The structure of Chariklo's rings from stellar occultations

D. Berard; B. Sicardy; J. I. B. Camargo; J. Desmars; F. Braga-Ribas; J.-L. Ortiz; R. Duffard; N. Morales; E. Meza; R. Leiva; G. Benedetti-Rossi; R. Vieira-Martins; A.-R. Gomes Junior; M. Assafin; F. Colas; J.-L. Dauvergne; P. Kervella; J. Lecacheux; L. Maquet; F. Vachier; S. Renner; B. Monard; A. A. Sickafoose; H. Breytenbach; A. Genade; W. Beisker; K.-L. Bath; H.-J. Bode; M. Backes; V. D. Ivanov; E. Jehin; M. Gillon; J. Manfroid; J. Pollock; G. Tancredi; S. Roland; R. Salvo; L. Vanzi; D. Herald; D. Gault; S. Kerr; H. Pavlov; K. M. Hill; J. Bradshaw; M. A. Barry; A. Cool; B. Lade; A. Cole; J. Broughton; J. Newman; R. Horvat; D. Maybour; D. Giles; L. Davis; R. A. Paton; B. Loader; A. Pennell; P.-D. Jaquiery; S. Brillant; F. Selman; C. Dumas; C. Herrera; G. Carraro; L. Monaco; A. Maury; A. Peyrot; J.-P. Teng-Chuen-Yu; A. Richichi; P. Irawati; C. de Witt; P. Schoenau; R. Prager; C. Colazo; R. Melia; J. Spagnotto; A. Blain; S. Alonso; A. Roman; P. Santos-Sanz; J.-L. Rizos; J.-L. Maestre; D. Dunham

doi:10.3847/1538-3881/aa830d

The structure of Chariklo's rings from stellar occultations

D. Berard, B. Sicardy, J. I. B. Camargo, J. Desmars, F. Braga-Ribas, J.-L. Ortiz, R. Duffard, N. Morales, E. Meza, R. Leiva, G. Benedetti-Rossi, R. Vieira-Martins, A.-R. Gomes Junior, M. Assafin, F. Colas, J.-L. Dauvergne, P. Kervella, J. Lecacheux, L. Maquet, F. VachierS. Renner, B. Monard, A. A. Sickafoose, H. Breytenbach, A. Genade, W. Beisker, K.-L. Bath, H.-J. Bode, M. Backes, V. D. Ivanov, E. Jehin, M. Gillon, J. Manfroid, J. Pollock, G. Tancredi, S. Roland, R. Salvo, L. Vanzi, D. Herald, D. Gault, S. Kerr, H. Pavlov, K. M. Hill, J. Bradshaw, M. A. Barry, A. Cool, B. Lade, A. Cole, J. Broughton, J. Newman, R. Horvat, D. Maybour, D. Giles, L. Davis, R. A. Paton, B. Loader, A. Pennell, P.-D. Jaquiery, S. Brillant, F. Selman, C. Dumas, C. Herrera, G. Carraro, L. Monaco, A. Maury, A. Peyrot, J.-P. Teng-Chuen-Yu, A. Richichi, P. Irawati, C. de Witt, P. Schoenau, R. Prager, C. Colazo, R. Melia, J. Spagnotto, A. Blain, S. Alonso, A. Roman, P. Santos-Sanz, J.-L. Rizos, J.-L. Maestre, D. Dunham

Western Sydney University

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37 Citations (Scopus)

Abstract

Two narrow and dense rings (called C1R and C2R) were discovered around the Centaur object (10199) Chariklo during a stellar occultation observed on 2013 June 3. Following this discovery, we planned observations of several occultations by Chariklo's system in order to better characterize the physical properties of the ring and main body. Here, we use 12 successful occulations by Chariklo observed between 2014 and 2016. They provide ring profiles (physical width, opacity, edge structure) and constraints on the radii and pole position. Our new observations are currently consistent with the circular ring solution and pole position, to within the Â±3.3 km formal uncertainty for the ring radii derived by Braga-Ribas et al. The six resolved C1R profiles reveal significant width variations from ∼5 to 7.5 km. The width of the fainter ring C2R is less constrained, and may vary between 0.1 and 1 km. The inner and outer edges of C1R are consistent with infinitely sharp boundaries, with typical upper limits of one kilometer for the transition zone between the ring and empty space. No constraint on the sharpness of C2Rs edges is available. A 1s upper limit of ∼20 m is derived for the equivalent width of narrow (physical width <4 km) rings up to distances of 12,000 km, counted in the ring plane.

Original language	English
Article number	144
Number of pages	21
Journal	The Astronomical Journal
Volume	154
Issue number	4
DOIs	https://doi.org/10.3847/1538-3881/aa830d
Publication status	Published - 2017

Keywords

asteroids
ephemerides
occultations
planetary rings

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10.3847/1538-3881/aa830d

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Berard, D., Sicardy, B., Camargo, J. I. B., Desmars, J., Braga-Ribas, F., Ortiz, J.-L., Duffard, R., Morales, N., Meza, E., Leiva, R., Benedetti-Rossi, G., Vieira-Martins, R., Junior, A.-R. G., Assafin, M., Colas, F., Dauvergne, J.-L., Kervella, P., Lecacheux, J., Maquet, L., ... Dunham, D. (2017). The structure of Chariklo's rings from stellar occultations. The Astronomical Journal, 154(4), Article 144. https://doi.org/10.3847/1538-3881/aa830d

@article{1f515923116046299c18131c1ae2adde,

title = "The structure of Chariklo's rings from stellar occultations",

abstract = "Two narrow and dense rings (called C1R and C2R) were discovered around the Centaur object (10199) Chariklo during a stellar occultation observed on 2013 June 3. Following this discovery, we planned observations of several occultations by Chariklo's system in order to better characterize the physical properties of the ring and main body. Here, we use 12 successful occulations by Chariklo observed between 2014 and 2016. They provide ring profiles (physical width, opacity, edge structure) and constraints on the radii and pole position. Our new observations are currently consistent with the circular ring solution and pole position, to within the {\^A}±3.3 km formal uncertainty for the ring radii derived by Braga-Ribas et al. The six resolved C1R profiles reveal significant width variations from ∼5 to 7.5 km. The width of the fainter ring C2R is less constrained, and may vary between 0.1 and 1 km. The inner and outer edges of C1R are consistent with infinitely sharp boundaries, with typical upper limits of one kilometer for the transition zone between the ring and empty space. No constraint on the sharpness of C2Rs edges is available. A 1s upper limit of ∼20 m is derived for the equivalent width of narrow (physical width <4 km) rings up to distances of 12,000 km, counted in the ring plane.",

keywords = "asteroids, ephemerides, occultations, planetary rings",

author = "D. Berard and B. Sicardy and Camargo, {J. I. B.} and J. Desmars and F. Braga-Ribas and J.-L. Ortiz and R. Duffard and N. Morales and E. Meza and R. Leiva and G. Benedetti-Rossi and R. Vieira-Martins and Junior, {A.-R. Gomes} and M. Assafin and F. Colas and J.-L. Dauvergne and P. Kervella and J. Lecacheux and L. Maquet and F. Vachier and S. Renner and B. Monard and Sickafoose, {A. A.} and H. Breytenbach and A. Genade and W. Beisker and K.-L. Bath and H.-J. Bode and M. Backes and Ivanov, {V. D.} and E. Jehin and M. Gillon and J. Manfroid and J. Pollock and G. Tancredi and S. Roland and R. Salvo and L. Vanzi and D. Herald and D. Gault and S. Kerr and H. Pavlov and Hill, {K. M.} and J. Bradshaw and Barry, {M. A.} and A. Cool and B. Lade and A. Cole and J. Broughton and J. Newman and R. Horvat and D. Maybour and D. Giles and L. Davis and Paton, {R. A.} and B. Loader and A. Pennell and P.-D. Jaquiery and S. Brillant and F. Selman and C. Dumas and C. Herrera and G. Carraro and L. Monaco and A. Maury and A. Peyrot and J.-P. Teng-Chuen-Yu and A. Richichi and P. Irawati and Witt, {C. de} and P. Schoenau and R. Prager and C. Colazo and R. Melia and J. Spagnotto and A. Blain and S. Alonso and A. Roman and P. Santos-Sanz and J.-L. Rizos and J.-L. Maestre and D. Dunham",

year = "2017",

doi = "10.3847/1538-3881/aa830d",

language = "English",

volume = "154",

journal = "The Astronomical Journal",

issn = "0004-6256",

publisher = "Institute of Physics Publishing",

number = "4",

}

Berard, D, Sicardy, B, Camargo, JIB, Desmars, J, Braga-Ribas, F, Ortiz, J-L, Duffard, R, Morales, N, Meza, E, Leiva, R, Benedetti-Rossi, G, Vieira-Martins, R, Junior, A-RG, Assafin, M, Colas, F, Dauvergne, J-L, Kervella, P, Lecacheux, J, Maquet, L, Vachier, F, Renner, S, Monard, B, Sickafoose, AA, Breytenbach, H, Genade, A, Beisker, W, Bath, K-L, Bode, H-J, Backes, M, Ivanov, VD, Jehin, E, Gillon, M, Manfroid, J, Pollock, J, Tancredi, G, Roland, S, Salvo, R, Vanzi, L, Herald, D, Gault, D, Kerr, S, Pavlov, H, Hill, KM, Bradshaw, J, Barry, MA, Cool, A, Lade, B, Cole, A, Broughton, J, Newman, J, Horvat, R, Maybour, D, Giles, D, Davis, L, Paton, RA, Loader, B, Pennell, A, Jaquiery, P-D, Brillant, S, Selman, F, Dumas, C, Herrera, C, Carraro, G, Monaco, L, Maury, A, Peyrot, A, Teng-Chuen-Yu, J-P, Richichi, A, Irawati, P, Witt, CD, Schoenau, P, Prager, R, Colazo, C, Melia, R, Spagnotto, J, Blain, A, Alonso, S, Roman, A, Santos-Sanz, P, Rizos, J-L, Maestre, J-L & Dunham, D 2017, 'The structure of Chariklo's rings from stellar occultations', The Astronomical Journal, vol. 154, no. 4, 144. https://doi.org/10.3847/1538-3881/aa830d

TY - JOUR

T1 - The structure of Chariklo's rings from stellar occultations

AU - Berard, D.

AU - Sicardy, B.

AU - Camargo, J. I. B.

AU - Desmars, J.

AU - Braga-Ribas, F.

AU - Ortiz, J.-L.

AU - Duffard, R.

AU - Morales, N.

AU - Meza, E.

AU - Leiva, R.

AU - Benedetti-Rossi, G.

AU - Vieira-Martins, R.

AU - Junior, A.-R. Gomes

AU - Assafin, M.

AU - Colas, F.

AU - Dauvergne, J.-L.

AU - Kervella, P.

AU - Lecacheux, J.

AU - Maquet, L.

AU - Vachier, F.

AU - Renner, S.

AU - Monard, B.

AU - Sickafoose, A. A.

AU - Breytenbach, H.

AU - Genade, A.

AU - Beisker, W.

AU - Bath, K.-L.

AU - Bode, H.-J.

AU - Backes, M.

AU - Ivanov, V. D.

AU - Jehin, E.

AU - Gillon, M.

AU - Manfroid, J.

AU - Pollock, J.

AU - Tancredi, G.

AU - Roland, S.

AU - Salvo, R.

AU - Vanzi, L.

AU - Herald, D.

AU - Gault, D.

AU - Kerr, S.

AU - Pavlov, H.

AU - Hill, K. M.

AU - Bradshaw, J.

AU - Barry, M. A.

AU - Cool, A.

AU - Lade, B.

AU - Cole, A.

AU - Broughton, J.

AU - Newman, J.

AU - Horvat, R.

AU - Maybour, D.

AU - Giles, D.

AU - Davis, L.

AU - Paton, R. A.

AU - Loader, B.

AU - Pennell, A.

AU - Jaquiery, P.-D.

AU - Brillant, S.

AU - Selman, F.

AU - Dumas, C.

AU - Herrera, C.

AU - Carraro, G.

AU - Monaco, L.

AU - Maury, A.

AU - Peyrot, A.

AU - Teng-Chuen-Yu, J.-P.

AU - Richichi, A.

AU - Irawati, P.

AU - Witt, C. de

AU - Schoenau, P.

AU - Prager, R.

AU - Colazo, C.

AU - Melia, R.

AU - Spagnotto, J.

AU - Blain, A.

AU - Alonso, S.

AU - Roman, A.

AU - Santos-Sanz, P.

AU - Rizos, J.-L.

AU - Maestre, J.-L.

AU - Dunham, D.

PY - 2017

Y1 - 2017

N2 - Two narrow and dense rings (called C1R and C2R) were discovered around the Centaur object (10199) Chariklo during a stellar occultation observed on 2013 June 3. Following this discovery, we planned observations of several occultations by Chariklo's system in order to better characterize the physical properties of the ring and main body. Here, we use 12 successful occulations by Chariklo observed between 2014 and 2016. They provide ring profiles (physical width, opacity, edge structure) and constraints on the radii and pole position. Our new observations are currently consistent with the circular ring solution and pole position, to within the Â±3.3 km formal uncertainty for the ring radii derived by Braga-Ribas et al. The six resolved C1R profiles reveal significant width variations from ∼5 to 7.5 km. The width of the fainter ring C2R is less constrained, and may vary between 0.1 and 1 km. The inner and outer edges of C1R are consistent with infinitely sharp boundaries, with typical upper limits of one kilometer for the transition zone between the ring and empty space. No constraint on the sharpness of C2Rs edges is available. A 1s upper limit of ∼20 m is derived for the equivalent width of narrow (physical width <4 km) rings up to distances of 12,000 km, counted in the ring plane.

AB - Two narrow and dense rings (called C1R and C2R) were discovered around the Centaur object (10199) Chariklo during a stellar occultation observed on 2013 June 3. Following this discovery, we planned observations of several occultations by Chariklo's system in order to better characterize the physical properties of the ring and main body. Here, we use 12 successful occulations by Chariklo observed between 2014 and 2016. They provide ring profiles (physical width, opacity, edge structure) and constraints on the radii and pole position. Our new observations are currently consistent with the circular ring solution and pole position, to within the Â±3.3 km formal uncertainty for the ring radii derived by Braga-Ribas et al. The six resolved C1R profiles reveal significant width variations from ∼5 to 7.5 km. The width of the fainter ring C2R is less constrained, and may vary between 0.1 and 1 km. The inner and outer edges of C1R are consistent with infinitely sharp boundaries, with typical upper limits of one kilometer for the transition zone between the ring and empty space. No constraint on the sharpness of C2Rs edges is available. A 1s upper limit of ∼20 m is derived for the equivalent width of narrow (physical width <4 km) rings up to distances of 12,000 km, counted in the ring plane.

KW - asteroids

KW - ephemerides

KW - occultations

KW - planetary rings

UR - http://hdl.handle.net/1959.7/uws:43819

U2 - 10.3847/1538-3881/aa830d

DO - 10.3847/1538-3881/aa830d

M3 - Article

SN - 0004-6256

VL - 154

JO - The Astronomical Journal

JF - The Astronomical Journal

IS - 4

M1 - 144

ER -

The structure of Chariklo's rings from stellar occultations

Abstract

Keywords

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