A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Basit Öğe Kaydı
dc.authoridBraga Ribas, Felipe/0000-0003-2311-2438
dc.authoridNARDIELLO, Domenico/0000-0003-1149-3659
dc.authoridSantana-Ros, Toni/0000-0002-0143-9440
dc.authoridErece, Orhan/0000-0002-9723-6823
dc.authoridWeber, Christian/0000-0003-2778-4047
dc.authoridKozhukhov, Oleksandr/0000-0002-3858-9389
dc.authoridDesmars, Josselin/0000-0002-2193-8204
dc.contributor.authorRommel, F. L.
dc.contributor.authorBraga-Ribas, F.
dc.contributor.authorOrtiz, J. L.
dc.contributor.authorSicardy, B.
dc.contributor.authorSantos-Sanz, P.
dc.contributor.authorDesmars, J.
dc.contributor.authorCamargo, J. I. B.
dc.date.accessioned2025-01-27T20:41:15Z
dc.date.available2025-01-27T20:41:15Z
dc.date.issued2023
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractContext. The physical characterization of trans-Neptunian objects is essential for improving our understanding of the formation and evolution of our Solar System. Stellar occultation is a ground-based technique that can be successfully used to determine some of the TNOs' fundamental physical properties with high precision, such as size and shape. Aims. This work is aimed at constraining the size, shape, and geometric albedo of the dwarf planet candidate (307261) 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also study the object's topography by analyzing the obtained limb and residuals between the observed chords and the best-fit ellipse. Metods. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS4 between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with between 3 and 61 positive chords. We derived the occultation light curves using differential aperture photometry, from which the star ingress and egress instants were calculated. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fit ellipse, combined with the object's rotational information from the literature, sets constraints on the object's size, shape, and albedo. Additionally, we developed a new method to characterize the topography features on the object's limb. Results. The global limb has a semi-major axis of a' = 412 +/- 10 km, a semi-minor axis of b'= 385 +/- 17 km, and the position angle of the minor axis is 121 degrees +/- 16 degrees. From this instantaneous limb, we obtained 2002 MS4's geometric albedo of p(V) = 0.1 +/- 0.025, using HV = 3.63 +/- 0.05 mag and a projected area-equivalent diameter of 796 +/- 24 km. Significant deviations from the fitted ellipse in the northernmost limb were detected from multiple sites, highlighting three distinct topographic features: one 11 km depth depression, followed by a 25(-5)(+4) km height elevation next to a crater-like depression, with an extension of 322 +/- 39 km and 45.1 +/- 1.5 km deep. Conclusions. Our results indicate the presence of an object that is approximate to 138 km smaller in diameter than that derived from thermal data, possibly indicating the presence of a thus-far unknown satellite. However, within the error bars, the geometric albedo in the V-band is in agreement with the results published in the literature, even with the radiometric-derived albedo. This stellar occultation has allowed for the first multichord measurement of a large topography in a TNO.
dc.description.sponsorshipCoordenacao de Aperfeicoamento de Pessoal de Nivel Superior -Brazil (CAPES) [001]; National Institute of Science and Technology of the eUniverse project; CNPq [103096/2023-0, 314772/2020-0, 307368/2021-1, 308150/2016-3, 305917/2019-6, 427700/2018-3, 310683/2017-3, 473002/2013-2, 128580/2020-8, 150612/2020-6, 305210/2018-1, CAPES/Cofecub-394/2016-05]; Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia 'Maria de Maeztu') [CEX2019-000918-M]; European Union [PID2021-122842OB-C21]; European Research Council funds under the European Community [669416]; CAPES [88887.705245/2022-00]; CAPES -FAPERJ/PAPDRJ [E26/203.173/2016, 88887.310463/2018-00, 88887.571156/2020-00]; FAPERJ [E-26/111.488/2013]; FAPESP [2018/11239-8]; FAPESP - F.R.S.-FNRS [T.0109.20]; Francqui Foundation; French Centre National d'Etudes Spatiales (CNES) [2022-2023]; National Research, Development and Innovation Office (NKFIH, Hungary) [K-138962, K-125015, KEP-7/2018]; Hungarian Academy of Sciences [MCIN/AEI/10.13039/501100011033, CEX2021-001131-S, PID2019-109467GB-I00, PID2021-128062NBI00, H2020-EU2-1-6/870377, 67985815]; CNRS; Portuguese Foundation for Science and Technology (FCT); European Social Fund (ESF) [SFRH/BD/131700/2017]; Heising-Simons Foundation; SPECULOOS network situated in Tenerife, Spain; ERC under the European Union [336480/SPECULOOS]; Consejeria de Economia, Conocimiento y Empleo del Gobierno de Canarias; European Regional Development Fund (ERDF) [ProID2021010134]; Agencia Estatal de Investigacion del Ministerio de Ciencia e Innovacion (AEI-MCINN) [PID2020-120464GB-100]; Slovak Grant Agency for Science [VEGA 2/0059/22, VEGA 2/0031/22]; Romanian National Authority for Scientific Research -UEFISCDI [PN-III-P1-1.1-TE-2019-1504]; Italian Amateur Astronomers Union (UAI) [FB210003, MAS IC120009]; Island Council of Ibiza - Scientific Research Projects Coordination Unit of Istanbul University [BAP-3685, FBG-2017-23943]; Presidency of Strategy and Budget of the Republic of Turkey [2016K12137]; Belgian FNRS [PDR T.0120.21]; ARC grant for Concerted Research Actions; Wallonia-Brussels Federation - University of Liege; Cadi Ayyad University of Marrakesh; Schmidt telescopes (Asiago, Italy) of the INAF-Astronomical Observatory of Padova; Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil; University of North Carolina at Chapel Hill; Michigan State University (MSU); STFC [ST/X005933/1, ST/T00147X/1] Funding Source: UKRI
dc.description.sponsorshipThis study was financed in part by the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior -Brazil (CAPES) -Finance Code 001, the National Institute of Science and Technology of the eUniverse project (INCT do e-Universo, CNPq grant 465376/2014-2), the Spanish MICIN/AEI/10.13039/501100011033, the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia 'Maria de Maeztu') through grant CEX2019-000918-M, the ERDF A way of making Europe by the European Union through grant PID2021-122842OB-C21, and within the Lucky Star umbrella that agglomerates the efforts of the Paris, Granada, and Rio teams, which the European Research Council funds under the European Community's H2020 (ERC Grant Agreement No. 669416). The following authors acknowledge the respective CNPq grants: F. L. R. 103096/2023-0; F.B.-R. 314772/2020-0; R.V.-M. 307368/2021-1; J.I.B.C. 308150/2016-3 and 305917/2019-6; M.A. 427700/2018-3, 310683/2017-3, 473002/2013-2; G.M. 128580/2020-8; B.E.M. 150612/2020-6; and O.C.W. 305210/2018-1. The following authors acknowledge the respective grants: B.E.M. thanks the CAPES/Cofecub-394/2016-05; G.M. thanks the CAPES grant 88887.705245/2022-00; G.B-R. acknowledges CAPES -FAPERJ/PAPDRJ grant E26/203.173/2016 and the scholarship granted in the scope of the Program CAPES-PrInt, process number 88887.310463/2018-00, Mobility number 88887.571156/2020-00; M.A. acknowledges FAPERJ grant E-26/111.488/2013; A.R.G.Jr acknowledges FAPESP grant 2018/11239-8; O.C.W. and R.S. acknowledge FAPESP grant 2016/24561-0; K.B. acknowledges the scholarship funded by F.R.S.-FNRS grant T.0109.20 and by the Francqui Foundation; D.N. acknowledges the support from the French Centre National d'Etudes Spatiales (CNES); D. S. thank to Fulbright Visiting Scholar (2022-2023) at the University of California, Berkeley; A.P. and R.S. thank to the National Research, Development and Innovation Office (NKFIH, Hungary) grants K-138962 and K-125015. Partial funding for the computational infrastructure and database servers is received from the grant KEP-7/2018 of the Hungarian Academy of Sciences; R.D., J.L.O., P.S.-S., N.M., R.H., A.S.L., and J.M. T.-R. acknowledge the MCIN/AEI/10.13039/501100011033 under the grant respective grants: CEX2021-001131-S, PID2019-109467GB-I00, and PID2021-128062NBI00; T.S.R. acknowledges funding from the NEO-MAPP project (H2020-EU2-1-6/870377); K.H. was supported by the project R.V.O.: 67985815; A.K. thanks to the IRAP, Midi-Pyrenees Observatory, CNRS, University of Toulouse, France; J.M.O. acknowledges the Portuguese Foundation for Science and Technology (FCT) and the European Social Fund (ESF) through the Ph.D. grant SFRH/BD/131700/2017; J.d.W. and MIT acknowledge the Heising-Simons Foundation, Dr. and Mrs. Colin Masson, and Dr. Peter A. Gilman for Artemis, the first telescope of the SPECULOOS network situated in Tenerife, Spain. The ULiege's contribution to SPECULOOS has received funding from the ERC under the European Union's Seventh Framework Programme (FP/2007-2013) (grant number 336480/SPECULOOS); J.L. acknowledges the ACIISII, Consejeria de Economia, Conocimiento y Empleo del Gobierno de Canarias, and the European Regional Development Fund (ERDF) under the grant ProID2021010134, also the Agencia Estatal de Investigacion del Ministerio de Ciencia e Innovacion (AEI-MCINN) under the grant PID2020-120464GB-100; D.T., R.K., M.H., and T.P. were supported by the Slovak Grant Agency for Science grants number VEGA 2/0059/22, and VEGA 2/0031/22; M. P. r was supported by a grant from the Romanian National Authority for Scientific Research -UEFISCDI, project number PN-III-P1-1.1-TE-2019-1504; P.B., M.M., and M.D.G. thank the support of the Italian Amateur Astronomers Union (UAI); C.F. acknowledges the support from ANID BASAL project FB210003, and grant MAS IC120009. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular, the institutions participating in the Gaia Multilateral Agreement. The Joan Oro Telescope (TJO) of the Montsec Observatory (OdM) is owned by the Catalan Government and operated by the Institute for Space Studies of Catalonia (IEEC). TCH telescope is financed by the Island Council of Ibiza..IST60 and.IST40 are the observational facilities of the Istanbul University Observatory, funded by the Scientific Research Projects Coordination Unit of Istanbul University with project numbers BAP-3685 and FBG-2017-23943 and the Presidency of Strategy and Budget of the Republic of Turkey with the project 2016K12137. TRAPPIST is a project funded by the Belgian FNRS grant PDR T.0120.21 and the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. E.J. is an FNRS Senior Research Associate. TRAPPIST-North is funded by the University of Liege and performed in collaboration with the Cadi Ayyad University of Marrakesh. This work made use of observations obtained at the 1.6 m telescope on the Pico dos Dias Observatory of the National Laboratory of Astrophysics (LNA/Brazil), at the Copernicus and Schmidt telescopes (Asiago, Italy) of the INAF-Astronomical Observatory of Padova, and at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). We thank the following observers who participated and provided data for the events listed in Appendix A: A. Ciarnella, A. L. Ivanov, A. Olsen, A. Ossola B. Dintinjana, B. Hanna, C. Costa, G. H. Rudnick, J. Paul, J. J. Castellani, J. Polak, K. Guhl, L. A. Molnar, L. Perez, M. Bertini, M. Bigi, M. Rottenborn, M. Sabil, N. V. Ivanova, P. Langill, P. Thierry, S. Bouquillon, S. Lamina, T. O. Dementiev, V. A. Ivanov, and X. Delmotte.
dc.identifier.doi10.1051/0004-6361/202346892
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.scopus2-s2.0-85176256860
dc.identifier.scopusqualityQ1
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202346892
dc.identifier.urihttps://hdl.handle.net/20.500.12428/24078
dc.identifier.volume678
dc.identifier.wosWOS:001100938600008
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherEdp Sciences S A
dc.relation.ispartofAstronomy & Astrophysics
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectKuiper belt objects: individual: 2002 MS4
dc.subjectmethods: observational
dc.titleA large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations
dc.typeArticle

Dosyalar

Koleksiyon

WoS İndeksli Yayınlar Koleksiyonu
Scopus İndeksli Yayınlar Koleksiyonu