlow; W. Beisker; R. Sfair; C. Snodgrass; N. Morales; E. Fernández-Valenzuela; L. S. Amaral; A. Amarante; R. A. Artola; M. Backes; K-L. Bath; S. Bouley; M. W. Buie; P. Cacella; C. A. Colazo; J. P. Colque; J-L. Dauvergne; M. Dominik; M. Emilio; C. Erickson; R. Evans; J. Fabrega-Polleri; D. Garcia-Lambas; B. L. Giacchini; W. Hanna; D. Herald; G. Hesler; T. C. Hinse; C. Jacques; E. Jehin; U. G. Jørgensen; S. Kerr; V. Kouprianov; S. E. Levine; T. Linder; P. D. Maley; D. I. Machado; L. Maquet; A. Maury; R. Melia; E. Meza; B. Mondon; T. Moura; J. Newman; T. Payet; C. L. Pereira; J. Pollock; R. C. Poltronieri; F. Quispe-Huaynasi; D. Reichart; T. de Santana; E. M. Schneiter; M. V. Sieyra; J. Skottfelt; J. F. Soulier; M. Starck; P. Thierry; P. J. Torres; L. L. Trabuco; E. Unda-Sanzana; T. A. R. Yamashita; O. C. Winter; A. Zapata; C. A. Zuluaga

doi:10.1051/0004-6361/202141543

Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020

B. E. Morgado, B. Sicardy, F. Braga-Ribas, J. Desmars, A. R. Gomes-Júnior, D. Bérard, R. Leiva, J. L. Ortiz, R. Vieira-Martins, G. Benedetti-Rossi, P. Santos-Sanz, J. I. B. Camargo, R. Duffard, F. L. Rommel, M. Assafin, R. C. Boufleur, F. Colas, M. Kretlow, W. Beisker, R. SfairC. Snodgrass, N. Morales, E. Fernández-Valenzuela, L. S. Amaral, A. Amarante, R. A. Artola, M. Backes, K-L. Bath, S. Bouley, M. W. Buie, P. Cacella, C. A. Colazo, J. P. Colque, J-L. Dauvergne, M. Dominik, M. Emilio, C. Erickson, R. Evans, J. Fabrega-Polleri, D. Garcia-Lambas, B. L. Giacchini, W. Hanna, D. Herald, G. Hesler, T. C. Hinse, C. Jacques, E. Jehin, U. G. Jørgensen, S. Kerr, V. Kouprianov, S. E. Levine, T. Linder, P. D. Maley, D. I. Machado, L. Maquet, A. Maury, R. Melia, E. Meza, B. Mondon, T. Moura, J. Newman, T. Payet, C. L. Pereira, J. Pollock, R. C. Poltronieri, F. Quispe-Huaynasi, D. Reichart, T. de Santana, E. M. Schneiter, M. V. Sieyra, J. Skottfelt, J. F. Soulier, M. Starck, P. Thierry, P. J. Torres, L. L. Trabuco, E. Unda-Sanzana, T. A. R. Yamashita, O. C. Winter, A. Zapata, C. A. Zuluaga

Research output: Contribution to journal › Article › peer-review

Abstract

The Centaur (10199) Chariklo has the first rings system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow the determination of sizes and shapes with kilometre accuracy and obtain characteristics of the occulting object and its vicinity. Using stellar occultations observed between 2017 and 2020, we aim at constraining Chariklo's and its rings physical parameters. We also determine the rings' structure, and obtain precise astrometrical positions of Chariklo. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the data sets, from which ingress and egress times, and rings' width and opacity were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and rings' structure. 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 confirmed the detection of W-shaped structures within C1R and an evident variation of 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 ring particle's size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3-sigma), and its width variations may indicate an eccentricity higher than 0.005. We fit a tri-axial shape to Chariklo's detections over eleven occultations and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8, 135.2 and 99.1 km. Ultimately, we provided seven astrometric positions at a milliarcseconds accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris.

Original language	English
Journal	Astronomy & Astrophysics
DOIs	https://doi.org/10.1051/0004-6361/202141543
Publication status	Accepted/In press - 12 Jul 2021

Keywords

Occultations
Methods: observational
Methods: data analysis
Minor planets, asteroids: individual: Chariklo
Planets and satellites: rings

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10.1051/0004-6361/202141543

Morgado-2021-Refined-physical-parameters-A&A-AAM
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Accepted author manuscript, 9.43 MB

http://adsabs.harvard.edu/abs/2021arXiv210707904M

Cite this

Morgado, B. E., Sicardy, B., Braga-Ribas, F., Desmars, J., Gomes-Júnior, A. R., Bérard, D., Leiva, R., Ortiz, J. L., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Sanz, P., Camargo, J. I. B., Duffard, R., Rommel, F. L., Assafin, M., Boufleur, R. C., Colas, F., Kretlow, M., Beisker, W., ... Zuluaga, C. A. (Accepted/In press). Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020. Astronomy & Astrophysics. https://doi.org/10.1051/0004-6361/202141543

@article{352651c4a14b42b69092dd306a281146,

title = "Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020",

abstract = "The Centaur (10199) Chariklo has the first rings system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow the determination of sizes and shapes with kilometre accuracy and obtain characteristics of the occulting object and its vicinity. Using stellar occultations observed between 2017 and 2020, we aim at constraining Chariklo's and its rings physical parameters. We also determine the rings' structure, and obtain precise astrometrical positions of Chariklo. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the data sets, from which ingress and egress times, and rings' width and opacity were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and rings' structure. 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 confirmed the detection of W-shaped structures within C1R and an evident variation of 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 ring particle's size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3-sigma), and its width variations may indicate an eccentricity higher than 0.005. We fit a tri-axial shape to Chariklo's detections over eleven occultations and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8, 135.2 and 99.1 km. Ultimately, we provided seven astrometric positions at a milliarcseconds accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris.",

keywords = "Occultations, Methods: observational, Methods: data analysis, Minor planets, asteroids: individual: Chariklo, Planets and satellites: rings",

author = "Morgado, {B. E.} and B. Sicardy and F. Braga-Ribas and J. Desmars and Gomes-J{\'u}nior, {A. R.} and D. B{\'e}rard and R. Leiva and Ortiz, {J. L.} and R. Vieira-Martins and G. Benedetti-Rossi and P. Santos-Sanz and Camargo, {J. I. B.} and R. Duffard and Rommel, {F. L.} and M. Assafin and Boufleur, {R. C.} and F. Colas and M. Kretlow and W. Beisker and R. Sfair and C. Snodgrass and N. Morales and E. Fern{\'a}ndez-Valenzuela and Amaral, {L. S.} and A. Amarante and Artola, {R. A.} and M. Backes and K-L. Bath and S. Bouley and Buie, {M. W.} and P. Cacella and Colazo, {C. A.} and Colque, {J. P.} and J-L. Dauvergne and M. Dominik and M. Emilio and C. Erickson and R. Evans and J. Fabrega-Polleri and D. Garcia-Lambas and Giacchini, {B. L.} and W. Hanna and D. Herald and G. Hesler and Hinse, {T. C.} and C. Jacques and E. Jehin and J{\o}rgensen, {U. G.} and S. Kerr and V. Kouprianov and Levine, {S. E.} and T. Linder and Maley, {P. D.} and Machado, {D. I.} and L. Maquet and A. Maury and R. Melia and E. Meza and B. Mondon and T. Moura and J. Newman and T. Payet and Pereira, {C. L.} and J. Pollock and Poltronieri, {R. C.} and F. Quispe-Huaynasi and D. Reichart and {de Santana}, T. and Schneiter, {E. M.} and Sieyra, {M. V.} and J. Skottfelt and Soulier, {J. F.} and M. Starck and P. Thierry and Torres, {P. J.} and Trabuco, {L. L.} and E. Unda-Sanzana and Yamashita, {T. A. R.} and Winter, {O. C.} and A. Zapata and Zuluaga, {C. A.}",

note = "Funding: UGJ acknowledges funding from the European Union H2020-MSCA- ITN-2019 under grant no. 860470 (CHAMELEON) and from the Novo Nordisk Foundation Interdisciplinary Synergy Programme grant no. NNF19OC0057374. The following authors acknowledge the respective CNPq grants: BEM 150612/2020-6; FB-R 314772/2020-0; RV-M 304544/2017-f5, 401903/2016-8; JIBC 308150/2016-3 and 305917/2019-6; MA 427700/2018-3, 310683/2017-3, 473002/2013-2. GBR acknowledges CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016 and CAPES-PRINT/UNESP grant 88887.571156/2020-00, MA FAPERJ grant E-26/111.488/2013 and ARGJr FAPESP grant 2018/11239-8. J.L.O., P.S-S., R.D., and N.M. acknowledge financial support from the State Agency for Researchof the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrof{\'i}sica de Andaluc{\'i}a (SEV-2017-0709), from Spanish project AYA2017-89637-R, and from FEDER. P.S-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 “LEO-SBNAF” (MCIU/AEI/FEDER, UE). E. Jehin is a Belgian FNRS Senior Research Associate. RS and OCW acknowledge FAPESP grant 2016/24561-0 and CNPq grant 305210/2018-1. TCH acknowledges financial support from the National Research Foundation (NRF; No. 2019R1I1A1A01059609).",

year = "2021",

month = jul,

day = "12",

doi = "10.1051/0004-6361/202141543",

language = "English",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Morgado, BE, Sicardy, B, Braga-Ribas, F, Desmars, J, Gomes-Júnior, AR, Bérard, D, Leiva, R, Ortiz, JL, Vieira-Martins, R, Benedetti-Rossi, G, Santos-Sanz, P, Camargo, JIB, Duffard, R, Rommel, FL, Assafin, M, Boufleur, RC, Colas, F, Kretlow, M, Beisker, W, Sfair, R, Snodgrass, C, Morales, N, Fernández-Valenzuela, E, Amaral, LS, Amarante, A, Artola, RA, Backes, M, Bath, K-L, Bouley, S, Buie, MW, Cacella, P, Colazo, CA, Colque, JP, Dauvergne, J-L, Dominik, M, Emilio, M, Erickson, C, Evans, R, Fabrega-Polleri, J, Garcia-Lambas, D, Giacchini, BL, Hanna, W, Herald, D, Hesler, G, Hinse, TC, Jacques, C, Jehin, E, Jørgensen, UG, Kerr, S, Kouprianov, V, Levine, SE, Linder, T, Maley, PD, Machado, DI, Maquet, L, Maury, A, Melia, R, Meza, E, Mondon, B, Moura, T, Newman, J, Payet, T, Pereira, CL, Pollock, J, Poltronieri, RC, Quispe-Huaynasi, F, Reichart, D, de Santana, T, Schneiter, EM, Sieyra, MV, Skottfelt, J, Soulier, JF, Starck, M, Thierry, P, Torres, PJ, Trabuco, LL, Unda-Sanzana, E, Yamashita, TAR, Winter, OC, Zapata, A & Zuluaga, CA 2021, 'Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020', Astronomy & Astrophysics. https://doi.org/10.1051/0004-6361/202141543

TY - JOUR

T1 - Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020

AU - Morgado, B. E.

AU - Sicardy, B.

AU - Braga-Ribas, F.

AU - Desmars, J.

AU - Gomes-Júnior, A. R.

AU - Bérard, D.

AU - Leiva, R.

AU - Ortiz, J. L.

AU - Vieira-Martins, R.

AU - Benedetti-Rossi, G.

AU - Santos-Sanz, P.

AU - Camargo, J. I. B.

AU - Duffard, R.

AU - Rommel, F. L.

AU - Assafin, M.

AU - Boufleur, R. C.

AU - Colas, F.

AU - Kretlow, M.

AU - Beisker, W.

AU - Sfair, R.

AU - Snodgrass, C.

AU - Morales, N.

AU - Fernández-Valenzuela, E.

AU - Amaral, L. S.

AU - Amarante, A.

AU - Artola, R. A.

AU - Backes, M.

AU - Bath, K-L.

AU - Bouley, S.

AU - Buie, M. W.

AU - Cacella, P.

AU - Colazo, C. A.

AU - Colque, J. P.

AU - Dauvergne, J-L.

AU - Dominik, M.

AU - Emilio, M.

AU - Erickson, C.

AU - Evans, R.

AU - Fabrega-Polleri, J.

AU - Garcia-Lambas, D.

AU - Giacchini, B. L.

AU - Hanna, W.

AU - Herald, D.

AU - Hesler, G.

AU - Hinse, T. C.

AU - Jacques, C.

AU - Jehin, E.

AU - Jørgensen, U. G.

AU - Kerr, S.

AU - Kouprianov, V.

AU - Levine, S. E.

AU - Linder, T.

AU - Maley, P. D.

AU - Machado, D. I.

AU - Maquet, L.

AU - Maury, A.

AU - Melia, R.

AU - Meza, E.

AU - Mondon, B.

AU - Moura, T.

AU - Newman, J.

AU - Payet, T.

AU - Pereira, C. L.

AU - Pollock, J.

AU - Poltronieri, R. C.

AU - Quispe-Huaynasi, F.

AU - Reichart, D.

AU - de Santana, T.

AU - Schneiter, E. M.

AU - Sieyra, M. V.

AU - Skottfelt, J.

AU - Soulier, J. F.

AU - Starck, M.

AU - Thierry, P.

AU - Torres, P. J.

AU - Trabuco, L. L.

AU - Unda-Sanzana, E.

AU - Yamashita, T. A. R.

AU - Winter, O. C.

AU - Zapata, A.

AU - Zuluaga, C. A.

N1 - Funding: UGJ acknowledges funding from the European Union H2020-MSCA- ITN-2019 under grant no. 860470 (CHAMELEON) and from the Novo Nordisk Foundation Interdisciplinary Synergy Programme grant no. NNF19OC0057374. The following authors acknowledge the respective CNPq grants: BEM 150612/2020-6; FB-R 314772/2020-0; RV-M 304544/2017-f5, 401903/2016-8; JIBC 308150/2016-3 and 305917/2019-6; MA 427700/2018-3, 310683/2017-3, 473002/2013-2. GBR acknowledges CAPES-FAPERJ/PAPDRJ grant E26/203.173/2016 and CAPES-PRINT/UNESP grant 88887.571156/2020-00, MA FAPERJ grant E-26/111.488/2013 and ARGJr FAPESP grant 2018/11239-8. J.L.O., P.S-S., R.D., and N.M. acknowledge financial support from the State Agency for Researchof the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709), from Spanish project AYA2017-89637-R, and from FEDER. P.S-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 “LEO-SBNAF” (MCIU/AEI/FEDER, UE). E. Jehin is a Belgian FNRS Senior Research Associate. RS and OCW acknowledge FAPESP grant 2016/24561-0 and CNPq grant 305210/2018-1. TCH acknowledges financial support from the National Research Foundation (NRF; No. 2019R1I1A1A01059609).

PY - 2021/7/12

Y1 - 2021/7/12

N2 - The Centaur (10199) Chariklo has the first rings system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow the determination of sizes and shapes with kilometre accuracy and obtain characteristics of the occulting object and its vicinity. Using stellar occultations observed between 2017 and 2020, we aim at constraining Chariklo's and its rings physical parameters. We also determine the rings' structure, and obtain precise astrometrical positions of Chariklo. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the data sets, from which ingress and egress times, and rings' width and opacity were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and rings' structure. 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 confirmed the detection of W-shaped structures within C1R and an evident variation of 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 ring particle's size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3-sigma), and its width variations may indicate an eccentricity higher than 0.005. We fit a tri-axial shape to Chariklo's detections over eleven occultations and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8, 135.2 and 99.1 km. Ultimately, we provided seven astrometric positions at a milliarcseconds accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris.

AB - The Centaur (10199) Chariklo has the first rings system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow the determination of sizes and shapes with kilometre accuracy and obtain characteristics of the occulting object and its vicinity. Using stellar occultations observed between 2017 and 2020, we aim at constraining Chariklo's and its rings physical parameters. We also determine the rings' structure, and obtain precise astrometrical positions of Chariklo. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the data sets, from which ingress and egress times, and rings' width and opacity were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and rings' structure. 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 confirmed the detection of W-shaped structures within C1R and an evident variation of 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 ring particle's size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3-sigma), and its width variations may indicate an eccentricity higher than 0.005. We fit a tri-axial shape to Chariklo's detections over eleven occultations and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8, 135.2 and 99.1 km. Ultimately, we provided seven astrometric positions at a milliarcseconds accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris.

KW - Occultations

KW - Methods: observational

KW - Methods: data analysis

KW - Minor planets, asteroids: individual: Chariklo

KW - Planets and satellites: rings

U2 - 10.1051/0004-6361/202141543

DO - 10.1051/0004-6361/202141543

M3 - Article

SN - 0004-6361

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

ER -