M. Kretlow, J. L. Ortiz, J. Desmars, N. Morales, F. L. Rommel, P. Santos-Sanz, M. Vara-Lubiano, E. Fernández-Valenzuela, A. Alvarez-Candal, R. Duffard, F. Braga-Ribas, B. Sicardy, A. Castro-Tirado, E. J. Fernández-García, M. Sánchez, A. Sota, M. Assafin, G. Benedetti-Rossi, R. Boufleur, J. I. B. Camargo, S. Cikota, A. Gomes-Junior, J. M. Gómez-Limón, Y. Kilic, J. Lecacheux, R. Leiva, J. Marques-Oliveira, R. Morales, B. Morgado, J. L. Rizos, F. Roques, D. Souami, R. Vieira-Martins, M. R. Alarcon, R. Boninsegna, O. Çakır, F. Casarramona, J. J. Castellani, I. de la Cueva, S. Fişek, A. Guijarro, T. Haymes, E. Jehin, S. Kidd, J. Licandro, J. L. Maestre, F. Murgas, E. Pallé, M. Popescu, A. Pratt, M. Serra-Ricart, J. C. Talbot
{"title":"根据恒星掩星和光度观测得出的跨海王星天体（143707）2003 UY117的物理特性","authors":"M. Kretlow, J. L. Ortiz, J. Desmars, N. Morales, F. L. Rommel, P. Santos-Sanz, M. Vara-Lubiano, E. Fernández-Valenzuela, A. Alvarez-Candal, R. Duffard, F. Braga-Ribas, B. Sicardy, A. Castro-Tirado, E. J. Fernández-García, M. Sánchez, A. Sota, M. Assafin, G. Benedetti-Rossi, R. Boufleur, J. I. B. Camargo, S. Cikota, A. Gomes-Junior, J. M. Gómez-Limón, Y. Kilic, J. Lecacheux, R. Leiva, J. Marques-Oliveira, R. Morales, B. Morgado, J. L. Rizos, F. Roques, D. Souami, R. Vieira-Martins, M. R. Alarcon, R. Boninsegna, O. Çakır, F. Casarramona, J. J. Castellani, I. de la Cueva, S. Fişek, A. Guijarro, T. Haymes, E. Jehin, S. Kidd, J. Licandro, J. L. Maestre, F. Murgas, E. Pallé, M. Popescu, A. Pratt, M. Serra-Ricart, J. C. Talbot","doi":"10.1051/0004-6361/202451329","DOIUrl":null,"url":null,"abstract":"<i>Context<i/>. Trans-Neptunian objects (TNOs) are considered to be among the most primitive objects in our Solar System. Knowledge of their primary physical properties is essential for understanding their origin and the evolution of the outer Solar System. In this context, stellar occultations are a powerful and sensitive technique for studying these distant and faint objects.<i>Aims<i/>. We aim to obtain the size, shape, absolute magnitude, and geometric albedo for TNO (143707) 2003 UY<sub>117<sub/>.<i>Methods<i/>. We predicted a stellar occultation by this TNO for 2020 October 23 UT and ran a specific campaign to investigate this event. We derived the projected profile shape and size from the occultation observations by means of an elliptical fit to the occultation chords. We also performed photometric observations of (143707) 2003 UY<sub>117<sub/> to obtain the absolute magnitude and the rotational period from the observed rotational light curve. Finally, we combined these results to derive the three-dimensional shape, volume-equivalent diameter, and geometric albedo for this TNO.<i>Results<i/>. From the stellar occultation, we obtained a projected ellipse with axes of (282 ± 18) × (184 ± 32) km. The area-equivalent diameter for this ellipse is <i>D<i/><sub>eq,A<sub/> = 228 ± 21 km. From our photometric <i>R<i/> band observations, we derived an absolute magnitude of <i>H<i/><sub><i>V<i/><sub/> = 5.97 ± 0.07 mag using <i>V<i/> − <i>R<i/> = 0.46 ± 0.07 mag, which was derived from a <i>V<i/> band subset of these data. The rotational light curve has a peak-to-valley amplitude of <i>∆m<i/> = 0.36 ± 0.13 mag. We find the most likely rotation period to be <i>P<i/> = 12.376 ± 0.0033 hours. By combining the occultation with the rotational light curve results and assuming a triaxial ellipsoid, we derived axes of <i>a<i/> × <i>b<i/> × <i>c<i/> = (332 ± 24) km × (216 ± 24) km × (180<sub>−24<sub/><sup>+28<sup/>) km for this ellipsoid, and therefore a volume-equivalent diameter of <i>D<i/><sub>eq,V<sub/> = 235 ± 25 km. Finally, the values for the absolute magnitude and for the area-equivalent diameter yield a geometric albedo of <i>p<i/><sub><i>V<i/><sub/> = 0.139 ± 0.027.","PeriodicalId":8571,"journal":{"name":"Astronomy & Astrophysics","volume":"121 1","pages":""},"PeriodicalIF":5.4000,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"title\":\"Physical properties of trans-Neptunian object (143707) 2003 UY117 derived from stellar occultation and photometric observations\",\"authors\":\"M. Kretlow, J. L. Ortiz, J. Desmars, N. Morales, F. L. Rommel, P. Santos-Sanz, M. Vara-Lubiano, E. Fernández-Valenzuela, A. Alvarez-Candal, R. Duffard, F. Braga-Ribas, B. Sicardy, A. Castro-Tirado, E. J. Fernández-García, M. Sánchez, A. Sota, M. Assafin, G. Benedetti-Rossi, R. Boufleur, J. I. B. Camargo, S. Cikota, A. Gomes-Junior, J. M. Gómez-Limón, Y. Kilic, J. Lecacheux, R. Leiva, J. Marques-Oliveira, R. Morales, B. Morgado, J. L. Rizos, F. Roques, D. Souami, R. Vieira-Martins, M. R. Alarcon, R. Boninsegna, O. Çakır, F. Casarramona, J. J. Castellani, I. de la Cueva, S. Fişek, A. Guijarro, T. Haymes, E. Jehin, S. Kidd, J. Licandro, J. L. Maestre, F. Murgas, E. Pallé, M. Popescu, A. Pratt, M. Serra-Ricart, J. C. Talbot\",\"doi\":\"10.1051/0004-6361/202451329\",\"DOIUrl\":null,\"url\":null,\"abstract\":\"<i>Context<i/>. Trans-Neptunian objects (TNOs) are considered to be among the most primitive objects in our Solar System. Knowledge of their primary physical properties is essential for understanding their origin and the evolution of the outer Solar System. In this context, stellar occultations are a powerful and sensitive technique for studying these distant and faint objects.<i>Aims<i/>. We aim to obtain the size, shape, absolute magnitude, and geometric albedo for TNO (143707) 2003 UY<sub>117<sub/>.<i>Methods<i/>. We predicted a stellar occultation by this TNO for 2020 October 23 UT and ran a specific campaign to investigate this event. We derived the projected profile shape and size from the occultation observations by means of an elliptical fit to the occultation chords. We also performed photometric observations of (143707) 2003 UY<sub>117<sub/> to obtain the absolute magnitude and the rotational period from the observed rotational light curve. Finally, we combined these results to derive the three-dimensional shape, volume-equivalent diameter, and geometric albedo for this TNO.<i>Results<i/>. From the stellar occultation, we obtained a projected ellipse with axes of (282 ± 18) × (184 ± 32) km. The area-equivalent diameter for this ellipse is <i>D<i/><sub>eq,A<sub/> = 228 ± 21 km. From our photometric <i>R<i/> band observations, we derived an absolute magnitude of <i>H<i/><sub><i>V<i/><sub/> = 5.97 ± 0.07 mag using <i>V<i/> − <i>R<i/> = 0.46 ± 0.07 mag, which was derived from a <i>V<i/> band subset of these data. The rotational light curve has a peak-to-valley amplitude of <i>∆m<i/> = 0.36 ± 0.13 mag. We find the most likely rotation period to be <i>P<i/> = 12.376 ± 0.0033 hours. By combining the occultation with the rotational light curve results and assuming a triaxial ellipsoid, we derived axes of <i>a<i/> × <i>b<i/> × <i>c<i/> = (332 ± 24) km × (216 ± 24) km × (180<sub>−24<sub/><sup>+28<sup/>) km for this ellipsoid, and therefore a volume-equivalent diameter of <i>D<i/><sub>eq,V<sub/> = 235 ± 25 km. Finally, the values for the absolute magnitude and for the area-equivalent diameter yield a geometric albedo of <i>p<i/><sub><i>V<i/><sub/> = 0.139 ± 0.027.\",\"PeriodicalId\":8571,\"journal\":{\"name\":\"Astronomy & Astrophysics\",\"volume\":\"121 1\",\"pages\":\"\"},\"PeriodicalIF\":5.4000,\"publicationDate\":\"2024-10-25\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"Astronomy & Astrophysics\",\"FirstCategoryId\":\"101\",\"ListUrlMain\":\"https://doi.org/10.1051/0004-6361/202451329\",\"RegionNum\":2,\"RegionCategory\":\"物理与天体物理\",\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"Q1\",\"JCRName\":\"ASTRONOMY & ASTROPHYSICS\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"Astronomy & Astrophysics","FirstCategoryId":"101","ListUrlMain":"https://doi.org/10.1051/0004-6361/202451329","RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"Q1","JCRName":"ASTRONOMY & ASTROPHYSICS","Score":null,"Total":0}
引用次数: 0
摘要
背景。跨海王星天体（TNOs）被认为是太阳系中最原始的天体之一。了解它们的主要物理特性对于了解它们的起源和外太阳系的演变至关重要。在这方面，恒星掩星是研究这些遥远而暗淡天体的一种强大而灵敏的技术。我们的目的是获得TNO (143707) 2003 UY117的大小、形状、绝对星等和几何反照率。我们预测了 2020 年 10 月 23 日（世界标准时间）这颗 TNO 将发生恒星掩星现象，并开展了一次专门的活动来研究这一事件。我们通过对掩星弦的椭圆拟合，从掩星观测中得出了预计的轮廓形状和大小。我们还对 (143707) 2003 UY117 进行了光度观测，从观测到的旋转光曲线中获得了绝对星等和旋转周期。最后，我们将这些结果结合起来，得出了这颗尘埃落定星的三维形状、体积当量直径和几何反照率。通过恒星掩星，我们得到了一个轴线为 (282 ± 18) × (184 ± 32) km 的投影椭圆。该椭圆的面积等效直径为 Deq,A = 228 ± 21 千米。从我们的 R 波段光度观测数据中，我们得出了 HV = 5.97 ± 0.07 等的绝对星等，使用的是 V - R = 0.46 ± 0.07 等的绝对星等，这是从这些数据的 V 波段子集中得出的。旋转光曲线的峰谷振幅为 ∆m = 0.36 ± 0.13 等。我们发现最有可能的自转周期是 P = 12.376 ± 0.0033 小时。结合掩星和自转光变曲线的结果，并假设椭球体为三轴，我们得出该椭球体的轴线为 a × b × c = (332 ± 24) km × (216 ± 24) km × (180-24+28) km，因此其体积当量直径为 Deq,V = 235 ± 25 km。最后，根据绝对大小和面积等效直径的数值，得出几何反照率 pV = 0.139 ± 0.027。
Physical properties of trans-Neptunian object (143707) 2003 UY117 derived from stellar occultation and photometric observations
Context. Trans-Neptunian objects (TNOs) are considered to be among the most primitive objects in our Solar System. Knowledge of their primary physical properties is essential for understanding their origin and the evolution of the outer Solar System. In this context, stellar occultations are a powerful and sensitive technique for studying these distant and faint objects.Aims. We aim to obtain the size, shape, absolute magnitude, and geometric albedo for TNO (143707) 2003 UY117.Methods. We predicted a stellar occultation by this TNO for 2020 October 23 UT and ran a specific campaign to investigate this event. We derived the projected profile shape and size from the occultation observations by means of an elliptical fit to the occultation chords. We also performed photometric observations of (143707) 2003 UY117 to obtain the absolute magnitude and the rotational period from the observed rotational light curve. Finally, we combined these results to derive the three-dimensional shape, volume-equivalent diameter, and geometric albedo for this TNO.Results. From the stellar occultation, we obtained a projected ellipse with axes of (282 ± 18) × (184 ± 32) km. The area-equivalent diameter for this ellipse is Deq,A = 228 ± 21 km. From our photometric R band observations, we derived an absolute magnitude of HV = 5.97 ± 0.07 mag using V − R = 0.46 ± 0.07 mag, which was derived from a V band subset of these data. The rotational light curve has a peak-to-valley amplitude of ∆m = 0.36 ± 0.13 mag. We find the most likely rotation period to be P = 12.376 ± 0.0033 hours. By combining the occultation with the rotational light curve results and assuming a triaxial ellipsoid, we derived axes of a × b × c = (332 ± 24) km × (216 ± 24) km × (180−24+28) km for this ellipsoid, and therefore a volume-equivalent diameter of Deq,V = 235 ± 25 km. Finally, the values for the absolute magnitude and for the area-equivalent diameter yield a geometric albedo of pV = 0.139 ± 0.027.
期刊介绍：
Astronomy & Astrophysics is an international Journal that publishes papers on all aspects of astronomy and astrophysics (theoretical, observational, and instrumental) independently of the techniques used to obtain the results.
京公网安备 11010802042870号
京ICP备2023020795号-1
分享
求助内容：
应助结果提醒方式：
扫码关注我们
