Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations

C l Pereira; F Braga-Ribas; B Sicardy; A r Gomes-Júnior; J l Ortiz; H c Branco; J i b Camargo; B e Morgado; R Vieira-Martins; M Assafin; G Benedetti-Rossi; J Desmars; M Emilio; R Morales; F l Rommel; T Hayamizu; T Gondou; E Jehin; R a Artola; A Asai; C Colazo; E Ducrot; R Duffard; J Fabrega; E Fernandez-Valenzuela; M Gillon; T Horaguchi; M Ida; K Kitazaki; L a Mammana; A Maury; M Melita; N Morales; C Moya-Sierralta; M Owada; J Pollock; J l Sanchez; P Santos-Sanz; N Sasanuma; D Sebastian; A Triaud; S Uchiyama; L Vanzi; H Watanabe; H Yamamura

doi:10.1093/mnras/stad3318

Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations

C l Pereira^*, F Braga-Ribas, B Sicardy, A r Gomes-Júnior, J l Ortiz, H c Branco, J i b Camargo, B e Morgado, R Vieira-Martins, M Assafin, G Benedetti-Rossi, J Desmars, M Emilio, R Morales, F l Rommel, T Hayamizu, T Gondou, E Jehin, R a Artola, A AsaiC Colazo, E Ducrot, R Duffard, J Fabrega, E Fernandez-Valenzuela, M Gillon, T Horaguchi, M Ida, K Kitazaki, L a Mammana, A Maury, M Melita, N Morales, C Moya-Sierralta, M Owada, J Pollock, J l Sanchez, P Santos-Sanz, N Sasanuma, D Sebastian, A Triaud, S Uchiyama, L Vanzi, H Watanabe, H Yamamura

^*Corresponding author for this work

Physics and Astronomy

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Abstract

The Centaur (60558) Echeclus was discovered on March 03, 2000, orbiting between the orbits of Jupiter and Uranus. After exhibiting frequent outbursts, it also received a comet designation, 174P. If the ejected material can be a source of debris to form additional structures, studying the surroundings of an active body like Echeclus can provide clues about the formation scenarios of rings, jets, or dusty shells around small bodies. Stellar occultation is a handy technique for this kind of investigation, as it can, from Earth-based observations, detect small structures with low opacity around these objects. Stellar occultation by Echeclus was predicted and observed in 2019, 2020, and 2021. We obtain upper detection limits of rings with widths larger than 0.5 km and optical depth of τ = 0.02. These values are smaller than those of Chariklo’s main ring; in other words, a Chariklo-like ring would have been detected. The occultation observed in 2020 provided two positive chords used to derive the triaxial dimensions of Echeclus based on a 3D model and pole orientation available in the literature. We obtained a = 37.0 ± 0.6 km, b = 28.4 ± 0.5 km, and c = 24.9 ± 0.4 km, resulting in an area-equivalent radius of 30.0 ± 0.5 km. Using the projected limb at the occultation epoch and the available absolute magnitude (⁠Hv=9.971±0.031
⁠), we calculate an albedo of pv = 0.050 ± 0.003. Constraints on the object’s density and internal friction are also proposed.

Original language	English
Article number	stad3318
Journal	Monthly Notices of the Royal Astronomical Society
Early online date	28 Oct 2023
DOIs	https://doi.org/10.1093/mnras/stad3318
Publication status	E-pub ahead of print - 28 Oct 2023

Bibliographical note

C.L.P is thankful for the support of the CAPES and FAPERJ/DSC-10
(E26/204.141/2022). This work was carried out within the “Lucky
Star” umbrella that agglomerates the efforts of the Paris, Granada,
and Rio teams, funded by the European Research Council under
the European Community’s H2020 (ERC Grant Agreement No.
669416). This study was partly financed by the National Institute
of Science and Technology of the e-Universe project (INCT do eUniverso, CNPq grant 465376/2014-2). This study was financed in part by CAPES – Finance Code 001. The authors acknowledge the respective CNPq grants: B.E.M. 150612/2020-6; F.B.R. 314772/2020-0; R.V.M. 307368/2021-1; M.A. 427700/2018-3, 310683/2017-3, 473002/2013-2; J.I.B.C. acknowledges grants 305917/2019-6, 306691/2022-1 (CNPq) and 201.681/2019 (FAPERJ). J. L. O. acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033, also acknowledges
the financial support by the Spanish grants PID2020-112789GBI00 from AEI and Proyecto de Excelencia de la Junta de Andalucía PY20-01309. P.S-S. acknowledges financial support from the Spanish I+D+i project PID2022-139555NB-I00 funded by MCIN/AEI/10.13039/501100011033. We acknowledges financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033. E.D. acknowledges support from the innovation and research Horizon 2020 program in the context of the Marie Sklodowska-Curie subvention 945298.
TRAPPIST-South is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique,FNRS) under the grant PDR T.0120.21. E.J. is F.R.S.-FNRS Senior Research Associate. This research received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant’s agreement n◦ 803193/BEBOP), from the Science and Technology Facilities Council (STFC; grant n◦ ST/S00193X/1), and from the MERAC foundation. This research received funding from the European Research Council (ERC) under
the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 803193/BEBOP). The ULiege’s contribution to SPECULOOS-South Observatory has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007–2013) (grant Agreement n◦336480/SPECULOOS), from the Balzan Prize and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant no. T.0109.20), from the University of Liege, and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. The contribution of the University of Cambridge to SPECULOOS-South Observatory is supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). M.G. is F.R.S.-FNRS Research Director. L. V. was partially funded by ANID, BASAL, FB210003. We thank the observers A. Hashimoto, M. Meunier for their efforts in the observational campaigns. Some results were based on observations taken at the 1.6 m telescope at Pico dos Dias Observatory of the National Laboratory of Astrophysics (L.N.A./Brazil). This work has made use of data from the European Space Agency (E.S.A.) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the
Gaia Data Processing and Analysis Consortium (D.P.A.C., https:
//www.cosmos.esa.int/web/gaia/dpac/consortium).

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Pereira, C. L., Braga-Ribas, F., Sicardy, B., Gomes-Júnior, A. R., Ortiz, J. L., Branco, H. C., Camargo, J. I. B., Morgado, B. E., Vieira-Martins, R., Assafin, M., Benedetti-Rossi, G., Desmars, J., Emilio, M., Morales, R., Rommel, F. L., Hayamizu, T., Gondou, T., Jehin, E., Artola, R. A., ... Yamamura, H. (2023). Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations. Monthly Notices of the Royal Astronomical Society, Article stad3318. Advance online publication. https://doi.org/10.1093/mnras/stad3318

@article{3ac3c97bc2b84f55880bbe34f3a0b5ff,

title = "Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations",

abstract = "The Centaur (60558) Echeclus was discovered on March 03, 2000, orbiting between the orbits of Jupiter and Uranus. After exhibiting frequent outbursts, it also received a comet designation, 174P. If the ejected material can be a source of debris to form additional structures, studying the surroundings of an active body like Echeclus can provide clues about the formation scenarios of rings, jets, or dusty shells around small bodies. Stellar occultation is a handy technique for this kind of investigation, as it can, from Earth-based observations, detect small structures with low opacity around these objects. Stellar occultation by Echeclus was predicted and observed in 2019, 2020, and 2021. We obtain upper detection limits of rings with widths larger than 0.5 km and optical depth of τ = 0.02. These values are smaller than those of Chariklo{\textquoteright}s main ring; in other words, a Chariklo-like ring would have been detected. The occultation observed in 2020 provided two positive chords used to derive the triaxial dimensions of Echeclus based on a 3D model and pole orientation available in the literature. We obtained a = 37.0 ± 0.6 km, b = 28.4 ± 0.5 km, and c = 24.9 ± 0.4 km, resulting in an area-equivalent radius of 30.0 ± 0.5 km. Using the projected limb at the occultation epoch and the available absolute magnitude (⁠Hv=9.971±0.031⁠), we calculate an albedo of pv = 0.050 ± 0.003. Constraints on the object{\textquoteright}s density and internal friction are also proposed.",

author = "Pereira, {C l} and F Braga-Ribas and B Sicardy and Gomes-J{\'u}nior, {A r} and Ortiz, {J l} and Branco, {H c} and Camargo, {J i b} and Morgado, {B e} and R Vieira-Martins and M Assafin and G Benedetti-Rossi and J Desmars and M Emilio and R Morales and Rommel, {F l} and T Hayamizu and T Gondou and E Jehin and Artola, {R a} and A Asai and C Colazo and E Ducrot and R Duffard and J Fabrega and E Fernandez-Valenzuela and M Gillon and T Horaguchi and M Ida and K Kitazaki and Mammana, {L a} and A Maury and M Melita and N Morales and C Moya-Sierralta and M Owada and J Pollock and Sanchez, {J l} and P Santos-Sanz and N Sasanuma and D Sebastian and A Triaud and S Uchiyama and L Vanzi and H Watanabe and H Yamamura",

note = "C.L.P is thankful for the support of the CAPES and FAPERJ/DSC-10 (E26/204.141/2022). This work was carried out within the “Lucky Star” umbrella that agglomerates the efforts of the Paris, Granada, and Rio teams, funded by the European Research Council under the European Community{\textquoteright}s H2020 (ERC Grant Agreement No. 669416). This study was partly financed by the National Institute of Science and Technology of the e-Universe project (INCT do eUniverso, CNPq grant 465376/2014-2). This study was financed in part by CAPES – Finance Code 001. The authors acknowledge the respective CNPq grants: B.E.M. 150612/2020-6; F.B.R. 314772/2020-0; R.V.M. 307368/2021-1; M.A. 427700/2018-3, 310683/2017-3, 473002/2013-2; J.I.B.C. acknowledges grants 305917/2019-6, 306691/2022-1 (CNPq) and 201.681/2019 (FAPERJ). J. L. O. acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033, also acknowledges the financial support by the Spanish grants PID2020-112789GBI00 from AEI and Proyecto de Excelencia de la Junta de Andaluc{\'i}a PY20-01309. P.S-S. acknowledges financial support from the Spanish I+D+i project PID2022-139555NB-I00 funded by MCIN/AEI/10.13039/501100011033. We acknowledges financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033. E.D. acknowledges support from the innovation and research Horizon 2020 program in the context of the Marie Sklodowska-Curie subvention 945298. TRAPPIST-South is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique,FNRS) under the grant PDR T.0120.21. E.J. is F.R.S.-FNRS Senior Research Associate. This research received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant{\textquoteright}s agreement n◦ 803193/BEBOP), from the Science and Technology Facilities Council (STFC; grant n◦ ST/S00193X/1), and from the MERAC foundation. This research received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant agreement no. 803193/BEBOP). The ULiege{\textquoteright}s contribution to SPECULOOS-South Observatory has received funding from the European Research Council under the European Union{\textquoteright}s Seventh Framework Programme (FP/2007–2013) (grant Agreement n◦336480/SPECULOOS), from the Balzan Prize and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant no. T.0109.20), from the University of Liege, and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. The contribution of the University of Cambridge to SPECULOOS-South Observatory is supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). M.G. is F.R.S.-FNRS Research Director. L. V. was partially funded by ANID, BASAL, FB210003. We thank the observers A. Hashimoto, M. Meunier for their efforts in the observational campaigns. Some results were based on observations taken at the 1.6 m telescope at Pico dos Dias Observatory of the National Laboratory of Astrophysics (L.N.A./Brazil). This work has made use of data from the European Space Agency (E.S.A.) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (D.P.A.C., https: //www.cosmos.esa.int/web/gaia/dpac/consortium). ",

year = "2023",

month = oct,

day = "28",

doi = "10.1093/mnras/stad3318",

language = "English",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "SIPRI/Oxford University Press",

}

Pereira, CL, Braga-Ribas, F, Sicardy, B, Gomes-Júnior, AR, Ortiz, JL, Branco, HC, Camargo, JIB, Morgado, BE, Vieira-Martins, R, Assafin, M, Benedetti-Rossi, G, Desmars, J, Emilio, M, Morales, R, Rommel, FL, Hayamizu, T, Gondou, T, Jehin, E, Artola, RA, Asai, A, Colazo, C, Ducrot, E, Duffard, R, Fabrega, J, Fernandez-Valenzuela, E, Gillon, M, Horaguchi, T, Ida, M, Kitazaki, K, Mammana, LA, Maury, A, Melita, M, Morales, N, Moya-Sierralta, C, Owada, M, Pollock, J, Sanchez, JL, Santos-Sanz, P, Sasanuma, N, Sebastian, D , Triaud, A, Uchiyama, S, Vanzi, L, Watanabe, H & Yamamura, H 2023, 'Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations', Monthly Notices of the Royal Astronomical Society. https://doi.org/10.1093/mnras/stad3318

TY - JOUR

T1 - Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations

AU - Pereira, C l

AU - Braga-Ribas, F

AU - Sicardy, B

AU - Gomes-Júnior, A r

AU - Ortiz, J l

AU - Branco, H c

AU - Camargo, J i b

AU - Morgado, B e

AU - Vieira-Martins, R

AU - Assafin, M

AU - Benedetti-Rossi, G

AU - Desmars, J

AU - Emilio, M

AU - Morales, R

AU - Rommel, F l

AU - Hayamizu, T

AU - Gondou, T

AU - Jehin, E

AU - Artola, R a

AU - Asai, A

AU - Colazo, C

AU - Ducrot, E

AU - Duffard, R

AU - Fabrega, J

AU - Fernandez-Valenzuela, E

AU - Gillon, M

AU - Horaguchi, T

AU - Ida, M

AU - Kitazaki, K

AU - Mammana, L a

AU - Maury, A

AU - Melita, M

AU - Morales, N

AU - Moya-Sierralta, C

AU - Owada, M

AU - Pollock, J

AU - Sanchez, J l

AU - Santos-Sanz, P

AU - Sasanuma, N

AU - Sebastian, D

AU - Triaud, A

AU - Uchiyama, S

AU - Vanzi, L

AU - Watanabe, H

AU - Yamamura, H

N1 - C.L.P is thankful for the support of the CAPES and FAPERJ/DSC-10 (E26/204.141/2022). This work was carried out within the “Lucky Star” umbrella that agglomerates the efforts of the Paris, Granada, and Rio teams, funded by the European Research Council under the European Community’s H2020 (ERC Grant Agreement No. 669416). This study was partly financed by the National Institute of Science and Technology of the e-Universe project (INCT do eUniverso, CNPq grant 465376/2014-2). This study was financed in part by CAPES – Finance Code 001. The authors acknowledge the respective CNPq grants: B.E.M. 150612/2020-6; F.B.R. 314772/2020-0; R.V.M. 307368/2021-1; M.A. 427700/2018-3, 310683/2017-3, 473002/2013-2; J.I.B.C. acknowledges grants 305917/2019-6, 306691/2022-1 (CNPq) and 201.681/2019 (FAPERJ). J. L. O. acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033, also acknowledges the financial support by the Spanish grants PID2020-112789GBI00 from AEI and Proyecto de Excelencia de la Junta de Andalucía PY20-01309. P.S-S. acknowledges financial support from the Spanish I+D+i project PID2022-139555NB-I00 funded by MCIN/AEI/10.13039/501100011033. We acknowledges financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033. E.D. acknowledges support from the innovation and research Horizon 2020 program in the context of the Marie Sklodowska-Curie subvention 945298. TRAPPIST-South is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique,FNRS) under the grant PDR T.0120.21. E.J. is F.R.S.-FNRS Senior Research Associate. This research received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant’s agreement n◦ 803193/BEBOP), from the Science and Technology Facilities Council (STFC; grant n◦ ST/S00193X/1), and from the MERAC foundation. This research received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 803193/BEBOP). The ULiege’s contribution to SPECULOOS-South Observatory has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007–2013) (grant Agreement n◦336480/SPECULOOS), from the Balzan Prize and Francqui Foundations, from the Belgian Scientific Research Foundation (F.R.S.-FNRS; grant no. T.0109.20), from the University of Liege, and from the ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. The contribution of the University of Cambridge to SPECULOOS-South Observatory is supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). M.G. is F.R.S.-FNRS Research Director. L. V. was partially funded by ANID, BASAL, FB210003. We thank the observers A. Hashimoto, M. Meunier for their efforts in the observational campaigns. Some results were based on observations taken at the 1.6 m telescope at Pico dos Dias Observatory of the National Laboratory of Astrophysics (L.N.A./Brazil). This work has made use of data from the European Space Agency (E.S.A.) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (D.P.A.C., https: //www.cosmos.esa.int/web/gaia/dpac/consortium).

PY - 2023/10/28

Y1 - 2023/10/28

N2 - The Centaur (60558) Echeclus was discovered on March 03, 2000, orbiting between the orbits of Jupiter and Uranus. After exhibiting frequent outbursts, it also received a comet designation, 174P. If the ejected material can be a source of debris to form additional structures, studying the surroundings of an active body like Echeclus can provide clues about the formation scenarios of rings, jets, or dusty shells around small bodies. Stellar occultation is a handy technique for this kind of investigation, as it can, from Earth-based observations, detect small structures with low opacity around these objects. Stellar occultation by Echeclus was predicted and observed in 2019, 2020, and 2021. We obtain upper detection limits of rings with widths larger than 0.5 km and optical depth of τ = 0.02. These values are smaller than those of Chariklo’s main ring; in other words, a Chariklo-like ring would have been detected. The occultation observed in 2020 provided two positive chords used to derive the triaxial dimensions of Echeclus based on a 3D model and pole orientation available in the literature. We obtained a = 37.0 ± 0.6 km, b = 28.4 ± 0.5 km, and c = 24.9 ± 0.4 km, resulting in an area-equivalent radius of 30.0 ± 0.5 km. Using the projected limb at the occultation epoch and the available absolute magnitude (⁠Hv=9.971±0.031⁠), we calculate an albedo of pv = 0.050 ± 0.003. Constraints on the object’s density and internal friction are also proposed.

AB - The Centaur (60558) Echeclus was discovered on March 03, 2000, orbiting between the orbits of Jupiter and Uranus. After exhibiting frequent outbursts, it also received a comet designation, 174P. If the ejected material can be a source of debris to form additional structures, studying the surroundings of an active body like Echeclus can provide clues about the formation scenarios of rings, jets, or dusty shells around small bodies. Stellar occultation is a handy technique for this kind of investigation, as it can, from Earth-based observations, detect small structures with low opacity around these objects. Stellar occultation by Echeclus was predicted and observed in 2019, 2020, and 2021. We obtain upper detection limits of rings with widths larger than 0.5 km and optical depth of τ = 0.02. These values are smaller than those of Chariklo’s main ring; in other words, a Chariklo-like ring would have been detected. The occultation observed in 2020 provided two positive chords used to derive the triaxial dimensions of Echeclus based on a 3D model and pole orientation available in the literature. We obtained a = 37.0 ± 0.6 km, b = 28.4 ± 0.5 km, and c = 24.9 ± 0.4 km, resulting in an area-equivalent radius of 30.0 ± 0.5 km. Using the projected limb at the occultation epoch and the available absolute magnitude (⁠Hv=9.971±0.031⁠), we calculate an albedo of pv = 0.050 ± 0.003. Constraints on the object’s density and internal friction are also proposed.

U2 - 10.1093/mnras/stad3318

DO - 10.1093/mnras/stad3318

M3 - Article

SN - 0035-8711

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

M1 - stad3318

ER -

Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations

Abstract

Bibliographical note

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