The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar

Recent stellar occultations have allowed accurate instantaneous size and apparent shape determinations of the large Kuiper belt object (50000) Quaoar and the detection of two rings with spatially variable optical depths. In this paper we present new visible range light curve data of Quaoar from the...

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Autores: Kiss, C., Müller, T. G., Marton, G., Szakáts, R., Pál, A., Molnár, L., Vilenius, E., Rengel, M., Ortiz, José Luis, Fernández-Valenzuela, E.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2024
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/370310
Acceso en línea:http://hdl.handle.net/10261/370310
Access Level:acceso abierto
Palabra clave:Kuiper belt objects: individual: (50000) quaoar
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repository_id_str
dc.title.none.fl_str_mv The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
title The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
spellingShingle The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
Kiss, C.
Kuiper belt objects: individual: (50000) quaoar
title_short The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
title_full The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
title_fullStr The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
title_full_unstemmed The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
title_sort The visible and thermal light curve of the large Kuiper belt object (50000) Quaoar
dc.creator.none.fl_str_mv Kiss, C.
Müller, T. G.
Marton, G.
Szakáts, R.
Pál, A.
Molnár, L.
Vilenius, E.
Rengel, M.
Ortiz, José Luis
Fernández-Valenzuela, E.
author Kiss, C.
author_facet Kiss, C.
Müller, T. G.
Marton, G.
Szakáts, R.
Pál, A.
Molnár, L.
Vilenius, E.
Rengel, M.
Ortiz, José Luis
Fernández-Valenzuela, E.
author_role author
author2 Müller, T. G.
Marton, G.
Szakáts, R.
Pál, A.
Molnár, L.
Vilenius, E.
Rengel, M.
Ortiz, José Luis
Fernández-Valenzuela, E.
author2_role author
author
author
author
author
author
author
author
author
dc.contributor.none.fl_str_mv Ministerio de Ciencia e Innovación (España)
Junta de Andalucía
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Kuiper belt objects: individual: (50000) quaoar
topic Kuiper belt objects: individual: (50000) quaoar
description Recent stellar occultations have allowed accurate instantaneous size and apparent shape determinations of the large Kuiper belt object (50000) Quaoar and the detection of two rings with spatially variable optical depths. In this paper we present new visible range light curve data of Quaoar from the Kepler/K2 mission, and thermal light curves at 100 and 160 µm obtained with Herschel/PACS. The K2 data provide a single-peaked period of 8.88 h, very close to the previously determined 8.84 h, and it favours an asymmetric double-peaked light curve with a 17.76 h period. We clearly detected a thermal light curve with relative amplitudes of ~ 10% at 100 and at 160 µm. A detailed thermophysical modelling of the system shows that the measurements can be best fit with a triaxial ellipsoid shape, a volume-equivalent diameter of 1090 km, and axis ratios of a/b = 1.19 and b/c = 1.16. This shape matches the published occultation shape, as well as visual and thermal light curve data. The radiometric size uncertainty remains relatively large (±40 km) as the ring and satellite contributions to the system-integrated flux densities are unknown. In the less likely case of negligible ring or satellite contributions, Quaoar would have a size above 1100 km and a thermal inertia ≤ 10 J m−2K−1s−1/2. A large and dark Weywot in combination with a possible ring contribution would lead to a size below 1080 km in combination with a thermal inertia ≳10 J m−2K−1s−1/2, notably higher than that of smaller Kuiper belt objects with similar albedo and colours. We find that Quaoar’s density is in the range 1.67–1.77 g cm−3, significantly lower than previous estimates. This density value closely matches the relationship observed between the size and density of the largest Kuiper belt objects. © The Authors 2024.
publishDate 2024
dc.date.none.fl_str_mv 2024
2024
2024
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/370310
url http://hdl.handle.net/10261/370310
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
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info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-112789GB-I00
info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2021-001131-S
http://dx.doi.org/10.1051/0004-6361/202348054
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dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
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instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
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spelling The visible and thermal light curve of the large Kuiper belt object (50000) QuaoarKiss, C.Müller, T. G.Marton, G.Szakáts, R.Pál, A.Molnár, L.Vilenius, E.Rengel, M.Ortiz, José LuisFernández-Valenzuela, E.Kuiper belt objects: individual: (50000) quaoarRecent stellar occultations have allowed accurate instantaneous size and apparent shape determinations of the large Kuiper belt object (50000) Quaoar and the detection of two rings with spatially variable optical depths. In this paper we present new visible range light curve data of Quaoar from the Kepler/K2 mission, and thermal light curves at 100 and 160 µm obtained with Herschel/PACS. The K2 data provide a single-peaked period of 8.88 h, very close to the previously determined 8.84 h, and it favours an asymmetric double-peaked light curve with a 17.76 h period. We clearly detected a thermal light curve with relative amplitudes of ~ 10% at 100 and at 160 µm. A detailed thermophysical modelling of the system shows that the measurements can be best fit with a triaxial ellipsoid shape, a volume-equivalent diameter of 1090 km, and axis ratios of a/b = 1.19 and b/c = 1.16. This shape matches the published occultation shape, as well as visual and thermal light curve data. The radiometric size uncertainty remains relatively large (±40 km) as the ring and satellite contributions to the system-integrated flux densities are unknown. In the less likely case of negligible ring or satellite contributions, Quaoar would have a size above 1100 km and a thermal inertia ≤ 10 J m−2K−1s−1/2. A large and dark Weywot in combination with a possible ring contribution would lead to a size below 1080 km in combination with a thermal inertia ≳10 J m−2K−1s−1/2, notably higher than that of smaller Kuiper belt objects with similar albedo and colours. We find that Quaoar’s density is in the range 1.67–1.77 g cm−3, significantly lower than previous estimates. This density value closely matches the relationship observed between the size and density of the largest Kuiper belt objects. © The Authors 2024.PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). This work was partly supported by the K-138962 and the ‘SeismoLab’ KKP-137523 Élvonal grants of the National Research, Development and Innovation Office (NKFIH, Hungary). G.M. acknowledges support by the János Bolyai Research Scholarship of the Hungarian Academy of Sciences. Part of this work was supported by the German DLR project number 50 OR 1108. Part of this work was supported by the Spanish projects PID2020-112789GB-I00 from AEI and Proyecto de Excelencia de la Junta de Andalucía PY20-01309. Financial support from the grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033 is also acknowledged. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the NASA Science Mission Directorate.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewedEDP SciencesMinisterio de Ciencia e Innovación (España)Junta de AndalucíaConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202420242024info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/370310reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-112789GB-I00info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/CEX2021-001131-Shttp://dx.doi.org/10.1051/0004-6361/202348054Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3703102026-05-22T06:33:51Z
score 15,81155

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