Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation

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dc.authoridSolmaz, Arif/0000-0002-3076-164X
dc.authoridSantos-Sanz, Pablo/0000-0002-1123-983X
dc.authoridKrugly, Yurij N/0000-0002-3171-9873
dc.authoridPopescu, Marcel/0000-0001-8585-204X
dc.authoridRibas, Felipe Braga/0000-0003-2311-2438
dc.authoridMorgado, Bruno Eduardo/0000-0003-0088-1808
dc.authoridKudak, Viktor/0000-0001-7494-3093
dc.authorwosidSolmaz, Arif/AAJ-3305-2021
dc.authorwosidSantos-Sanz, Pablo/O-1308-2019
dc.authorwosidNir, Guy/HJJ-0199-2023
dc.authorwosidKrugly, Yurij N/O-7164-2018
dc.authorwosidPopescu, Marcel/AAA-4863-2019
dc.authorwosidRibas, Felipe Braga/H-4727-2012
dc.authorwosidOliveira, Joana/KHV-0466-2024
dc.contributor.authorSantos-Sanz, P.
dc.contributor.authorOrtiz, J. L.
dc.contributor.authorSicardy, B.
dc.contributor.authorPopescu, M.
dc.contributor.authorBenedetti-Rossi, G.
dc.contributor.authorMorales, N.
dc.contributor.authorVara-Lubiano, M.
dc.date.accessioned2024-08-04T20:53:07Z
dc.date.available2024-08-04T20:53:07Z
dc.date.issued2022
dc.departmentİnönü Üniversitesien_US
dc.description.abstractContext. As part of our international program aimed at obtaining accurate physical properties of trans-Neptunian objects (TNOs), we predicted a stellar occultation by the TNO (38628) Huya of the star Gaia DR2 4352760586390566400 (m(G) = 11.5 mag) on March 18, 2019. After an extensive observational campaign geared at obtaining the astrometric data, we updated the prediction and found it favorable to central Europe. Therefore, we mobilized half a hundred of professional and amateur astronomers in this region and the occultation was finally detected by 21 telescopes located at 18 sites in Europe and Asia. This places the Huya event among the best ever observed stellar occultation by a TNO in terms of the number of chords. Aims. The aim of our work is to determine an accurate size, shape, and geometric albedo for the TNO (38628) Huya by using the observations obtained from a multi-chord stellar occultation. We also aim to provide constraints on the density and other internal properties of this TNO. Methods. The 21 positive detections of the occultation by Huya allowed us to obtain well-separated chords which permitted us to fit an ellipse for the limb of the body at the moment of the occultation (i.e., the instantaneous limb) with kilometric accuracy. Results. The projected semi-major and minor axes of the best ellipse fit obtained using the occultation data are (a ', b ') = (217.6 +/- 3.5 km, 194.1 +/- 6.1 km) with a position angle for the minor axis of P ' = 55.2 degrees +/- 9.1. From this fit, the projected area-equivalent diameter is 411.0 +/- 7.3 km. This diameter is compatible with the equivalent diameter for Huya obtained from radiometric techniques (D = 406 +/- 16 km). From this instantaneous limb, we obtained the geometric albedo for Huya (p(V) = 0.079 +/- 0.004) and we explored possible three-dimensional shapes and constraints to the mass density for this TNO. We did not detect the satellite of Huya through this occultation, but the presence of rings or debris around Huya was constrained using the occultation data. We also derived an upper limit for a putative Pluto-like global atmosphere of about p(surf) = 10 nbar.en_US
dc.description.sponsorshipSpanish grant (MCIU/AEI/FEDER, UE) [AYA-RTI2018-098657-J-I00]; State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award [SEV2017-0709]; Spanish grant [AYA-2017-84637-R, PID2020-112789GB-I00]; Proyectos de Excelencia de la Junta de Andalucia [2012-FQM1776, PY20-01309]; European Union's Horizon 2020 Research and Innovation Programme, project Small Bodies Near and Far (SBNAF) [687378]; European Research Council under the European Community's H2020 (2014-2020/ERC) [669416]; Romanian National Authority for Scientific Research and Innovation, CNCS - UEFISCDI [PN-III-P1-1.1-TE-2019-1504]; Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior - Brasil (CAPES) [001]; National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq) [465376/2014-2]; CNPq [309578/2017-5, 304544/2017-5, 401903/2016-8, 308150/2016-3, 305917/2019-6, 427700/2018-3, 310683/2017-3, 473002/2013-2, 150612/2020-6]; CAPES; FAPERJ/PAPDRJ [E26/203.173/2016]; Portuguese Foundation for Science and Technology (FCT); European Social Fund (ESF) [SFRH/BD/131700/2017]; Preeminant Postdoctoral Program of the University of Central Florida; National Research, Development and Innovation Office (NKFIH, Hungary) [K-125015, K-138962]; European Union's Horizon 2020 Research and Innovation Programme [871149]; Fundação para a Ciência e a Tecnologia [SFRH/BD/131700/2017] Funding Source: FCT; STFC [ST/T00147X/1] Funding Source: UKRIen_US
dc.description.sponsorshipP.S-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 LEO-SBNAF (MCIU/AEI/FEDER, UE). P.S-S., J.L.O., N.M., M.V-L. and R.D. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofisica de Andalucia (SEV2017-0709), they also acknowledge the financial support by the Spanish grants AYA-2017-84637-R and PID2020-112789GB-I00, and the Proyectos de Excelencia de la Junta de Andalucia 2012-FQM1776 and PY20-01309. The research leading to these results has received funding from the European Union's Horizon 2020 Research and Innovation Programme, under Grant Agreement no. 687378, as part of the project Small Bodies Near and Far (SBNAF). Part of the research leading to these results has received funding from the European Research Council under the European Community's H2020 (2014-2020/ERC Grant Agreement no. 669416 LUCKY STAR). Part of the work of M.P. was financed by a grant of the Romanian National Authority for Scientific Research and Innovation, CNCS - UEFISCDI, PN-III-P1-1.1-TE-2019-1504. This study was financed in part by the Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior -Brasil (CAPES) -Finance Code 001 and the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant 465376/2014-2). The following authors acknowledge the respective CNPq grants: F.B-R 309578/2017-5; R.V.-M. 304544/2017-5, 401903/2016-8; J.I.B.C. 308150/2016-3 and 305917/2019-6; M.A 427700/2018-3, 310683/2017-3 and 473002/2013-2; B.E.M. 150612/2020-6. G.B.R. thanks the support of CAPES and FAPERJ/PAPDRJ (E26/203.173/2016) grant. J.M.O. acknowledges financial support from the Portuguese Foundation for Science and Technology (FCT) and the European Social Fund (ESF) through the PhD grant SFRH/BD/131700/2017. E.F-V. acknowledges funding through the Preeminant Postdoctoral Program of the University of Central Florida. C.K., A.P. and R.S. have been supported by the grants K-125015 and K-138962 of the National Research, Development and Innovation Office (NKFIH, Hungary). E.P. acknowledges the Europlanet 2024 RI project funded by the European Union's Horizon 2020 Research and Innovation Programme (Grant agreement No. 871149). We are grateful to the CAHA and OSN staffs. This research is partially based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by Junta de Andalucia and Consejo Superior de Investigaciones Cientificas (IAA-CSIC). This research was also partially based on observation carried out at the Observatorio de Sierra Nevada (OSN) operated by Instituto de Astrofisica de Andalucia (CSIC). This article is also based on observations made in the Observatorios de Canarias del IAC with the Liverpool Telescope operated on the island of La Palma by the Instituto de Astrofisica de Canarias in the Observatorio del Roque de los Muchachos. Part of the results were based on observations taken at Pico dos Dias Observatory of the National Laboratory of Astrophysics (LNA/Brazil). Part of the data were collected during the photometric monitoring observations with the robotic and remotely controlled observatory at the University of Athens Observatory -UOAO (Gazeas 2016). We thank the Adiyaman University Astrophysics Application and Research Center for their support in the acquisition of data with the ADYU60 telescope. 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.en_US
dc.identifier.doi10.1051/0004-6361/202141546
dc.identifier.issn0004-6361
dc.identifier.issn1432-0746
dc.identifier.scopus2-s2.0-85141325900en_US
dc.identifier.scopusqualityQ1en_US
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202141546
dc.identifier.urihttps://hdl.handle.net/11616/100980
dc.identifier.volume664en_US
dc.identifier.wosWOS:000841954000001en_US
dc.identifier.wosqualityQ1en_US
dc.indekslendigikaynakWeb of Scienceen_US
dc.indekslendigikaynakScopusen_US
dc.language.isoenen_US
dc.publisherEdp Sciences S Aen_US
dc.relation.ispartofAstronomy & Astrophysicsen_US
dc.relation.publicationcategoryMakale - Uluslararası Hakemli Dergi - Kurum Öğretim Elemanıen_US
dc.rightsinfo:eu-repo/semantics/openAccessen_US
dc.subjectKuiper belt objectsen_US
dc.subjectindividualen_US
dc.subjectHuyaen_US
dc.subjectmethodsen_US
dc.subjectobservationalen_US
dc.subjecttechniquesen_US
dc.subjectphotometricen_US
dc.titlePhysical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultationen_US
dc.typeArticleen_US

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