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117 results on '"Morgado, B E"'

1. Constraints on Triton atmospheric evolution from occultations: 1989-2022

Author: Sicardy, B., Tej, A., Gomes-Junior, A. R., Romanov, F. D., Bertrand, T., Ashok, N. M., Lellouch, E., Morgado, B. E., Assafin, M., Desmars, J., Camargo, J. I. B., Kilic, Y., Ortiz, J. L., Vieira-Martins, R., Braga-Ribas, F., Ninan, J. P., Bhatt, B. C., Kumar, S. Pramod, Swain, V., Sharma, S., Saha, A., Ojha, D. K., Pawar, G., Deshmukh, S., Deshpande, A., Ganesh, S., Jain, J. K., Mathew, S. K., Kumar, H., Bhalerao, V., Anupama, G. C., Barway, S., Brandeker, A., Floren, H. G., Olofsson, G., Bruno, G., Mao, Y. M., Ye, R. H., Zou, Q. Y., Sun, Y. K., Shen, Y. Y., Zhao, J. Y., Grishin, D. N., Romanova, L. V., Marchis, F., Fukui, K., Kukita, R., Benedetti-Rossi, G., Santos-Sanz, P., Dhyani, N., Gokhale, A., and Kate, A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Context - Around the year 2000, Triton's south pole experienced an extreme summer solstice that occurs every about 650 years, when the subsolar latitude reached about 50{\deg}. Bracketing this epoch, a few occultations probed Triton's atmosphere in 1989, 1995, 1997, 2008 and 2017. A recent ground-based stellar occultation observed on 6 October 2022 provides a new measurement of Triton's atmospheric pressure which is presented here. Aims- The goal is to constrain the Volatile Transport Models (VTMs) of Triton's atmosphere that is basically in vapor pressure equilibrium with the nitrogen ice at its surface. Methods - Fits to the occultation light curves yield Triton's atmospheric pressure at the reference radius 1400 km, from which the surface pressure is induced. Results - The fits provide a pressure p_1400= 1.211 +/- 0.039 microbar at radius 1400 km (47 km altitude), from which a surface pressure of p_surf= 14.54 +/- 0.47 microbar is induced (1-sigma error bars). To within error bars, this is identical to the pressure derived from the previous occultation of 5 October 2017, p_1400 = 1.18 +/- 0.03 microbar and p_surf= 14.1 +/- 0.4 microbar, respectively. Based on recent models of Triton's volatile cycles, the overall evolution over the last 30 years of the surface pressure is consistent with N2 condensation taking place in the northern hemisphere. However, models typically predict a steady decrease in surface pressure for the period 2005-2060, which is not confirmed by this observation. Complex surface-atmosphere interactions, such as ice albedo runaway and formation of local N2 frosts in the equatorial regions of Triton could explain the relatively constant pressure between 2017 and 2022., Comment: 8 pages, 4 figures, accepted for publication in Astronomy and Astrophysics
Published: 2024

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

Author: 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., Asai, A., Colazo, C., Ducrot, E., Duffard, R., Fabrega, J., Fernandez-Valenzuela, E., Gillon, M., Horaguchi, T., Ida, M., Kitazaki, K., Mammana, L. A., Maury, A., Melita, M., Morales, N., Moya-Sierralta, C., Owada, M., Pollock, J., Sanchez, J. L., Santos-Sanz, P., Sasanuma, N., Sebastian, D., Triaud, A., Uchiyama, S., Vanzi, L., Watanabe, H., and Yamamura, H.
Subjects: Astrophysics - Earth and Planetary Astrophysics
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 $\tau$ = 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 $a = 37.0\pm0.6$ km, $b = 28.4 \pm 0.5$ km, and $c= 24.9 \pm 0.4$ km, resulting in an area-equivalent radius of $30.0 \pm 0.5$ km. Using the projected limb at the occultation epoch and the available absolute magnitude ($\rm{H}_{\rm{v}} = 9.971 \pm 0.031$), we calculate an albedo of $p_{\rm{v}} = 0.050 \pm 0.003$. Constraints on the object's density and internal friction are also proposed., Comment: Accepted for publication on MNRAS
Published: 2023

3. Kilometer-precise (UII) Umbriel physical properties from the multichord stellar occultation on 2020 September 21

Author: Assafin, M., Santos-Filho, S., Morgado, B. E., Gomes-Júnior, A. R., Sicardy, B., Margoti, G., Benedetti-Rossi, G., Braga-Ribas, F., Laidler, T., Camargo, J. I. B., Vieira-Martins, R., Swift, T., Dunham, D., George, T., Bardecker, J., Anderson, C., Nolthenius, R., Bender, K., Viscome, G., Oesper, D., Dunford, R., Getrost, K., Kitting, C., Green, K., Bria, R., Olsen, A., Scheck, A., Billard, B., Wasiuta, M. E., Tatum, R., Maley, P., di Cicco, D., Gamble, D., Ceravolo, P., Ceravolo, D., Hanna, W., Smith, N., Carlson, N., Messner, S., Bean, J., Moore, J., and Venable, R.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We report the results of the stellar occultation by (UII) Umbriel on September 21st, 2020. The shadow crossed the USA and Canada, and 19 positive chords were obtained. A limb parameter accounted for putative topographic features in the limb fittings. Ellipse fittings were not robust - only upper limits were derived for the true size/shape of a putative Umbriel ellipsoid. The adopted spherical solution gives radius = 582.4 +/- 0.8 km, smaller/close to 584.7 +/- 2.8 km from Voyager II. The apparent ellipse fit results in a true semi-major axis of 584.9 +/- 3.8 km, semi-minor axes of 582.3 +/- 0.6 km and true oblateness of 0.004 +/- 0.008 for a putative ellipsoid. The geometric albedo was pV = 0.26 +/- 0.01. The density was rho = 1.54 +/- 0.04 g cm-3. The surface gravity was 0.251 +/- 0.006 m s-2 and the escape velocity 0.541 +/- 0.006 km s-1 . Upper limits of 13 and 72 nbar (at 1 sigma and 3 sigma levels, respectively) were obtained for the surface pressure of a putative isothermal CO2 atmosphere at T = 70 K. A milliarcsecond precision position was derived: RA = 02h 30m 28.84556s +/- 0.1 mas, DE = 14o 19' 36.5836" +/- 0.2 mas. A large limb parameter of 4.2 km was obtained, in striking agreement with opposite southern hemisphere measurements by Voyager II in 1986. Occultation and Voyager results indicate that the same strong topography variation in the surface of Umbriel is present on both hemispheres.
Published: 2023
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4. The 2021 mutual phenomena involving the Galilean satellites of Jupiter and the inner satellite Thebe

Author: Catani, L. M., Assafin, M., Morgado, B. E., Santos-Filho, S., Braga-Ribas, F., Vieira-Martins, R., Arcas-Silva, J., Milone, A. C., Lima, I. J., and Botelho, R. B.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Astrometric studies and orbital modeling of planetary moons have contributed significantly to advancing our understanding of their orbital dynamics. These studies require precise positions measured over extended periods. In this paper, we present the results of the 2021 Brazilian Jovian mutual phenomena campaign. The data correspond to eight events between Galilean satellites, in addition to a rare eclipse of Thebe, an inner satellite, totaling nine events. A geometric model along with the DE440/JUP365 ephemerides was used to reproduce the events and simulate the light curves. A Monte Carlo method and chi-squared statistics were used to fit the simulated light curves to the observations. The reflectance model adopted for our simulations was the complete version of the Oren-Nayer model. The average uncertainty of the relative positions of the Galilean satellites was 5 mas (15 km) and for the inner Thebe satellite 32 mas (96 km). The seven mutual events (nine independent observations) here analyzed represent and addition of 17% events (10% light curves) with respect to the PHEMU21 international campaign. Furthermore, our result of Thebe eclipse is only the second measurement published to date. Our results contribute to the ephemeris database, being fundamental to improving satellite orbits and thus minimizing their uncertainties., Comment: 10 pages, 5 figures
Published: 2023
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5. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS$_4$ measured from stellar occultations

Author: Rommel, F. L., Braga-Ribas, F., Ortiz, J. L., Sicardy, B., Santos-Sanz, P., Desmars, J., Camargo, J. I. B., Vieira-Martins, R., Assafin, M., Morgado, B. E., Boufleur, R. C., Benedetti-Rossi, G., Gomes-Júnior, A. R., Fernández-Valenzuela, E., Holler, B. J., Souami, D., Duffard, R., Margoti, G., Vara-Lubiano, M., Lecacheux, J., Plouvier, J. L., Morales, N., Maury, A., Fabrega, J., Ceravolo, P., Jehin, E., Albanese, D., Mariey, H., Cikota, S., Ruždjak, D., Cikota, A., Szakáts, R., Aissa, D. Baba, Gringahcene, Z., Kashuba, V., Koshkin, N., Zhukov, V., Fişek, S., Çakır, O., Özer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, T., Pereira, C. L., Emilio, M., Burdanov, A. Y., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Sanchez, R. Zanmar, Tagliaferri, U., Di Sora, M., Isopi, G., Krugly, Y., Slyusarev, I., Chiorny, V., Mikuž, H., Bacci, P., Maestripieri, M., Grazia, M. D., de la Cueva, I., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O. M., Serra-Ricart, M., Alarcon, M. R., Licandro, J., Masi, G., Bacci, R., Bosch, J. M., Behem, R., Prost, J. -P., Renner, S., Conjat, M., Bachini, M., Succi, G., Stoian, L., Juravle, A., Carosati, D., Gowe, B., Carrillo, J., Zheleznyak, A. P., Montigiani, N., Foster, C. R., Mannucci, M., Ruocco, N., Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Collins, M., Pál, A., Csák, B., Fernández-Garcia, E., Castro-Tirado, A. J., Hudin, L., Madiedo, J. M., Anghel, R. M., Calvo-Fernández, J. F., Valvasori, A., Guido, E., Gherase, R. M., Kamoun, S., Fafet, R., Sánchez-González, M., Curelaru, L., Vîntdevară, C. D., Danescu, C. A., Gout, J. -F., Schmitz, C. J., Sota, A., Belskaya, I., Rodríguez-Marco, M., Kilic, Y., Frappa, E., Klotz, A., Lavayssière, M., Oliveira, J. Marques, Popescu, M., Mammana, L. A., Fernández-Lajús, E., Schmidt, M., Hopp, U., Komžík, R., Pribulla, T., Tomko, D., Husárik, M., Erece, O., Eryilmaz, S., Buzzi, L., Gährken, B., Nardiello, D., Hornoch, K., Sonbas, E., Er, H., Burwitz, V., Sybilski, P. Waldemar, Bykowski, W., Müller, T. G., Ogloza, W., Gonçalves, R., Ferreira, J. F., Ferreira, M., Bento, M., Meister, S., Bagiran, M. N., Tekeş, M., Marciniak, A., Moravec, Z., Delinčák, P., Gianni, G., Casalnuovo, G. B., Boutet, M., Sanchez, J., Klemt, B., Wuensche, N., Burzynski, W., Borkowski, M., Serrau, M., Dangl, G., Klös, O., Weber, C., Urbaník, M., Rousselot, L., Kubánek, J., André, P., Colazo, C., Spagnotto, J., Sickafoose, A. A., Hueso, R., Sánchez-Lavega, A., Fisher, R. S., Rengstorf, A. W., Perelló, C., Dascalu, M., Altan, M., Gazeas, K., de Santana, T., Sfair, R., Winter, O. C., Kalkan, S., Canales-Moreno, O., Trigo-Rodríguez, J. M., Tsamis, V., Tigani, K., Sioulas, N., Lekkas, G., Bertesteanu, D. N., Dumitrescu, V., Wilberger, A. J., Barnes, J. W., Fieber-Beyer, S. K., Swaney, R. L., Fuentes, C., Mendez, R. A., Dumitru, B. D., Flynn, R. L., and Wake, D. A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: This work aims at constraining the size, shape, and geometric albedo of the dwarf planet candidate 2002 MS4 through the analysis of nine stellar occultation events. Using multichord detection, we also studied the object's topography by analyzing the obtained limb and the residuals between observed chords and the best-fitted ellipse. 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 three to up to sixty-one positive chords. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS4. The best-fitted ellipse, combined with the object's rotational information from the literature, constrains the object's size, shape, and albedo. Additionally, we developed a new method to characterize topography features on the object's limb. The global limb has a semi-major axis of 412 $\pm$ 10 km, a semi-minor axis of 385 $\pm$ 17 km, and the position angle of the minor axis is 121 $^\circ$ $\pm$ 16$^\circ$. From this instantaneous limb, we obtained 2002 MS4's geometric albedo and the projected area-equivalent diameter. Significant deviations from the fitted ellipse in the northernmost limb are detected from multiple sites highlighting three distinct topographic features: one 11 km depth depression followed by a 25$^{+4}_{-5}$ km height elevation next to a crater-like depression with an extension of 322 $\pm$ 39 km and 45.1 $\pm$ 1.5 km deep. Our results present an object that is $\approx$138 km smaller in diameter than derived from thermal data, possibly indicating the presence of a so-far unknown satellite. However, within the error bars, the geometric albedo in the V-band agrees with the results published in the literature, even with the radiometric-derived albedo.
Published: 2023
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6. The changing material around (2060) Chiron from an occultation on 2022 December 15

Author: Ortiz, J. L., Pereira, C. L., Sicardy, B., Braga-Ribas, F., Takey, A., Fouad, A. M., Shaker, A. A., Kaspi, S., Brosch, N., Kretlow, M., Leiva, R., Desmars, J., Morgado, B. E., Morales, N., Vara-Lubiano, M., Santos-Sanz, P., Fernández-Valenzuela, E., Souami, D., Duffard, R., Rommel, F. L., Kilic, Y., Erece, O., Koseoglu, D., Ege, E., Morales, R., Alvarez-Candal, A., Rizos, J. L., Gómez-Limón, J. M., Assafin, M., Vieira-Martins, R., Gomes-Júnior, A. R., Camargo, J. I. B., and Lecacheux, J.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We could accurately predict the shadow path and successfully observe an occultation of a bright star by Chiron on 2022 December 15. The Kottamia Astronomical Observatory in Egypt did not detect the occultation by the solid body, but we detected three extinction features in the light curve that had symmetrical counterparts with respect to the central time of the occultation. One of the features is broad and shallow, whereas the other two features are sharper with a maximum extinction of $\sim$25$\%$ at the achieved spatial resolution of 19 km per data point. From the Wise observatory in Israel, we detected the occultation caused by the main body and several extinction features surrounding the body. When all the secondary features are plotted in the sky plane we find that they can be caused by a broad $\sim$580 km disk with concentrations at radii of 325 \pm 16 km and 423 \pm 11 km surrounding Chiron. At least one of these structures appears to be outside the Roche limit. The ecliptic coordinates of the pole of the disk are $\lambda$ = 151$^\circ~\pm$ 8$^\circ$ and $\beta$ = 18$^\circ~\pm$ 11$^\circ$, in agreement with previous results. We also show our long-term photometry indicating that Chiron had suffered a brightness outburst of at least 0.6 mag between March and September 2021 and that Chiron was still somewhat brighter at the occultation date than at its nominal pre-outburst phase. The outermost extinction features might be consistent with a bound or temporarily bound structure associated with the brightness increase. However, the nature of the brightness outburst is unclear, and it is also unclear whether the dust or ice released in the outburst could be feeding a putative ring structure or if it emanated from it., Comment: 6 pages, 4, figures
Published: 2023
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7. The two rings of (50000) Quaoar

Author: Pereira, C. L., Sicardy, B., Morgado, B. E., Braga-Ribas, F., Fernández-Valenzuela, E., Souami, D., Holler, B. J., Boufleur, R. C., Margoti, G., Assafin, M., Ortiz, J. L., Santos-Sanz, P., Epinat, B., Kervella, P., Desmars, J., Vieira-Martins, R., Kilic, Y., Gomes-Júnior, A. R., Camargo, J. I. B., Emilio, M., Vara-Lubiano, M., Kretlow, M., Albert, L., Alcock, C., Ball, J. G., Bender, K., Buie, M. W., Butterfield, K., Camarca, M., Castro-Chacón, J. H., Dunford, R., Fisher, R. S., Gamble, D., Geary, J. C., Gnilka, C. L., Green, K. D., Hartman, Z. D., Huang, C-K., Januszewski, H., Johnston, J., Kagitani, M., Kamin, R., Kavelaars, J. J., Keller, J. M., de Kleer, K. R., Lehner, M. J., Luken, A., Marchis, F., Marlin, T., McGregor, K., Nikitin, V., Nolthenius, R., Patrick, C., Redfield, S., Rengstorf, A. W., Reyes-Ruiz, M., Seccull, T., Skrutskie, M. F., Smith, A. B., Sproul, M., Stephens, A. W., Szentgyorgyi, A., Sánchez-Sanjuán, S., Tatsumi, E., Verbiscer, A., Wang, S-Y., Yoshida, F., Young, R., and Zhang, Z-W.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Quaoar is a classical Trans-Neptunian Object (TNO) with an area equivalent diameter of 1,100 km and an orbital semi-major axis of 43.3 astronomical units. Based on stellar occultations observed between 2018 and 2021, an inhomogeneous ring (Q1R, Quaoar's first ring) was detected around this body. Aims. A new stellar occultation by Quaoar was observed on August 9th, 2022 aiming to improve Quaoar's shape models and the physical parameters of Q1R while searching for additional material around the body. Methods. The occultation provided nine effective chords across Quaoar, pinning down its size, shape, and astrometric position. Large facilities, such as Gemini North and the Canada-France-Hawaii Telescope (CFHT), were used to obtain high acquisition rates and signal-to-noise ratios. The light curves were also used to characterize the Q1R ring (radial profiles and orbital elements). Results. Quaoar's elliptical fit to the occultation chords yields the limb with an apparent semi-major axis of $579.5\pm4.0$ km, apparent oblateness of $0.12\pm0.01$, and area-equivalent radius of $543\pm2$ km. Quaoar's limb orientation is consistent with Q1R and Weywot orbiting in Quaoar's equatorial plane. The orbital radius of Q1R is refined to a value of $4,057\pm6$ km. The radial opacity profile of the more opaque ring profile follows a Lorentzian shape that extends over 60 km, with a full width at half maximum (FWHM) of $\sim5$ km and a peak normal optical depth of 0.4. Besides the secondary events related to the already reported rings, new secondary events detected during the August 2022 occultation in three different data sets are consistent with another ring around Quaoar with a radius of $2,520\pm20$ km, assuming the ring is circular and co-planar with Q1R. This new ring has a typical width of 10 km and a normal optical depth of $\sim$0.004. Like Q1R, it also lies outside Quaoar's classical Roche limit., Comment: Accepted for publication in Astronomy & Astrophysics (17-April-2023). 18 pages, 12 figures
Published: 2023
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8. A stellar occultation by the transneptunian object (50000) Quaoar observed by CHEOPS

Author: Morgado, B. E., Bruno, G., Gomes-Júnior, A. R., Pagano, I., Sicardy, B., Fortier, A., Desmars, J., Maxted, P. F. L., Braga-Ribas, F., Queloz, D., Sousa, S. G., Ortiz, J. L., Brandeker, A., Cameron, A. Collier, Pereira, C. L., Florén, H. G., Hara, N., Souami, D., Isaak, K. G., Olofsson, G., Santos-Sanz, P., Wilson, T. G., Broughton, J., Alibert, Y., Alonso, R., Anglada, G., Bárczy, T., Barrado, D., Barros, S. C. C., Baumjohann, W., Beck, M., Beck, T., Benz, W., Billot, N., Bonfils, X., Broeg, C., Cabrera, J., Charnoz, S., Csizmadia, S., Davies, M. B., Deleuil, M., Delrez, L., Demangeon, O. D. S., Demory, B. O., Ehrenreich, D., Erikson, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Güdel, M., Heng, K., Hoyer, S., Kiss, L. L., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Lovis, C., Magrin, D., Marafatto, L., Nascimbeni, V., Ottensamer, R., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Ragazzoni, R., Rando, N., Ratti, F., Rauer, H., Reimers, C., Ribas, I., Santos, N. C., Scandariato, G., Ségransan, D., Simon, A. E., Smith, A. M. S., Steller, M., Szabó, G. M., Thomas, N., Udry, S., Van Grootel, V., Walton, N. A., and Westerdorff, K.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Stellar occultation is a powerful technique that allows the determination of some physical parameters of the occulting object. The result depends on the photometric accuracy, the temporal resolution, and the number of chords obtained. Space telescopes can achieve high photometric accuracy as they are not affected by atmospheric scintillation. Using ESA's CHEOPS space telescope, we observed a stellar occultation by the Transneptunian object (50000) Quaoar. We compare the obtained chord with previous occultations by this object and determine its astrometry with sub-milliarcsecond precision. Also, we determine upper limits to the presence of a global methane atmosphere on the occulting body. We predicted and observed a stellar occultation by Quaoar using the CHEOPS space telescope. We measured the occultation light curve from this data-set and determined the dis- and re-appearance of the star behind the occulting body. Furthermore, a ground-based telescope in Australia was used to constrain Quaoar's limb. Combined with results from previous works, these measurements allow us to obtain a precise position of Quaoar at the occultation time. We present results obtained from the first stellar occultation by a Transneptunian object (TNO) using space telescope orbiting Earth. It was the occultation by Quaoar observed on 2020 June 11. We used the CHEOPS light curve to obtain a surface pressure upper limit of 85 nbar for the detection of a global methane atmosphere. Also, combining this observation with a ground-based observation we fit Quaoar's limb to determine its astrometric position with an uncertainty below 1.0 mas. This observation is a first of its kind, and it shall be considered as a proof of concept of stellar occultation observations of Transneptunian objects with space telescopes orbiting Earth. Moreover, it shows significant prospects for the James Webb Space Telescope., Comment: 9 pages, 10 figures
Published: 2022
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9. Occultation Portal: a web-based platform for data collection and analysis of stellar occultations

Author: Kilic, Y., Braga-Ribas, F., Kaplan, M., Erece, O., Souami, D., Dindar, M., Desmars, J., Sicardy, B., Morgado, B. E., Shameoni, M. N., Rommel, F. L., and Gomes-Júnior, A. R.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Recording a stellar occultation is one powerful method that gives direct information about the physical properties of the occulting solar system object. In order to obtain reliable and accurate results, simultaneous observations from different locations across-track of the projected path are of great importance. However, organising all the observing stations, aggregating, and analysing the data is time-consuming and not that easy. We have developed a web portal named Occultation Portal (OP) to manage all those occultation observation campaigns from a central server. With this portal, the instrumental and observational information of all observers participating in a stellar occultation campaign and the concerned data are archived systematically in a standard format. The researchers can then visualise the archived data on an event basis. The investigators can also extract the light curve for each data-set with the added reduction pipeline to the portal base. This paper describes in detail the portal structure and the developed features., Comment: 13 pages, 12 figures, 1 table, and 1 listing, accepted for publication in MNRAS
Published: 2022
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10. Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation

Author: Santos-Sanz, P., Ortiz, J. L., Sicardy, B., Popescu, M., Benedetti-Rossi, G., Morales, N., Vara-Lubiano, M., Camargo, J. I. B., Pereira, C. L., Rommel, F. L., Assafin, M., Desmars, J., Braga-Ribas, F., Duffard, R., Oliveira, J. Marques, Vieira-Martins, R., Fernández-Valenzuela, E., Morgado, B. E., Acar, M., Anghel, S., Atalay, E., Ateş, A., Bakış, H., Bakış, V., Eker, Z., Erece, O., Kaspi, S., Kayhan, C., Kilic, S. E., Kilic, Y., Manulis, I., Nedelcu, D. A., Niaei, M. S., Nir, G., Ofek, E., Ozisik, T., Petrescu, E., Satir, O., Solmaz, A., Sonka, A., Tekes, M., Unsalan, O., Yesilyaprak, C., Anghel, R., Berteşteanu, D., Curelaru, L., Danescu, C., Dumitrescu, V., Gherase, R., Hudin, L., Stoian, A-M., Tercu, J. O., Truta, R., Turcu, V., Vantdevara, C., Belskaya, I., Dementiev, T. O., Gazeas, K., Karampotsiou, S., Kashuba, V., Kiss, Cs., Koshkin, N., Kozhukhov, O. M., Krugly, Y., Lecacheux, J., Pal, A., Püsküllü, Ç., Szakats, R., Zhukov, V., Bamberger, D., Mondon, B., Perelló, C., Pratt, A., Schnabel, C., Selva, A., Teng, J. P., Tigani, K., Tsamis, V., Weber, C., Wells, G., Kalkan, S., Kudak, V., Marciniak, A., Ogloza, W., Ozdemir, T., Pakstiene, E., Perig, V., and Zejmo, M.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Within our international program to obtain accurate physical properties of trans-Neptunian objects (TNOs) we predicted a stellar occultation by the TNO (38628) Huya of the star Gaia DR2 4352760586390566400 (mG = 11.5 mag.) for March 18, 2019. After an extensive observational campaign, we updated the prediction and it turned out to be favorable to central Europe. Therefore, we mobilized half a hundred professional and amateur astronomers, and the occultation was finally detected from 21 telescopes located at 18 sites. This makes the Huya event one of the best ever observed stellar occultation by a TNO in terms of the number of chords. We determine accurate size, shape, and geometric albedo, and we also provide constraints on the density and other internal properties of this TNO. 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. The projected semi-major and minor axes of the best ellipse fit obtained using the occultation data are (a', b') = (217.6 $\pm$ 3.5 km, 194.1 $\pm$ 6.1 km) with a position angle of the minor axis P' = 55.2 $\pm$ 9.1 degrees. From this fit, the projected area-equivalent diameter is 411.0 $\pm$ 7.3 km. This diameter is compatible with the equivalent diameter for Huya obtained from radiometric techniques (D = 406 $\pm$ 16 km). From this instantaneous limb, we obtained the geometric albedo for Huya (p$\rm_V$ = 0.079 $\pm$ 0.004) and we explored possible 3D 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 is constrained using the occultation data. We also derived an upper limit for a putative Pluto-like global atmosphere of about p$_{\rm surf}$ = 10 nbar., Comment: Accepted for publication in Astronomy & Astrophysics (30-April-2022). 19 pages, 7 figures
Published: 2022
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11. Milliarcsecond astrometry for the Galilean moons using stellar occultations

Author: Morgado, B. E., Gomes-Júnior, A. R., Braga-Ribas, F., Vieira-Martins, R., Desmars, J., Lainey, V., D'aversa, E., Dunham, D., Moore, J., Baillié, K., Herald, D., Assafin, M., Sicardy, B., Aoki, S., Bardecker, J., Barton, J., Blank, T., Bruns, D., Carlson, N., Carlson, R. W., Cobble, K., Dunham, J., Eisfeldt, D., Emilio, M., Jacques, C., Hinse, T. C., Kim, Y., Malacarne, M., Maley, P. D., Maury, A., Meza, E., Oliva, F., Orton, G. S., Pereira, C. L., Person, M., Plainaki, C., Sfair, R., Sindoni, G., Smith, M., Sussenbach, E., Stuart, P., Vrolijk, J., and Winter, O. C.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: A stellar occultation occurs when a Solar System object passes in front of a star for an observer. This technique allows the determination of sizes and shapes of the occulting body with kilometer precision. Also, this technique constrains the occulting body's positions, albedos, densities, etc. In the context of the Galilean moons, these events can provide their best ground-based astrometry, with uncertainties in the order of 1 mas ($\sim$ 3 km at Jupiter's distance during opposition). We organized campaigns and successfully observed a stellar occultation by Io (JI) in 2021, one by Ganymede (JIII) in 2020, and one by Europa (JII) in 2019, with stations in North and South America. Also, we re-analyzed two previously published events, one by Europa in 2016 and another by Ganymede in 2017. Then, we fit the known 3D shape of the occulting satellite and determine its center of figure. That resulted in astrometric positions with uncertainties in the milliarcsecond level. The positions obtained from these stellar occultations can be used together with dynamical models to ensure highly accurate orbits of the Galilean moons. These orbits can help plan future space probes aiming at the Jovian system, such as JUICE by ESA and Europa Clipper by NASA, and allow more efficient planning of flyby maneuvers., Comment: 19 pages, 25 figures, Accepted on March 14, 2022 for publication in The Astronomical Journal
Published: 2022
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12. Constraints on the structure and seasonal variations of Triton's atmosphere from the 5 October 2017 stellar occultation and previous observations

Author: Oliveira, J. Marques, Sicardy, B., Gomes-Júnior, A. R., Ortiz, J. L., Strobel, D. F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Bérard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos-Sanz, P., Morales, N., Duffard, R., Fernández-Valenzuela, E., Castro-Tirado, A. J., Braga-Ribas, F., Morgado, B. E., Assafin, M., Camargo, J. I. B., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Filho, S., Banda-Huarca, M. V., Quispe-Huaynasi, F., Pereira, C. L., Rommel, F. L., Margoti, G., Dias-Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, R., Pérez-Hoyos, S., Sánchez-Lavega, A., Rojas, J. F., Beisker, W., Kretlow, M., Herald, D., Gault, D., Bath, K. -L., Bode, H. -J., Bredner, E., Guhl, K., Haymes, T. V., Hummel, E., Kattentidt, B., Klös, O., Pratt, A., Thome, B., Avdellidou, C., Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A. A., Xilouris, E. M., Alikakos, I., Gourzelas, A., Liakos, A., Charmandaris, V., Jelínek, M., Štrobl, J., Eberle, A., Rapp, K., Gährken, B., Klemt, B., Kowollik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, D., Brandis, L., Pütz, I., Perdelwitz, V., Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J. -M., Ciabattari, F., Di Luca, R., Alboresi, D., Leto, G., Sanchez, R. Zanmar, Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, C., Savio, R. Lo, Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., Gallego, S., Tortorelli, L., Sposetti, S., Sussenbach, J., Abbeel, F. Van Den, André, P., Llibre, M., Pailler, F., Ardissone, J., Boutet, M., Sanchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J. L., Dechambre, O., Delay, P., Delcroix, M., Rousselot, L., Ferreira, J., Machado, P., Tanga, P., Rivet, J. -P., Frappa, E., Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A. N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, J. -F., Metz, F., Erpelding, D., Nougayrède, P., Midavaine, T., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Aissa, D. Baba, Grigahcene, Z., Briggs, D., Broadbent, S., Denyer, P., Haigh, N. J., Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., Talbot, J., Alonso, S., Reche, A. Román, Casanova, V., Briggs, E., Iglesias-Marzoa, R., Ibáñez, J. Abril, Martín, M. C. Díaz, González, H., García, J. L. Maestre, Marchant, J., Ordonez-Etxeberria, I., Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perello, C., Cabedo, V., Gonçalves, R., Ferreira, M., Dias, F. Marques, Daassou, A., Barkaoui, K., Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., Moutamid, M. El, Lamarche, C., Pollock, J. T., Caton, D. B., Kouprianov, V., Timerson, B. W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J. -P., Françoise, J., Mondon, B., Payet, T., Boissel, C., Castets, M., Hubbard, W. B., Hill, R., Reitsema, H. J., Mousis, O., Ball, L., Neilsen, G., Hutcheon, S., Lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., and Downs, B.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: A stellar occultation by Neptune's main satellite, Triton, was observed on 5 October 2017 from Europe, North Africa, and the USA. We derived 90 light curves from this event, 42 of which yielded a central flash detection. We aimed at constraining Triton's atmospheric structure and the seasonal variations of its atmospheric pressure since the Voyager 2 epoch (1989). We also derived the shape of the lower atmosphere from central flash analysis. We used Abel inversions and direct ray-tracing code to provide the density, pressure, and temperature profiles in the altitude range $\sim$8 km to $\sim$190 km, corresponding to pressure levels from 9 {\mu}bar down to a few nanobars. Results. (i) A pressure of 1.18$\pm$0.03 {\mu}bar is found at a reference radius of 1400 km (47 km altitude). (ii) A new analysis of the Voyager 2 radio science occultation shows that this is consistent with an extrapolation of pressure down to the surface pressure obtained in 1989. (iii) A survey of occultations obtained between 1989 and 2017 suggests that an enhancement in surface pressure as reported during the 1990s might be real, but debatable, due to very few high S/N light curves and data accessible for reanalysis. The volatile transport model analysed supports a moderate increase in surface pressure, with a maximum value around 2005-2015 no higher than 23 {\mu}bar. The pressures observed in 1995-1997 and 2017 appear mutually inconsistent with the volatile transport model presented here. (iv) The central flash structure does not show evidence of an atmospheric distortion. We find an upper limit of 0.0011 for the apparent oblateness of the atmosphere near the 8 km altitude., Comment: 52 pages, 26 figures in the main paper, 2 figures in appendix B, 9 figures in appendix C, 1 long table over 5 pages
Published: 2022
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13. SORA: Stellar Occultation Reduction and Analysis

Author: Gomes-Júnior, A. R., Morgado, B. E., Benedetti-Rossi, G., Boufleur, R. C., Rommel, F. L., Banda-Huarca, M. V., Kilic, Y., Braga-Ribas, F., and Sicardy, B.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The stellar occultation technique provides competitive accuracy in determining the sizes, shapes, astrometry, etc., of the occulting body, comparable to in-situ observations by spacecraft. With the increase in the number of known Solar System objects expected from the LSST, the highly precise astrometric catalogues, such as Gaia, and the improvement of ephemerides, occultations observations will become more common with a higher number of chords in each observation. In the context of the Big Data era, we developed SORA, an open-source python library to reduce and analyse stellar occultation data efficiently. It includes routines from predicting such events up to the determination of Solar System bodies' sizes, shapes, and positions., Comment: 15 pages, 7 figures
Published: 2022
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14. Refined physical parameters for Chariklo's body and rings from stellar occultations observed between 2013 and 2020

Author: Morgado, B. E., Sicardy, B., Braga-Ribas, F., Desmars, J., Gomes-Júnior, A. R., Bérard, D., Leiva, R., Ortiz, J. L., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Sanz, P., Camargo, J. I. B., Duffard, R., Rommel, F. L., Assafin, M., Boufleur, R. C., Colas, F., Kretlow, M., Beisker, W., Sfair, R., Snodgrass, C., Morales, N., Fernández-Valenzuela, E., Amaral, L. S., Amarante, A., Artola, R. A., Backes, M., Bath, K-L., Bouley, S., Buie, M. W., Cacella, P., Colazo, C. A., Colque, J. P., Dauvergne, J-L., Dominik, M., Emilio, M., Erickson, C., Evans, R., Fabrega-Polleri, J., Garcia-Lambas, D., Giacchini, B. L., Hanna, W., Herald, D., Hesler, G., Hinse, T. C., Jacques, C., Jehin, E., Jørgensen, U. G., Kerr, S., Kouprianov, V., Levine, S. E., Linder, T., Maley, P. D., Machado, D. I., Maquet, L., Maury, A., Melia, R., Meza, E., Mondon, B., Moura, T., Newman, J., Payet, T., Pereira, C. L., Pollock, J., Poltronieri, R. C., Quispe-Huaynasi, F., Reichart, D., de Santana, T., Schneiter, E. M., Sieyra, M. V., Skottfelt, J., Soulier, J. F., Starck, M., Thierry, P., Torres, P. J., Trabuco, L. L., Unda-Sanzana, E., Yamashita, T. A. R., Winter, O. C., Zapata, A., and Zuluaga, C. A.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The Centaur (10199) Chariklo has the first rings system discovered around a small object. It was first observed using stellar occultation in 2013. Stellar occultations allow the determination of sizes and shapes with kilometre accuracy and obtain characteristics of the occulting object and its vicinity. Using stellar occultations observed between 2017 and 2020, we aim at constraining Chariklo's and its rings physical parameters. We also determine the rings' structure, and obtain precise astrometrical positions of Chariklo. We predicted and organised several observational campaigns of stellar occultations by Chariklo. Occultation light curves were measured from the data sets, from which ingress and egress times, and rings' width and opacity were obtained. These measurements, combined with results from previous works, allow us to obtain significant constraints on Chariklo's shape and rings' structure. We characterise Chariklo's ring system (C1R and C2R), and obtain radii and pole orientations that are consistent with, but more accurate than, results from previous occultations. We confirmed the detection of W-shaped structures within C1R and an evident variation of radial width. The observed width ranges between 4.8 and 9.1 km with a mean value of 6.5 km. One dual observation (visible and red) does not reveal any differences in the C1R opacity profiles, indicating ring particle's size larger than a few microns. The C1R ring eccentricity is found to be smaller than 0.022 (3-sigma), and its width variations may indicate an eccentricity higher than 0.005. We fit a tri-axial shape to Chariklo's detections over eleven occultations and determine that Chariklo is consistent with an ellipsoid with semi-axes of 143.8, 135.2 and 99.1 km. Ultimately, we provided seven astrometric positions at a milliarcseconds accuracy level, based on Gaia EDR3, and use it to improve Chariklo's ephemeris., Comment: 32 pages, 11 Figures in the main text, paper was accepted for publication in Section 10. Planets and planetary systems of Astronomy and Astrophysics on 12/07/2021
Published: 2021
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15. Stellar occultations enable milliarcsecond astrometry for Trans-Neptunian objects and Centaurs

Author: Rommel, F. L., Braga-Ribas, F., Desmars, J., Camargo, J. I. B., Ortiz, J. L., Sicardy, B., Vieira-Martins, R., Assafin, M., Santos-Sanz, P., Duffard, R., Fernández-Valenzuela, E., Lecacheux, J., Morgado, B. E., Benedetti-Rossi, G., Gomes-Júnior, A. R., Pereira, C. L., Herald, D., Hanna, W., Bradshaw, J., Morales, N., Brimacombe, J., Burtovoi, A., Carruthers, T., de Barros, J. R., Fiori, M., Gilmore, A., Hooper, D., Hornoch, K., Jacques, C., Janik, T., Kerr, S., Kilmartin, P., Winkel, Jan Maarten, Naletto, G., Nardiello, D., Nascimbeni, V., Newman, J., Ossola, A., Pál, A., Pimentel, E., Pravec, P., Sposetti, S., Stechina, A., Szákats, R., Ueno, Y., Zampieri, L., Broughton, J., Dunham, J. B., Dunham, D. W., Gault, D., Hayamizu, T., Hosoi, K., Jehin, E., Jones, R., Kitazaki, K., Komžík, R., Marciniak, A., Maury, A., Mikuž, H., Nosworthy, P., Polleri, J. Fábrega, Rahvar, S., Sfair, R., Siqueira, P. B., Snodgrass, C., Sogorb, P., Tomioka, H., Tregloan-Reed, J., and Winter, O. C.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Trans-Neptunian objects (TNOs) and Centaurs are remnants of our planetary system formation, and their physical properties have invaluable information for evolutionary theories. Stellar occultation is a ground-based method for studying these small bodies and has presented exciting results. These observations can provide precise profiles of the involved body, allowing an accurate determination of its size and shape. The goal is to show that even single-chord detections of TNOs allow us to measure their milliarcsecond astrometric positions in the reference frame of the Gaia second data release (DR2). Accurated ephemerides can then be generated, allowing predictions of stellar occultations with much higher reliability. We analyzed data from stellar occultations to obtain astrometric positions of the involved bodies. The events published before the Gaia era were updated so that the Gaia DR2 catalog is the reference. Previously determined sizes were used to calculate the position of the object center and its corresponding error with respect to the detected chord and the International Celestial Reference System (ICRS) propagated Gaia DR2 star position. We derive 37 precise astrometric positions for 19 TNOs and 4 Centaurs. Twenty-one of these events are presented here for the first time. Although about 68\% of our results are based on single-chord detection, most have intrinsic precision at the submilliarcsecond level. Lower limits on the diameter and shape constraints for a few bodies are also presented as valuable byproducts. Using the Gaia DR2 catalog, we show that even a single detection of a stellar occultation allows improving the object ephemeris significantly, which in turn enables predicting a future stellar occultation with high accuracy. Observational campaigns can be efficiently organized with this help, and may provide a full physical characterization of the involved object., Comment: 16 pages, 28 figures. The manuscript was accepted and is to be published
Published: 2020
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16. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author: Ortiz, J. L., Santos-Sanz, P., Sicardy, B., Benedetti-Rossi, G., Bérard, D., Morales, N., Duffard, R., Braga-Ribas, F., Hopp, U., Ries, C., Nascimbeni, V., Marzari, F., Granata, V., Pál, A., Kiss, C., Pribulla, T., Komžík, R., Hornoch, K., Pravec, P., Bacci, P., Maestripieri, M., Nerli, L., Mazzei, L., Bachini, M., Martinelli, F., Succi, G., Ciabattari, F., Mikuz, H., Carbognani, A., Gaehrken, B., Mottola, S., Hellmic, S., Rommel, F. L., Fernández-Valenzuela, E., Bagatin, A. Campo, Cikota, S., Cikota, A., Lecacheux, J., Vieira-Martins, R., Camargo, J. I. B., Assafin, M., Colas, F., Behrend, R., Desmars, J., Meza, E., Alvarez-Candal, A., Beisker, W., Gomes-Junior, A. R., Morgado, B. E., Roques, F., Vachier, F., Berthier, J., Mueller, T. G., Madiedo, J. M., Unsalan, O., Sonbas, E., Karaman, N., Erece, O., Koseoglu, D. T., Ozisik, T., Kalkan, S., Guney, Y., Niaei, M. S., Satir, O., Yesilyaprak, C., Puskullu, C., Kabas, A., Demircan, O., Alikakos, J., Charmandaris, V., Leto, G., Ohlert, J., Christille, J. M., Szakáts, R., Farkas, A. Takácsné, Varga-Verebélyi, E., Marton, G., Marciniak, A., Bartczak, P., Santana-Ros, T., Butkiewicz-Bąk, M., Dudziński, G., Alí-Lagoa, V., Gazeas, K., Tzouganatos, L., Paschalis, N., Tsamis, V., Sánchez-Lavega, A., Pérez-Hoyos, S., Hueso, R., Guirado, J. C., Peris, V., and Iglesias-Marzoa, R.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Among the four known transneptunian dwarf planets, Haumea is an exotic, very elongated, and fast rotating body. In contrast to the other dwarf planets, its size, shape, albedo, and density are not well constrained. Here we report results of a multi-chord stellar occultation, observed on 2017 January 21. Secondary events observed around the main body are consistent with the presence of a ring of opacity 0.5, width 70 km, and radius 2,287$_{-45}^{+75}$ km. The Centaur Chariklo was the first body other than a giant planet to show a ring system and the Centaur Chiron was later found to possess something similar to Chariklo's rings. Haumea is the first body outside the Centaur population with a ring. The ring is coplanar with both Haumea's equator and the orbit of its satellite Hi'iaka. Its radius places close to the 3:1 mean motion resonance with Haumea's spin period. The occultation by the main body provides an instantaneous elliptical limb with axes 1,704 $\pm$ 4 km x 1,138 $\pm$ 26 km. Combined with rotational light-curves, it constrains Haumea's 3D orientation and its triaxial shape, which is inconsistent with a homogeneous body in hydrostatic equilibrium. Haumea's largest axis is at least 2,322 $\pm$ 60 km, larger than thought before. This implies an upper limit of 1,885 $\pm$ 80 kg m$^{-3}$ for Haumea's density, smaller and less puzzling than previous estimations, and a geometric albedo of 0.51 $\pm$ 0.02, also smaller than previous estimations. No global N$_2$ or CH$_4$ atmosphere with pressures larger than 15 and 50 nbar (3-$\sigma$ limits), respectively, is detected.
Published: 2020
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17. Author Correction: A dense ring of the trans-Neptunian object Quaoar outside its Roche limit

Author: Morgado, B. E., Sicardy, B., Braga-Ribas, F., Ortiz, J. L., Salo, H., Vachier, F., Desmars, J., Pereira, C. L., Santos-Sanz, P., Sfair, R., de Santana, T., Assafin, M., Vieira-Martins, R., Gomes-Júnior, A. R., Margoti, G., Dhillon, V. S., Fernández-Valenzuela, E., Broughton, J., Bradshaw, J., Langersek, R., Benedetti-Rossi, G., Souami, D., Holler, B. J., Kretlow, M., Boufleur, R. C., Camargo, J. I. B., Duffard, R., Beisker, W., Morales, N., Lecacheux, J., Rommel, F. L., Herald, D., Benz, W., Jehin, E., Jankowsky, F., Marsh, T. R., Littlefair, S. P., Bruno, G., Pagano, I., Brandeker, A., Collier-Cameron, A., Florén, H. G., Hara, N., Olofsson, G., Wilson, T. G., Benkhaldoun, Z., Busuttil, R., Burdanov, A., Ferrais, M., Gault, D., Gillon, M., Hanna, W., Kerr, S., Kolb, U., Nosworthy, P., Sebastian, D., Snodgrass, C., Teng, J. P., and de Wit, J.
Published: 2024
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18. A dense ring of the trans-Neptunian object Quaoar outside its Roche limit

Author: Morgado, B. E., Sicardy, B., Braga-Ribas, F., Ortiz, J. L., Salo, H., Vachier, F., Desmars, J., Pereira, C. L., Santos-Sanz, P., Sfair, R., de Santana, T., Assafin, M., Vieira-Martins, R., Gomes-Júnior, A. R., Margoti, G., Dhillon, V. S., Fernández-Valenzuela, E., Broughton, J., Bradshaw, J., Langersek, R., Benedetti-Rossi, G., Souami, D., Holler, B. J., Kretlow, M., Boufleur, R. C., Camargo, J. I. B., Duffard, R., Beisker, W., Morales, N., Lecacheux, J., Rommel, F. L., Herald, D., Benz, W., Jehin, E., Jankowsky, F., Marsh, T. R., Littlefair, S. P., Bruno, G., Pagano, I., Brandeker, A., Collier-Cameron, A., Florén, H. G., Hara, N., Olofsson, G., Wilson, T. G., Benkhaldoun, Z., Busuttil, R., Burdanov, A., Ferrais, M., Gault, D., Gillon, M., Hanna, W., Kerr, S., Kolb, U., Nosworthy, P., Sebastian, D., Snodgrass, C., Teng, J. P., and de Wit, J.
Published: 2023
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19. Size and shape of Chariklo from multi-epoch stellar occultations

Author: Leiva, R, Sicardy, B, Camargo, J I B, Ortiz, J -L, Desmars, J, Bérard, D, Lellouch, E, Meza, E, Kervella, P, Snodgrass, C, Duffard, R, Morales, N, Gomes-Júnior, A R, Benedetti-Rossi, G, Vieira-Martins, R, Braga-Ribas, F, Assafin, M, Morgado, B E, Colas, F, De Witt, C, Sickafoose, A A, Breytenbach, H, Dauvergne, J -L, Schoenau, P, Maquet, L, Bath, K L, Bode, H J, Cool, A, Lade, B, Kerr, S, and Herald, D
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We use data from five stellar occultations observed between 2013 and 2016 to constrain Chariklo's size and shape, and the ring reflectivity. We consider four possible models for Chariklo (sphere, Maclaurin spheroid, tri-axial ellipsoid and Jacobi ellipsoid) and we use a Bayesian approach to estimate the corresponding parameters. The spherical model has a radius $R=129\pm3$ km. The Maclaurin model has equatorial and polar radii $a=b=143^{+3}_{-6}$ km and $c=96^{+14}_{-4}$ km, respectively, with density $970^{+300}_{-180}$ kg m$^{-3}$. The ellipsoidal model has semiaxes $a=148^{+6}_{-4}$ km, $b=132^{+6}_{-5}$ km and $c=102^{+10}_{-8}$ km. Finally, the Jacobi model has semiaxes $a$=157$\pm$4 km, $b$=139$\pm$ 4 km and $c$=86$\pm$1 km, and density $796^{+2}_{-4}$ kg m$^{-3}$ . Depending on the model, we obtain topographic features of 6-11 km, typical of Saturn icy satellites with similar size and density. We constrain Chariklo's geometric albedo between 3.1\% (sphere) and 4.9\% (ellipsoid), while the ring $I/F$ reflectivity is less constrained between 0.6\% (Jacobi) and 8.9\% (sphere). The ellipsoid model explains both the optical light curve and the long-term photometry variation of the system, giving a plausible value for the geometric albedo of the ring particles of $10-15\%$. The derived Chariklo's mass of 6-8$\times10^{18}$ kg places the rings close to the 3:1 resonance between the ring mean motion and Chariklo's rotation period., Comment: Accepted for publication in AJ
Published: 2017
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20. The two rings of (50000) Quaoar (Corrigendum)

Author: Pereira, C. L., primary, Sicardy, B., additional, Morgado, B. E., additional, Braga-Ribas, F., additional, Fernández-Valenzuela, E., additional, Souami, D., additional, Holler, B. J., additional, Boufleur, R. C., additional, Margoti, G., additional, Assafin, M., additional, Ortiz, J. L., additional, Santos-Sanz, P., additional, Epinat, B., additional, Kervella, P., additional, Desmars, J., additional, Vieira-Martins, R., additional, Kilic, Y., additional, Gomes-Júnior, A. R., additional, Camargo, J. I. B., additional, Emilio, M., additional, Vara-Lubiano, M., additional, Kretlow, M., additional, Albert, L., additional, Alcock, C., additional, Ball, J. G., additional, Bender, K., additional, Buie, M. W., additional, Butterfield, K., additional, Camarca, M., additional, Castro-Chacón, J. H., additional, Dunford, R., additional, Fisher, R. S., additional, Gamble, D., additional, Geary, J. C., additional, Gnilka, C. L., additional, Green, K. D., additional, Hartman, Z. D., additional, Huang, C-K., additional, Januszewski, H., additional, Johnston, J., additional, Kagitani, M., additional, Kamin, R., additional, Kavelaars, J. J., additional, Keller, J. M., additional, de Kleer, K. R., additional, Lehner, M. J., additional, Luken, A., additional, Marchis, F., additional, Marlin, T., additional, McGregor, K., additional, Nikitin, V., additional, Nolthenius, R., additional, Patrick, C., additional, Redfield, S., additional, Rengstorf, A. W., additional, Reyes-Ruiz, M., additional, Seccull, T., additional, Skrutskie, M. F., additional, Smith, A. B., additional, Sproul, M., additional, Stephens, A. W., additional, Szentgyorgyi, A., additional, Sánchez-Sanjuán, S., additional, Tatsumi, E., additional, Verbiscer, A., additional, Wang, S-Y., additional, Yoshida, F., additional, Young, R., additional, and Zhang, Z-W., additional
Published: 2024
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21. New orbits of irregular satellites designed for the predictions of stellar occultations up to 2020, based on thousands of new observations

Author: Gomes-Júnior, A. R., Assafin, M., Beauvalet, L., Desmars, J., Vieira-Martins, R., Camargo, J. I. B., Morgado, B. E., and Braga-Ribas, F.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Gomes-J\'unior et al. (2015) published 3613 positions for the 8 largest irregular satellites of Jupiter and 1787 positions for the largest irregular satellite of Saturn, Phoebe. These observations were made between 1995 and 2014 and have an estimated error of about 60 to 80 mas. Based on this set of positions, we derived new orbits for the eight largest irregular satellites of Jupiter: Himalia, Elara, Pasiphae, Carme, Lysithea, Sinope, Ananke and Leda. For Phoebe we updated the ephemeris from Desmars et al. (2013) using 75% more positions than the previous one. Due to their orbital characteristics, it is common belief that the irregular satellites were captured by the giant planets in the early Solar System, but there is no consensus for a single model explaining where they were formed. Size, shape, albedo and composition would help to trace back their true origin, but these physical parameters are yet poorly known for irregular satellites. The observation of stellar occultations would allow for the determination of such parameters. Indeed Jupiter will cross the galactic plane in 2019-2020 and Saturn in 2018, improving a lot the chances of observing such events in the near future. Using the derived ephemerides and the UCAC4 catalogue we managed to identify 5442 candidate stellar occultations between January 2016 and December 2020 for the 9 satellites studied here. We discussed how the successful observation of a stellar occultation by these objects is possible and present some potential occultations., Comment: 8 pages, 4 figures
Published: 2016
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22. Astrometric positions for 18 irregular satellites of giant planets from 23 years of observations

Author: Gomes-Júnior, A. R., Assafin, M., Vieira-Martins, R., Arlot, J. -E., Camargo, J. I. B., Braga-Ribas, F., Neto, D. N. da Silva, Andrei, A. H., Dias-Oliveira, A., Morgado, B. E., Benedetti-Rossi, G., Duchemin, Y., Desmars, J., Lainey, V., and Thuillot, W.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The irregular satellites of the giant planets are believed to have been captured during the evolution of the solar system. Knowing their physical parameters, such as size, density, and albedo is important for constraining where they came from and how they were captured. The best way to obtain these parameters are observations in situ by spacecrafts or from stellar occultations by the objects. Both techniques demand that the orbits are well known. We aimed to obtain good astrometric positions of irregular satellites to improve their orbits and ephemeris. We identified and reduced observations of several irregular satellites from three databases containing more than 8000 images obtained between 1992 and 2014 at three sites (Observat\'orio do Pico dos Dias, Observatoire de Haute-Provence, and European Southern Observatory - La Silla). We used the software PRAIA (Platform for Reduction of Astronomical Images Automatically) to make the astrometric reduction of the CCD frames. The UCAC4 catalog represented the International Celestial Reference System in the reductions. Identification of the satellites in the frames was done through their ephemerides as determined from the SPICE/NAIF kernels. Some procedures were followed to overcome missing or incomplete information (coordinates, date), mostly for the older images. We managed to obtain more than 6000 positions for 18 irregular satellites: 12 of Jupiter, 4 of Saturn, 1 of Uranus (Sycorax), and 1 of Neptune (Nereid). For some satellites the number of obtained positions is more than 50\% of what was used in earlier orbital numerical integrations. Comparison of our positions with recent JPL ephemeris suggests there are systematic errors in the orbits for some of the irregular satellites. The most evident case was an error in the inclination of Carme., Comment: 9 pages, with 3 being online material
Published: 2015
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23. Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations

Author: Pereira, C L, primary, Braga-Ribas, F, additional, Sicardy, B, additional, Gomes-Júnior, A R, additional, Ortiz, J L, additional, Branco, H C, additional, Camargo, J I B, additional, Morgado, B E, additional, Vieira-Martins, R, additional, Assafin, M, additional, Benedetti-Rossi, G, additional, Desmars, J, additional, Emilio, M, additional, Morales, R, additional, Rommel, F L, additional, Hayamizu, T, additional, Gondou, T, additional, Jehin, E, additional, Artola, R A, additional, Asai, A, additional, Colazo, C, additional, Ducrot, E, additional, Duffard, R, additional, Fabrega, J, additional, Fernandez-Valenzuela, E, additional, Gillon, M, additional, Horaguchi, T, additional, Ida, M, additional, Kitazaki, K, additional, Mammana, L A, additional, Maury, A, additional, Melita, M, additional, Morales, N, additional, Moya-Sierralta, C, additional, Owada, M, additional, Pollock, J, additional, Sanchez, J L, additional, Santos-Sanz, P, additional, Sasanuma, N, additional, Sebastian, D, additional, Triaud, A, additional, Uchiyama, S, additional, Vanzi, L, additional, Watanabe, H, additional, and Yamamura, H, additional
Published: 2023
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24. Kilometer-precise (UII) Umbriel physical properties from the multichord stellar occultation on 2020 September 21

Author: Assafin, M, primary, Santos-Filho, S, additional, Morgado, B E, additional, Gomes-Júnior, A R, additional, Sicardy, B, additional, Margoti, G, additional, Benedetti-Rossi, G, additional, Braga-Ribas, F, additional, Laidler, T, additional, Camargo, J I B, additional, Vieira-Martins, R, additional, Swift, T, additional, Dunham, D, additional, George, T, additional, Bardecker, J, additional, Anderson, C, additional, Nolthenius, R, additional, Bender, K, additional, Viscome, G, additional, Oesper, D, additional, Dunford, R, additional, Getrost, K, additional, Kitting, C, additional, Green, K, additional, Bria, R, additional, Olsen, A, additional, Scheck, A, additional, Billard, B, additional, Wasiuta, M E, additional, Tatum, R, additional, Maley, P, additional, di Cicco, D, additional, Gamble, D, additional, Ceravolo, P, additional, Ceravolo, D, additional, Hanna, W, additional, Smith, N, additional, Carlson, N, additional, Messner, S, additional, Bean, J, additional, Moore, J, additional, and Venable, R, additional
Published: 2023
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25. The 2021 mutual phenomena involving the Galilean satellites of Jupiter and the inner satellite Thebe

Author: Catani, L M, primary, Assafin, M, additional, Morgado, B E, additional, Santos-Filho, S, additional, Braga-Ribas, F, additional, Vieira-Martins, R, additional, Arcas-Silva, J, additional, Milone, A C, additional, Lima, I J, additional, and Botelho, R B, additional
Published: 2023
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26. A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS4 measured from stellar occultations

Author: Rommel, F. L., primary, Braga-Ribas, F., additional, Ortiz, J. L., additional, Sicardy, B., additional, Santos-Sanz, P., additional, Desmars, J., additional, Camargo, J. I. B., additional, Vieira-Martins, R., additional, Assafin, M., additional, Morgado, B. E., additional, Boufleur, R. C., additional, Benedetti-Rossi, G., additional, Gomes-Júnior, A. R., additional, Fernández-Valenzuela, E., additional, Holler, B. J., additional, Souami, D., additional, Duffard, R., additional, Margoti, G., additional, Vara-Lubiano, M., additional, Lecacheux, J., additional, Plouvier, J. L., additional, Morales, N., additional, Maury, A., additional, Fabrega, J., additional, Ceravolo, P., additional, Jehin, E., additional, Albanese, D., additional, Mariey, H., additional, Cikota, S., additional, Ruždjak, D., additional, Cikota, A., additional, Szakáts, R., additional, Baba Aissa, D., additional, Gringahcene, Z., additional, Kashuba, V., additional, Koshkin, N., additional, Zhukov, V., additional, Fişek, S., additional, Çakir, O., additional, Özer, S., additional, Schnabel, C., additional, Schnabel, M., additional, Signoret, F., additional, Morrone, L., additional, Santana-Ros, T., additional, Pereira, C. L., additional, Emilio, M., additional, Burdanov, A. Y., additional, de Wit, J., additional, Barkaoui, K., additional, Gillon, M., additional, Leto, G., additional, Frasca, A., additional, Catanzaro, G., additional, Sanchez, R. Zanmar, additional, Tagliaferri, U., additional, Di Sora, M., additional, Isopi, G., additional, Krugly, Y., additional, Slyusarev, I., additional, Chiorny, V., additional, Mikuž, H., additional, Bacci, P., additional, Maestripieri, M., additional, Grazia, M. D., additional, de la Cueva, I., additional, Yuste-Moreno, M., additional, Ciabattari, F., additional, Kozhukhov, O. M., additional, Serra-Ricart, M., additional, Alarcon, M. R., additional, Licandro, J., additional, Masi, G., additional, Bacci, R., additional, Bosch, J. M., additional, Behem, R., additional, Prost, J.-P., additional, Renner, S., additional, Conjat, M., additional, Bachini, M., additional, Succi, G., additional, Stoian, L., additional, Juravle, A., additional, Carosati, D., additional, Gowe, B., additional, Carrillo, J., additional, Zheleznyak, A. P., additional, Montigiani, N., additional, Foster, C. R., additional, Mannucci, M., additional, Ruocco, N., additional, Cuevas, F., additional, Di Marcantonio, P., additional, Coretti, I., additional, Iafrate, G., additional, Baldini, V., additional, Collins, M., additional, Pál, A., additional, Csák, B., additional, Fernández-Garcia, E., additional, Castro-Tirado, A. J., additional, Hudin, L., additional, Madiedo, J. M., additional, Anghel, R. M., additional, Calvo-Fernández, J. F., additional, Valvasori, A., additional, Guido, E., additional, Gherase, R. M., additional, Kamoun, S., additional, Fafet, R., additional, Sánchez-González, M., additional, Curelaru, L., additional, Vîntdevară, C. D., additional, Danescu, C. A., additional, Gout, J.-F., additional, Schmitz, C. J., additional, Sota, A., additional, Belskaya, I., additional, Rodríguez-Marco, M., additional, Kilic, Y., additional, Frappa, E., additional, Klotz, A., additional, Lavayssière, M., additional, Oliveira, J. Marques, additional, Popescu, M., additional, Mammana, L. A., additional, Fernández-Lajús, E., additional, Schmidt, M., additional, Hopp, U., additional, Komžík, R., additional, Pribulla, T., additional, Tomko, D., additional, Husárik, M., additional, Erece, O., additional, Eryilmaz, S., additional, Buzzi, L., additional, Gährken, B., additional, Nardiello, D., additional, Hornoch, K., additional, Sonbas, E., additional, Er, H., additional, Burwitz, V., additional, Sybilski, P. Waldemar, additional, Bykowski, W., additional, Müller, T. G., additional, Ogloza, W., additional, Gonçalves, R., additional, Ferreira, J. F., additional, Ferreira, M., additional, Bento, M., additional, Meister, S., additional, Bagiran, M. N., additional, Tekeş, M., additional, Marciniak, A., additional, Moravec, Z., additional, Delinčák, P., additional, Gianni, G., additional, Casalnuovo, G. B., additional, Boutet, M., additional, Sanchez, J., additional, Klemt, B., additional, Wuensche, N., additional, Burzynski, W., additional, Borkowski, M., additional, Serrau, M., additional, Dangl, G., additional, Klös, O., additional, Weber, C., additional, Urbaník, M., additional, Rousselot, L., additional, Kubánek, J., additional, André, P., additional, Colazo, C., additional, Spagnotto, J., additional, Sickafoose, A. A., additional, Hueso, R., additional, Sánchez-Lavega, A., additional, Fisher, R. S., additional, Rengstorf, A. W., additional, Perelló, C., additional, Dascalu, M., additional, Altan, M., additional, Gazeas, K., additional, de Santana, T., additional, Sfair, R., additional, Winter, O. C., additional, Kalkan, S., additional, Canales-Moreno, O., additional, Trigo-Rodríguez, J. M., additional, Tsamis, V., additional, Tigani, K., additional, Sioulas, N., additional, Lekkas, G., additional, Bertesteanu, D. N., additional, Dumitrescu, V., additional, Wilberger, A. J., additional, Barnes, J. W., additional, Fieber-Beyer, S. K., additional, Swaney, R. L., additional, Fuentes, C., additional, Mendez, R. A., additional, Dumitru, B. D., additional, Flynn, R. L., additional, and Wake, D. A., additional
Published: 2023
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27. Dynamical characterization of the 6/1 mean motion resonance between Quaoar’s ring and Weywot

Author: Rodríguez, Adrián, primary, Morgado, B E, additional, and Callegari, N, additional
Published: 2023
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28. Changing material around (2060) Chiron revealed by an occultation on December 15, 2022

Author: Ortiz, J. L., primary, Pereira, C. L., additional, Sicardy, B., additional, Braga-Ribas, F., additional, Takey, A., additional, Fouad, A. M., additional, Shaker, A. A., additional, Kaspi, S., additional, Brosch, N., additional, Kretlow, M., additional, Leiva, R., additional, Desmars, J., additional, Morgado, B. E., additional, Morales, N., additional, Vara-Lubiano, M., additional, Santos-Sanz, P., additional, Fernández-Valenzuela, E., additional, Souami, D., additional, Duffard, R., additional, Rommel, F. L., additional, Kilic, Y., additional, Erece, O., additional, Koseoglu, D., additional, Ege, E., additional, Morales, R., additional, Alvarez-Candal, A., additional, Rizos, J. L., additional, Gómez-Limón, J. M., additional, Assafin, M., additional, Vieira-Martins, R., additional, Gomes-Júnior, A. R., additional, Camargo, J. I. B., additional, and Lecacheux, J., additional
Published: 2023
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29. Constraints on the evolution of the Triton atmosphere from occultations: 1989–2022.

Author: Sicardy, B., Tej, A., Gomes-Júnior, A. R., Romanov, F. D., Bertrand, T., Ashok, N. M., Lellouch, E., Morgado, B. E., Assafin, M., Desmars, J., Camargo, J. I. B., Kilic, Y., Ortiz, J. L., Vieira-Martins, R., Braga-Ribas, F., Ninan, J. P., Bhatt, B. C., Pramod Kumar, S., Swain, V., and Sharma, S.
Subjects: ATMOSPHERIC pressure measurement, SURFACE pressure, VAPOR pressure, ATMOSPHERE, ATMOSPHERIC pressure
Abstract: Context. In about 2000, the south pole of Triton experienced an extreme summer solstice that occurs every ∼650 years, when the subsolar latitude reached about 50°S. Bracketing this epoch, a few occultations probed the Triton atmosphere in 1989, 1995, 1997, 2008, and 2017. A recent ground-based stellar occultation observed on 6 October 2022 provides a new measurement of the atmospheric pressure on Triton. This is presented here. Aims. The goal is to constrain the volatile transport models (VTMs) of the Triton atmosphere. The atmosphere is basically in vapor pressure equilibrium with the nitrogen ice at its surface. Methods. Fits to the occultation light curves yield the atmospheric pressure of Triton at the reference radius 1400 km, from which the surface pressure is deduced. Results. The fits provide a pressure p1400 = 1.211 ± 0.039 μbar at radius 1400 km (47 km altitude), from which a surface pressure of psurf = 14.54 ± 0.47 μbar is deduced (1σ error bars). To within the error bars, this is identical to the pressure derived from the previous occultation of 5 October 2017, p1400 = 1.18 ± 0.03 μbar and psurf = 14.1 ± 0.4 μbar, respectively. Based on recent models of the volatile cycles of Triton, the overall evolution of the surface pressure over the last 30 years is consistent with N2 condensation taking place in the northern hemisphere. However, models typically predict a steady decrease in the surface pressure for the period 2005-2060, which is not confirmed by this observation. Complex surface-atmosphere interactions, such as ice albedo runaway and formation of local N2 frosts in the equatorial regions of Triton, could explain the relatively constant pressure between 2017 and 2022. [ABSTRACT FROM AUTHOR]
Published: 2024
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30. Physical properties of Centaur (60558) 174P/Echeclus from stellar occultations.

Author: 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, and Asai, A
Subjects: OCCULTATIONS (Astronomy), INTERNAL friction, ORBITS (Astronomy), SMALL solar system bodies, DETECTION limit, ALBEDO
Abstract: The Centaur (60558) Echeclus was discovered on 2000 March 03, 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 (⁠|$\rm {H}_{\rm {v}} = 9.971 \pm 0.031$|⁠), we calculate an albedo of p v = 0.050 ± 0.003. Constraints on the object's density and internal friction are also proposed. [ABSTRACT FROM AUTHOR]
Published: 2024
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31. The two rings of (50000) Quaoar

Author: Pereira, C. L., primary, Sicardy, B., additional, Morgado, B. E., additional, Braga-Ribas, F., additional, Fernández-Valenzuela, E., additional, Souami, D., additional, Holler, B. J., additional, Boufleur, R. C., additional, Margoti, G., additional, Assafin, M., additional, Ortiz, J. L., additional, Santos-Sanz, P., additional, Epinat, B., additional, Kervella, P., additional, Desmars, J., additional, Vieira-Martins, R., additional, Kilic, Y., additional, Gomes Júnior, A. R., additional, Camargo, J. I. B., additional, Emilio, M., additional, Vara-Lubiano, M., additional, Kretlow, M., additional, Albert, L., additional, Alcock, C., additional, Ball, J. G., additional, Bender, K., additional, Buie, M. W., additional, Butterfield, K., additional, Camarca, M., additional, Castro-Chacón, J. H., additional, Dunford, R., additional, Fisher, R. S., additional, Gamble, D., additional, Geary, J. C., additional, Gnilka, C. L., additional, Green, K. D., additional, Hartman, Z. D., additional, Huang, C.-K., additional, Januszewski, H., additional, Johnston, J., additional, Kagitani, M., additional, Kamin, R., additional, Kavelaars, J. J., additional, Keller, J. M., additional, de Kleer, K. R., additional, Lehner, M. J., additional, Luken, A., additional, Marchis, F., additional, Marlin, T., additional, McGregor, K., additional, Nikitin, V., additional, Nolthenius, R., additional, Patrick, C., additional, Redfield, S., additional, Rengstorf, A. W., additional, Reyes-Ruiz, M., additional, Seccull, T., additional, Skrutskie, M. F., additional, Smith, A. B., additional, Sproul, M., additional, Stephens, A. W., additional, Szentgyorgyi, A., additional, Sánchez-Sanjuán, S., additional, Tatsumi, E., additional, Verbiscer, A., additional, Wang, S.-Y., additional, Yoshida, F., additional, Young, R., additional, and Zhang, Z.-W., additional
Published: 2023
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32. A dense ring of the trans-Neptunian object Quaoar outside its Roche limit

Author: Morgado, B. E. (B. E.), Sicardy, B. (B.), Braga-Ribas, F. (F.), Ortiz, J. L. (J. L.), Salo, H. (H.), Vachier, F. (F.), Desmars, J. (J.), Pereira, C. L. (C. L.), Santos-Sanz, P. (P.), Sfair, R. (R.), de Santana, T. (T.), Assafin, M. (M.), Vieira-Martins, R. (R.), Gomes-Júnior, A. R. (A. R.), Margoti, G. (G.), Dhillon, V. S. (V. S.), Fernández-Valenzuela, E. (E.), Broughton, J. (J.), Bradshaw, J. (J.), Langersek, R. (R.), Benedetti-Rossi, G. (G.), Souami, D. (D.), Holler, B. J. (B. J.), Kretlow, M. (M.), Boufleur, R. C. (R. C.), Camargo, J. I. (J. I. B.), Duffard, R. (R.), Beisker, W. (W.), Morales, N. (N.), Lecacheux, J. (J.), Rommel, F. L. (F. L.), Herald, D. (D.), Benz, W. (W.), Jehin, E. (E.), Jankowsky, F. (F.), Marsh, T. R. (T. R.), Littlefair, S. P. (S. P.), Bruno, G. (G.), Pagano, I. (I.), Brandeker, A. (A.), Collier-Cameron, A. (A.), Florén, H. G. (H. G.), Hara, N. (N.), Olofsson, G. (G.), Wilson, T. G. (T. G.), Benkhaldoun, Z. (Z.), Busuttil, R. (R.), Burdanov, A. (A.), Ferrais, M. (M.), Gault, D. (D.), Gillon, M. (M.), Hanna, W. (W.), Kerr, S. (S.), Kolb, U. (U.), Nosworthy, P. (P.), Sebastian, D. (D.), Snodgrass, C. (C.), Teng, J. P. (J. P.), de Wit, J. (J.), Morgado, B. E. (B. E.), Sicardy, B. (B.), Braga-Ribas, F. (F.), Ortiz, J. L. (J. L.), Salo, H. (H.), Vachier, F. (F.), Desmars, J. (J.), Pereira, C. L. (C. L.), Santos-Sanz, P. (P.), Sfair, R. (R.), de Santana, T. (T.), Assafin, M. (M.), Vieira-Martins, R. (R.), Gomes-Júnior, A. R. (A. R.), Margoti, G. (G.), Dhillon, V. S. (V. S.), Fernández-Valenzuela, E. (E.), Broughton, J. (J.), Bradshaw, J. (J.), Langersek, R. (R.), Benedetti-Rossi, G. (G.), Souami, D. (D.), Holler, B. J. (B. J.), Kretlow, M. (M.), Boufleur, R. C. (R. C.), Camargo, J. I. (J. I. B.), Duffard, R. (R.), Beisker, W. (W.), Morales, N. (N.), Lecacheux, J. (J.), Rommel, F. L. (F. L.), Herald, D. (D.), Benz, W. (W.), Jehin, E. (E.), Jankowsky, F. (F.), Marsh, T. R. (T. R.), Littlefair, S. P. (S. P.), Bruno, G. (G.), Pagano, I. (I.), Brandeker, A. (A.), Collier-Cameron, A. (A.), Florén, H. G. (H. G.), Hara, N. (N.), Olofsson, G. (G.), Wilson, T. G. (T. G.), Benkhaldoun, Z. (Z.), Busuttil, R. (R.), Burdanov, A. (A.), Ferrais, M. (M.), Gault, D. (D.), Gillon, M. (M.), Hanna, W. (W.), Kerr, S. (S.), Kolb, U. (U.), Nosworthy, P. (P.), Sebastian, D. (D.), Snodgrass, C. (C.), Teng, J. P. (J. P.), and de Wit, J. (J.)
Abstract: Planetary rings are observed not only around giant planets¹, but also around small bodies such as the Centaur Chariklo² and the dwarf planet Haumea³. Up to now, all known dense rings were located close enough to their parent bodies, being inside the Roche limit, where tidal forces prevent material with reasonable densities from aggregating into a satellite. Here we report observations of an inhomogeneous ring around the trans-Neptunian body (50000) Quaoar. This trans-Neptunian object has an estimated radius⁴ of 555 km and possesses a roughly 80-km satellite⁵ (Weywot) that orbits at 24 Quaoar radii⁶,⁷. The detected ring orbits at 7.4 radii from the central body, which is well outside Quaoar’s classical Roche limit, thus indicating that this limit does not always determine where ring material can survive. Our local collisional simulations show that elastic collisions, based on laboratory experiments⁸, can maintain a ring far away from the body. Moreover, Quaoar’s ring orbits close to the 1/3 spin–orbit resonance9 with Quaoar, a property shared by Chariklo’s ²,¹⁰,¹¹ and Haumea’s³ rings, suggesting that this resonance plays a key role in ring confinement for small bodies.
Published: 2023

33. A dense ring of the trans-Neptunian object Quaoar outside its Roche limit

Author: Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Research Council, European Commission, Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Morgado, B. E., Ortiz, José Luis, Santos Sanz, Pablo, Kretlow, M., Duffard, René D., Morales, Nicolás, de Wit, J., Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Research Council, European Commission, Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Morgado, B. E., Ortiz, José Luis, Santos Sanz, Pablo, Kretlow, M., Duffard, René D., Morales, Nicolás, and de Wit, J.
Abstract: Planetary rings are observed not only around giant planets1, but also around small bodies such as the Centaur Chariklo2 and the dwarf planet Haumea3. Up to now, all known dense rings were located close enough to their parent bodies, being inside the Roche limit, where tidal forces prevent material with reasonable densities from aggregating into a satellite. Here we report observations of an inhomogeneous ring around the trans-Neptunian body (50000) Quaoar. This trans-Neptunian object has an estimated radius4 of 555 km and possesses a roughly 80-km satellite5 (Weywot) that orbits at 24 Quaoar radii6,7. The detected ring orbits at 7.4 radii from the central body, which is well outside Quaoar’s classical Roche limit, thus indicating that this limit does not always determine where ring material can survive. Our local collisional simulations show that elastic collisions, based on laboratory experiments8, can maintain a ring far away from the body. Moreover, Quaoar’s ring orbits close to the 1/3 spin–orbit resonance9 with Quaoar, a property shared by Chariklo’s2,10,11 and Haumea’s3 rings, suggesting that this resonance plays a key role in ring confinement for small bodies. © 2023, The Author(s), under exclusive licence to Springer Nature Limited.
Published: 2023

34. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author: Ortiz, J. L., Santos-Sanz, P., Sicardy, B., Benedetti-Rossi, G., Brard, D., Morales, N., Duffard, R., Braga-Ribas, F., Hopp, U., Ries, C., Nascimbeni, V., Marzari, F., Granata, V., Pl, A., Kiss, C., Pribulla, T., Komk, R., Hornoch, K., Pravec, P., Bacci, P., Maestripieri, M., Nerli, L., Mazzei, L., Bachini, M., Martinelli, F., Succi, G., Ciabattari, F., Mikuz, H., Carbognani, A., Gaehrken, B., Mottola, S., Hellmich, S., Rommel, F. L., Fernndez-Valenzuela, E., Bagatin, A. Campo, Cikota, S., Cikota, A., Lecacheux, J., Vieira-Martins, R., Camargo, J. I. B., Assafin, M., Colas, F., Behrend, R., Desmars, J., Meza, E., Alvarez-Candal, A., Beisker, W., Gomes-Junior, A. R., Morgado, B. E., Roques, F., Vachier, F., Berthier, J., Mueller, T. G., Madiedo, J. M., Unsalan, O., Sonbas, E., Karaman, N., Erece, O., Koseoglu, D. T., Ozisik, T., Kalkan, S., Guney, Y., Niaei, M. S., Satir, O., Yesilyaprak, C., Puskullu, C., Kabas, A., Demircan, O., Alikakos, J., Charmandaris, V., Leto, G., Ohlert, J., Christille, J. M., Szakts, R., Farkas, A. Takcsn, Varga-Vereblyi, E., Marton, G., Marciniak, A., Bartczak, P., Santana-Ros, T., Butkiewicz-Bk, M., Dudziski, G., Al-Lagoa, V., Gazeas, K., Tzouganatos, L., Paschalis, N., Tsamis, V., Snchez-Lavega, A., Prez-Hoyos, S., Hueso, R., Guirado, J. C., Peris, V., and Iglesias-Marzoa, R.
Subjects: Minor planets -- Observations, Planetary rings -- Observations, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract: Author(s): J. L. Ortiz (corresponding author) [1]; P. Santos-Sanz [1]; B. Sicardy [2]; G. Benedetti-Rossi [3]; D. Brard [2]; N. Morales [1]; R. Duffard [1]; F. Braga-Ribas [3, 4]; U. [...]
Published: 2017
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35. A dense ring of the trans-Neptunian object Quaoar outside its Roche limit

Author: Morgado, B E, Sicardy, B, Braga-Ribas, F, Ortiz, J L, Salo, H, Vachier, F, Desmars, J, Pereira, C L, Santos-Sanz, P, Sfair, R, de Santana, T, Assafin, M, Vieira-Martins, R, Gomes-Júnior, A R, Margoti, G, Dhillon, V S, Fernández-Valenzuela, E, Broughton, J, Bradshaw, J, Langersek, R, Benedetti-Rossi, G, Souami, D, Holler, B J, Kretlow, M, Boufleur, R C, Camargo, J I B, Duffard, R, Beisker, W, Morales, N, Lecacheux, J, Rommel, F L, Herald, D, Benz, Willy, Jehin, E, Jankowsky, F, Marsh, T R, Littlefair, S P, Bruno, G, Pagano, I, Brandeker, A, Collier-Cameron, A, Florén, H G, Hara, N, Olofsson, G, Wilson, T G, Benkhaldoun, Z, Busuttil, R, Burdanov, A, Ferrais, M, Gault, D, Gillon, M, Hanna, W, Kerr, S, Kolb, U, Nosworthy, P, Sebastian, D, Snodgrass, C, Teng, J P, de Wit, J, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Polytechnique des Sciences Avancées (IPSA), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. St Andrews Centre for Exoplanet Science, University of St Andrews. School of Physics and Astronomy, Ministerio de Ciencia e Innovación (España), Junta de Andalucía, European Research Council, European Commission, and Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil)
Subjects: MCC, QC Physics, Multidisciplinary, [SDU]Sciences of the Universe [physics], QB Astronomy, 520 Astronomie, 3rd-DAS, 530 Physik, AC, QC, QB
Abstract: Full list of authors: Morgado, B. E.; Sicardy, B.; Braga-Ribas, F.; Ortiz, J. L.; Salo, H.; Vachier, F.; Desmars, J.; Pereira, C. L.; Santos-Sanz, P.; Sfair, R.; de Santana, T.; Assafin, M.; Vieira-Martins, R.; Gomes-Junior, A. R.; Margoti, G.; Dhillon, V. S.; Fernandez-Valenzuela, E.; Broughton, J.; Bradshaw, J.; Langersek, R.; Benedetti-Rossi, G.; Souami, D.; Holler, B. J.; Kretlow, M.; Boufleur, R. C.; Camargo, J. I. B.; Duffard, R.; Beisker, W.; Morales, N.; Lecacheux, J.; Rommel, F. L.; Herald, D.; Benz, W.; Jehin, E.; Jankowsky, F.; Marsh, T. R.; Littlefair, S. P.; Bruno, G.; Pagano, I.; Brandeker, A.; Collier-Cameron, A.; Floren, H. G.; Hara, N.; Olofsson, G.; Wilson, T. G.; Benkhaldoun, Z.; Busuttil, R.; Burdanov, A.; Ferrais, M.; Gault, D.; Gillon, M.; Hanna, W.; Kerr, S.; Kolb, U.; Nosworthy, P.; Sebastian, D.; Snodgrass, C.; Teng, J. P.; de Wit, J., Planetary rings are observed not only around giant planets1, but also around small bodies such as the Centaur Chariklo2 and the dwarf planet Haumea3. Up to now, all known dense rings were located close enough to their parent bodies, being inside the Roche limit, where tidal forces prevent material with reasonable densities from aggregating into a satellite. Here we report observations of an inhomogeneous ring around the trans-Neptunian body (50000) Quaoar. This trans-Neptunian object has an estimated radius4 of 555 km and possesses a roughly 80-km satellite5 (Weywot) that orbits at 24 Quaoar radii6,7. The detected ring orbits at 7.4 radii from the central body, which is well outside Quaoar’s classical Roche limit, thus indicating that this limit does not always determine where ring material can survive. Our local collisional simulations show that elastic collisions, based on laboratory experiments8, can maintain a ring far away from the body. Moreover, Quaoar’s ring orbits close to the 1/3 spin–orbit resonance9 with Quaoar, a property shared by Chariklo’s2,10,11 and Haumea’s3 rings, suggesting that this resonance plays a key role in ring confinement for small bodies. © 2023, The Author(s), under exclusive licence to Springer Nature Limited., This work was carried out under the Lucky Star umbrella that agglomerates the efforts of the Paris, Granada and Rio teams, which is funded by the ERC under the European Community’s H2020 (ERC grant agreement no. 669416). Part of the results were obtained using CHEOPS data. CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden and the UK. The CHEOPS Consortium gratefully acknowledge the support received by all the agencies, offices, universities and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. The design and construction of HiPERCAM was supported by the ERC under the European Union’s Seventh Framework Programme (FP/2007-2013) under ERC-2013-ADG grant agreement no. 340040 (HiPERCAM). HiPERCAM operations and V.S.D. are funded by the Science and Technology Facilities Council (grant no. ST/V000853/1). The GTC is installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, on the island of La Palma. This work has made use of data from the 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). This study was financed in part by the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant no. 465376/2014-2). This study was financed in part by CAPES - Finance Code 001. The following authors acknowledge the respective (1) CNPq grants to B.E.M. no. 150612/2020-6; F.B.-R. no. 314772/2020-0; R.V.-M. no. 307368/2021-1; M.A. nos. 427700/2018-3, 310683/2017-3 and 473002/2013-2; and J.I.B.C. nos. 308150/2016-3 and 305917/2019-6. (2) CAPES/Cofecub grant to B.E.M. no. 394/2016-05. (3) FAPERJ grant no. M.A. E-26/111.488/2013. (4) FAPESP (Fundação de Amparo à Pesquisa do Estado de São Paulo) grants to A.R.G.-J. no. 2018/11239-8 and R.S. no. 2016/24561-0. (5) CAPES-PrInt Program grant to G.B.-R. no. 88887.310463/2018-00, mobility number 88887.571156/2020-00. (6) DFG (the German Research Foundation) grant to R.S. no. 446102036. P.S-S. and R.D. acknowledge financial support by the Spanish grant no. AYA-RTI2018-098657-J-I00 ‘LEO-SBNAF’ (MCIU/AEI/FEDER, UE). J.L.O., P.S-S., R.D. and N.M. 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 Astrofísica de Andalucía (grant no. SEV-2017-0709), and they also acknowledge the financial support by the Spanish grant nos. AYA-2017-84637-R and PID2020-112789GB-I00, and the Proyectos de Excelencia de la Junta de Andalucía grant nos. 2012-FQM1776 and PY20-01309. G.B-R. and I.P. acknowledge support from CHEOPS ASI-INAF agreement no. 2019-29-HH.0. A.B. was supported by the SNSA. A.C.-C. and T.G.W. acknowledge support from STFC consolidated grant nos. ST/R000824/1 and ST/V000861/1, and UK Space Agency grant no. ST/R003203/1. U.K. and R.B. acknowledge support by The OpenSTEM Laboratories, an initiative funded by the Higher Education Funding Council for England and the Wolfson Foundation. J.W. gratefully acknowledges financial support from the Heising-Simons Foundation, C. Masson and P. 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 agreement no. 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. TRAPPIST is a project funded by the Belgian Fonds (National) de la Recherche Scientique (F.R.S.-FNRS) under grant no. PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege, in collaboration with the Cadi Ayyad University of Marrakech (Morocco). E.J. is FNRS Senior Research Associate., With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).
Published: 2023
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36. Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation

Author: Santos-Sanz, P., primary, Ortiz, J. L., additional, Sicardy, B., additional, Popescu, M., additional, Benedetti-Rossi, G., additional, Morales, N., additional, Vara-Lubiano, M., additional, Camargo, J. I. B., additional, Pereira, C. L., additional, Rommel, F. L., additional, Assafin, M., additional, Desmars, J., additional, Braga-Ribas, F., additional, Duffard, R., additional, Marques Oliveira, J., additional, Vieira-Martins, R., additional, Fernández-Valenzuela, E., additional, Morgado, B. E., additional, Acar, M., additional, Anghel, S., additional, Atalay, E., additional, Ateş, A., additional, Bakiş, H., additional, Bakis, V., additional, Eker, Z., additional, Erece, O., additional, Kaspi, S., additional, Kayhan, C., additional, Kilic, S. E., additional, Kilic, Y., additional, Manulis, I., additional, Nedelcu, D. A., additional, Niaei, M. S., additional, Nir, G., additional, Ofek, E., additional, Ozisik, T., additional, Petrescu, E., additional, Satir, O., additional, Solmaz, A., additional, Sonka, A., additional, Tekes, M., additional, Unsalan, O., additional, Yesilyaprak, C., additional, Anghel, R., additional, Berteşteanu, D., additional, Curelaru, L., additional, Danescu, C., additional, Dumitrescu, V., additional, Gherase, R., additional, Hudin, L., additional, Stoian, A-M., additional, Tercu, J. O., additional, Truta, R., additional, Turcu, V., additional, Vantdevara, C., additional, Belskaya, I., additional, Dementiev, T. O., additional, Gazeas, K., additional, Karampotsiou, S., additional, Kashuba, V., additional, Kiss, Cs., additional, Koshkin, N., additional, Kozhukhov, O. M., additional, Krugly, Y., additional, Lecacheux, J., additional, Pal, A., additional, Püsküllü, Ç., additional, Szakats, R., additional, Zhukov, V., additional, Bamberger, D., additional, Mondon, B., additional, Perelló, C., additional, Pratt, A., additional, Schnabel, C., additional, Selva, A., additional, Teng, J. P., additional, Tigani, K., additional, Tsamis, V., additional, Weber, C., additional, Wells, G., additional, Kalkan, S., additional, Kudak, V., additional, Marciniak, A., additional, Ogloza, W., additional, Özdemir, T., additional, Pakštiene, E., additional, Perig, V., additional, and Żejmo, M., additional
Published: 2022
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37. A stellar occultation by the transneptunian object (50000) Quaoar observed by CHEOPS

Author: Morgado, B. E., primary, Bruno, G., additional, Gomes-Júnior, A. R., additional, Pagano, I., additional, Sicardy, B., additional, Fortier, A., additional, Desmars, J., additional, Maxted, P. F. L., additional, Braga-Ribas, F., additional, Queloz, D., additional, Sousa, S. G., additional, Ortiz, J. L., additional, Brandeker, A., additional, Collier Cameron, A., additional, Pereira, C. L., additional, Florén, H. G., additional, Hara, N., additional, Souami, D., additional, Isaak, K. G., additional, Olofsson, G., additional, Santos-Sanz, P., additional, Wilson, T. G., additional, Broughton, J., additional, Alibert, Y., additional, Alonso, R., additional, Anglada, G., additional, Bárczy, T., additional, Barrado, D., additional, Barros, S. C. C., additional, Baumjohann, W., additional, Beck, M., additional, Beck, T., additional, Benz, W., additional, Billot, N., additional, Bonfils, X., additional, Broeg, C., additional, Cabrera, J., additional, Charnoz, S., additional, Csizmadia, S., additional, Davies, M. B., additional, Deleuil, M., additional, Delrez, L., additional, Demangeon, O. D. S., additional, Demory, B. O., additional, Ehrenreich, D., additional, Erikson, A., additional, Fossati, L., additional, Fridlund, M., additional, Gandolfi, D., additional, Gillon, M., additional, Güdel, M., additional, Heng, K., additional, Hoyer, S., additional, Kiss, L. L., additional, Laskar, J., additional, Lecavelier des Etangs, A., additional, Lendl, M., additional, Lovis, C., additional, Magrin, D., additional, Marafatto, L., additional, Nascimbeni, V., additional, Ottensamer, R., additional, Pallé, E., additional, Peter, G., additional, Piazza, D., additional, Piotto, G., additional, Pollacco, D., additional, Ragazzoni, R., additional, Rando, N., additional, Ratti, F., additional, Rauer, H., additional, Reimers, C., additional, Ribas, I., additional, Santos, N. C., additional, Scandariato, G., additional, Ségransan, D., additional, Simon, A. E., additional, Smith, A. M. S., additional, Steller, M., additional, Szabó, G. M., additional, Thomas, N., additional, Udry, S., additional, Van Grootel, V., additional, Walton, N. A., additional, and Westerdorff, K., additional
Published: 2022
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38. Occultation portal: A web-based platform for data collection and analysis of stellar occultations

Author: Kilic, Y, primary, Braga-Ribas, F, additional, Kaplan, M, additional, Erece, O, additional, Souami, D, additional, Dindar, M, additional, Desmars, J, additional, Sicardy, B, additional, Morgado, B E, additional, Shameoni, M N, additional, Rommel, F L, additional, and Gomes-Júnior, A R, additional
Published: 2022
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39. Milliarcsecond Astrometry for the Galilean Moons Using Stellar Occultations

Author: Morgado, B. E., primary, Gomes-Júnior, A. R., additional, Braga-Ribas, F., additional, Vieira-Martins, R., additional, Desmars, J., additional, Lainey, V., additional, D’aversa, E., additional, Dunham, D., additional, Moore, J., additional, Baillié, K., additional, Herald, D., additional, Assafin, M., additional, Sicardy, B., additional, Aoki, S., additional, Bardecker, J., additional, Barton, J., additional, Blank, T., additional, Bruns, D., additional, Carlson, N., additional, Carlson, R. W., additional, Cobble, K., additional, Dunham, J., additional, Eisfeldt, D., additional, Emilio, M., additional, Jacques, C., additional, Hinse, T. C., additional, Kim, Y., additional, Malacarne, M., additional, Maley, P. D., additional, Maury, A., additional, Meza, E., additional, Oliva, F., additional, Orton, G. S., additional, Pereira, C. L., additional, Person, M., additional, Plainaki, C., additional, Sfair, R., additional, Sindoni, G., additional, Smith, M., additional, Sussenbach, E., additional, Stuart, P., additional, Vrolijk, J., additional, and Winter, O. C., additional
Published: 2022
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40. Constraints on the structure and seasonal variations of Triton’s atmosphere from the 5 October 2017 stellar occultation and previous observations

Author: Marques Oliveira, J., primary, Sicardy, B., additional, Gomes-Júnior, A. R., additional, Ortiz, J. L., additional, Strobel, D. F., additional, Bertrand, T., additional, Forget, F., additional, Lellouch, E., additional, Desmars, J., additional, Bérard, D., additional, Doressoundiram, A., additional, Lecacheux, J., additional, Leiva, R., additional, Meza, E., additional, Roques, F., additional, Souami, D., additional, Widemann, T., additional, Santos-Sanz, P., additional, Morales, N., additional, Duffard, R., additional, Fernández-Valenzuela, E., additional, Castro-Tirado, A. J., additional, Braga-Ribas, F., additional, Morgado, B. E., additional, Assafin, M., additional, Camargo, J. I. B., additional, Vieira-Martins, R., additional, Benedetti-Rossi, G., additional, Santos-Filho, S., additional, Banda-Huarca, M. V., additional, Quispe-Huaynasi, F., additional, Pereira, C. L., additional, Rommel, F. L., additional, Margoti, G., additional, Dias-Oliveira, A., additional, Colas, F., additional, Berthier, J., additional, Renner, S., additional, Hueso, R., additional, Pérez-Hoyos, S., additional, Sánchez-Lavega, A., additional, Rojas, J. F., additional, Beisker, W., additional, Kretlow, M., additional, Herald, D., additional, Gault, D., additional, Bath, K.-L., additional, Bode, H.-J., additional, Bredner, E., additional, Guhl, K., additional, Haymes, T. V., additional, Hummel, E., additional, Kattentidt, B., additional, Klös, O., additional, Pratt, A., additional, Thome, B., additional, Avdellidou, C., additional, Gazeas, K., additional, Karampotsiou, E., additional, Tzouganatos, L., additional, Kardasis, E., additional, Christou, A. A., additional, Xilouris, E. M., additional, Alikakos, I., additional, Gourzelas, A., additional, Liakos, A., additional, Charmandaris, V., additional, Jelínek, M., additional, Štrobl, J., additional, Eberle, A., additional, Rapp, K., additional, Gährken, B., additional, Klemt, B., additional, Kowollik, S., additional, Bitzer, R., additional, Miller, M., additional, Herzogenrath, G., additional, Frangenberg, D., additional, Brandis, L., additional, Pütz, I., additional, Perdelwitz, V., additional, Piehler, G. M., additional, Riepe, P., additional, von Poschinger, K., additional, Baruffetti, P., additional, Cenadelli, D., additional, Christille, J.-M., additional, Ciabattari, F., additional, Di Luca, R., additional, Alboresi, D., additional, Leto, G., additional, Zanmar Sanchez, R., additional, Bruno, P., additional, Occhipinti, G., additional, Morrone, L., additional, Cupolino, L., additional, Noschese, A., additional, Vecchione, A., additional, Scalia, C., additional, Lo Savio, R., additional, Giardina, G., additional, Kamoun, S., additional, Barbosa, R., additional, Behrend, R., additional, Spano, M., additional, Bouchet, E., additional, Cottier, M., additional, Falco, L., additional, Gallego, S., additional, Tortorelli, L., additional, Sposetti, S., additional, Sussenbach, J., additional, Van Den Abbeel, F., additional, André, P., additional, Llibre, M., additional, Pailler, F., additional, Ardissone, J., additional, Boutet, M., additional, Sanchez, J., additional, Bretton, M., additional, Cailleau, A., additional, Pic, V., additional, Granier, L., additional, Chauvet, R., additional, Conjat, M., additional, Dauvergne, J. L., additional, Dechambre, O., additional, Delay, P., additional, Delcroix, M., additional, Rousselot, L., additional, Ferreira, J., additional, Machado, P., additional, Tanga, P., additional, Rivet, J.-P., additional, Frappa, E., additional, Irzyk, M., additional, Jabet, F., additional, Kaschinski, M., additional, Klotz, A., additional, Rieugnie, Y., additional, Klotz, A. N., additional, Labrevoir, O., additional, Lavandier, D., additional, Walliang, D., additional, Leroy, A., additional, Bouley, S., additional, Lisciandra, S., additional, Coliac, J.-F., additional, Metz, F., additional, Erpelding, D., additional, Nougayrède, P., additional, Midavaine, T., additional, Miniou, M., additional, Moindrot, S., additional, Morel, P., additional, Reginato, B., additional, Reginato, E., additional, Rudelle, J., additional, Tregon, B., additional, Tanguy, R., additional, David, J., additional, Thuillot, W., additional, Hestroffer, D., additional, Vaudescal, G., additional, Baba Aissa, D., additional, Grigahcene, Z., additional, Briggs, D., additional, Broadbent, S., additional, Denyer, P., additional, Haigh, N. J., additional, Quinn, N., additional, Thurston, G., additional, Fossey, S. J., additional, Arena, C., additional, Jennings, M., additional, Talbot, J., additional, Alonso, S., additional, Román Reche, A., additional, Casanova, V., additional, Briggs, E., additional, Iglesias-Marzoa, R., additional, Abril Ibáñez, J., additional, Díaz Martín, M. C., additional, González, H., additional, Maestre García, J. L., additional, Marchant, J., additional, Ordonez-Etxeberria, I., additional, Martorell, P., additional, Salamero, J., additional, Organero, F., additional, Ana, L., additional, Fonseca, F., additional, Peris, V., additional, Brevia, O., additional, Selva, A., additional, Perello, C., additional, Cabedo, V., additional, Gonçalves, R., additional, Ferreira, M., additional, Marques Dias, F., additional, Daassou, A., additional, Barkaoui, K., additional, Benkhaldoun, Z., additional, Guennoun, M., additional, Chouqar, J., additional, Jehin, E., additional, Rinner, C., additional, Lloyd, J., additional, El Moutamid, M., additional, Lamarche, C., additional, Pollock, J. T., additional, Caton, D. B., additional, Kouprianov, V., additional, Timerson, B. W., additional, Blanchard, G., additional, Payet, B., additional, Peyrot, A., additional, Teng-Chuen-Yu, J.-P., additional, Françoise, J., additional, Mondon, B., additional, Payet, T., additional, Boissel, C., additional, Castets, M., additional, Hubbard, W. B., additional, Hill, R., additional, Reitsema, H. J., additional, Mousis, O., additional, Ball, L., additional, Neilsen, G., additional, Hutcheon, S., additional, Lay, K., additional, Anderson, P., additional, Moy, M., additional, Jonsen, M., additional, Pink, I., additional, Walters, R., additional, and Downs, B., additional
Published: 2022
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41. VizieR Online Data Catalog: Triton light curves from 05/10/2017 (Marques Oliveira+, 2022)

Author: Marques Oliveira, J., Sicardy, B., Gomes-Junior, A. R., Ortiz, J. L., Strobel, D. F., Bertrand, T., Forget, F., Lellouch, E., Desmars, J., Berard, D., Doressoundiram, A., Lecacheux, J., Leiva, R., Meza, E., Roques, F., Souami, D., Widemann, T., Santos-Sanz, P., Morales, N., Duffard, R., Fernandez-Valenzuela, E., Castro-Tirado, A. J., Braga-Ribas, F., Morgado, B. E., Assafin, M., Camargo, J. I. B., Vieira-Martins, R., Benedetti-Rossi, G., Santos-Filho, S., Banda-Huarca, M. V., Quispe-Huaynasi, F., Pereira, C. L., Rommel, F. L., Margoti, G., Dias-Oliveira, A., Colas, F., Berthier, J., Renner, S., Hueso, R., Perez-Hoyos, S., Sanchez-Lavega, A., Rojas, J. F., Beisker, W., Kretlow, M., Herald, D., Gault, D., Bath, K.-L., Bode, H.-J., Bredner, E., Guhl, K., Haymes, T. V., Hummel, E., Kattentidt, B., Klos, O., Pratt, A., Thome, B., Avdellidou, C., Gazeas, K., Karampotsiou, E., Tzouganatos, L., Kardasis, E., Christou, A. A., Xilouris, E. M., Alikakos, I., Gourzelas, A., Liakos, A., Charmandaris, V., Jelinek, M., Strobl, J., Eberle, A., Rapp, K., Gahrken, B., Kowo Llik, S., Bitzer, R., Miller, M., Herzogenrath, G., Frangenberg, D., Brandis, L., Puetz, I., Perdelwitz, V., Piehler, G. M., Riepe, P., von Poschinger, K., Baruffetti, P., Cenadelli, D., Christille, J.-M., Ciabattari, F., Di, Luca R., Alboresi, D., Leto, G., Zanmar Sanchez, R., Bruno, P., Occhipinti, G., Morrone, L., Cupolino, L., Noschese, A., Vecchione, A., Scalia, C., Lo Savio, R., Giardina, G., Kamoun, S., Barbosa, R., Behrend, R., Spano, M., Bouchet, E., Cottier, M., Falco, L., Gallego, S., Tortorelli, L., Sposetti, S., Sussenbach, J., van den Abbeel, F., Andre, P., Llibre, M., Pailler, F., Ardissone, J., Boutet, M., Sanchez, J., Bretton, M., Cailleau, A., Pic, V., Granier, L., Chauvet, R., Conjat, M., Dauvergne, J. L., Dechambre, O., Delay, P., Delcroix, M., Rousselot, L., Ferreira, J., Machado, P., Tanga, P., Rivet, J.-P., Frappa, E., Irzyk, M., Jabet, F., Kaschinski, M., Klotz, A., Rieugnie, Y., Klotz, A. N., Labrevoir, O., Lavandier, D., Walliang, D., Leroy, A., Bouley, S., Lisciandra, S., Coliac, J.-F., Metz, F., Erpelding, D., Nougayrede, P., Miniou, M., Moindrot, S., Morel, P., Reginato, B., Reginato, E., Rudelle, J., Tregon, B., Tanguy, R., David, J., Thuillot, W., Hestroffer, D., Vaudescal, G., Baba Aissa, D., Grigahcene, Z., Briggs, D., Broadbent, S., Denyer, P., Haigh, N. J., Quinn, N., Thurston, G., Fossey, S. J., Arena, C., Jennings, M., Talbot, J., Alonso, S., Roman Reche, A., Casanova, V., Briggs, E., Iglesias-Marzoa, R., Abril Ibanez, J., Diaz, Martin M. C., Gonzalez, H., Maestre Garcia, J. L., Marchant, J., Ordonez-Etxeberria, I., Martorell, P., Salamero, J., Organero, F., Ana, L., Fonseca, F., Peris, V., Brevia, O., Selva, A., Perello, C., Cabedo, V., Goncalves, R., Ferreira, M., Marques Dias, F., Daassou, A., Barkaoui, K., Benkhaldoun, Z., Guennoun, M., Chouqar, J., Jehin, E., Rinner, C., Lloyd, J., El Moutamid, M., Lamarche, C., Pollock, J. T., Caton, D. B., Kouprianov, V., Timerson, B. W., Blanchard, G., Payet, B., Peyrot, A., Teng-Chuen-Yu, J.-P., Francoise, J., Mondon, B., Payet, T., Boissel, C., Castets, M., Hubbard, W. B., Hill, R., Reitsema, H. J., Mousis, O., Ball, L., Hutcheon, S., Lay, K., Anderson, P., Moy, M., Jonsen, M., Pink, I., Walters, R., Downs, B., Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Photometry, Planets, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Solar system
Abstract: International audience; The data provided features all light curves from the 5 October 2017 event. The names of the files are the same names, in lower caps and with no spaces, that are presented in Figures C.1 and C.2. The first column of all files is the time in seconds, starting on 5 October 2017 00:00:00 UTC. The second column of all files is the normalised flux, where the unocculted flux oscillates around 1. (2 data files).
Published: 2022

42. SORA: Stellar occultation reduction and analysis

Author: Gomes-Júnior, A R, primary, Morgado, B E, additional, Benedetti-Rossi, G, additional, Boufleur, R C, additional, Rommel, F L, additional, Banda-Huarca, M V, additional, Kilic, Y, additional, Braga-Ribas, F, additional, and Sicardy, B, additional
Published: 2022
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43. Refined physical parameters for Chariklo’s body and rings from stellar occultations observed between 2013 and 2020

Author: Morgado, B. E., primary, Sicardy, B., additional, Braga-Ribas, F., additional, Desmars, J., additional, Gomes-Júnior, A. R., additional, Bérard, D., additional, Leiva, R., additional, Ortiz, J. L., additional, Vieira-Martins, R., additional, Benedetti-Rossi, G., additional, Santos-Sanz, P., additional, Camargo, J. I. B., additional, Duffard, R., additional, Rommel, F. L., additional, Assafin, M., additional, Boufleur, R. C., additional, Colas, F., additional, Kretlow, M., additional, Beisker, W., additional, Sfair, R., additional, Snodgrass, C., additional, Morales, N., additional, Fernández-Valenzuela, E., additional, Amaral, L. S., additional, Amarante, A., additional, Artola, R. A., additional, Backes, M., additional, Bath, K.-L., additional, Bouley, S., additional, Buie, M. W., additional, Cacella, P., additional, Colazo, C. A., additional, Colque, J. P., additional, Dauvergne, J.-L., additional, Dominik, M., additional, Emilio, M., additional, Erickson, C., additional, Evans, R., additional, Fabrega-Polleri, J., additional, Garcia-Lambas, D., additional, Giacchini, B. L., additional, Hanna, W., additional, Herald, D., additional, Hesler, G., additional, Hinse, T. C., additional, Jacques, C., additional, Jehin, E., additional, Jørgensen, U. G., additional, Kerr, S., additional, Kouprianov, V., additional, Levine, S. E., additional, Linder, T., additional, Maley, P. D., additional, Machado, D. I., additional, Maquet, L., additional, Maury, A., additional, Melia, R., additional, Meza, E., additional, Mondon, B., additional, Moura, T., additional, Newman, J., additional, Payet, T., additional, Pereira, C. L., additional, Pollock, J., additional, Poltronieri, R. C., additional, Quispe-Huaynasi, F., additional, Reichart, D., additional, de Santana, T., additional, Schneiter, E. M., additional, Sieyra, M. V., additional, Skottfelt, J., additional, Soulier, J. F., additional, Starck, M., additional, Thierry, P., additional, Torres, P. J., additional, Trabuco, L. L., additional, Unda-Sanzana, E., additional, Yamashita, T. A. R., additional, Winter, O. C., additional, Zapata, A., additional, and Zuluaga, C. A., additional
Published: 2021
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44. Stellar occultations enable milliarcsecond astrometry for Trans-Neptunian objects and Centaurs

Author: Rommel, F. L., primary, Braga-Ribas, F., additional, Desmars, J., additional, Camargo, J. I. B., additional, Ortiz, J. L., additional, Sicardy, B., additional, Vieira-Martins, R., additional, Assafin, M., additional, Santos-Sanz, P., additional, Duffard, R., additional, Fernández-Valenzuela, E., additional, Lecacheux, J., additional, Morgado, B. E., additional, Benedetti-Rossi, G., additional, Gomes-Júnior, A. R., additional, Pereira, C. L., additional, Herald, D., additional, Hanna, W., additional, Bradshaw, J., additional, Morales, N., additional, Brimacombe, J., additional, Burtovoi, A., additional, Carruthers, T., additional, de Barros, J. R., additional, Fiori, M., additional, Gilmore, A., additional, Hooper, D., additional, Hornoch, K., additional, Jacques, C., additional, Janik, T., additional, Kerr, S., additional, Kilmartin, P., additional, Winkel, Jan Maarten, additional, Naletto, G., additional, Nardiello, D., additional, Nascimbeni, V., additional, Newman, J., additional, Ossola, A., additional, Pál, A., additional, Pimentel, E., additional, Pravec, P., additional, Sposetti, S., additional, Stechina, A., additional, Szakáts, R., additional, Ueno, Y., additional, Zampieri, L., additional, Broughton, J., additional, Dunham, J. B., additional, Dunham, D. W., additional, Gault, D., additional, Hayamizu, T., additional, Hosoi, K., additional, Jehin, E., additional, Jones, R., additional, Kitazaki, K., additional, Komžík, R., additional, Marciniak, A., additional, Maury, A., additional, Mikuž, H., additional, Nosworthy, P., additional, Fábrega Polleri, J., additional, Rahvar, S., additional, Sfair, R., additional, Siqueira, P. B., additional, Snodgrass, C., additional, Sogorb, P., additional, Tomioka, H., additional, Tregloan-Reed, J., additional, and Winter, O. C., additional
Published: 2020
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45. The first observed stellar occultations by the irregular satellite Phoebe (Saturn IX) and improved rotational period

Author: Gomes-Júnior, A R, primary, Assafin, M, additional, Braga-Ribas, F, additional, Benedetti-Rossi, G, additional, Morgado, B E, additional, Camargo, J I B, additional, Vieira-Martins, R, additional, Desmars, J, additional, Sicardy, B, additional, Barry, T, additional, Campbell-White, J, additional, Fernández-Lajús, E, additional, Giles, D, additional, Hanna, W, additional, Hayamizu, T, additional, Hirose, T, additional, De Horta, A, additional, Horvat, R, additional, Hosoi, K, additional, Jehin, E, additional, Kerr, S, additional, Machado, D I, additional, Mammana, L A, additional, Maybour, D, additional, Owada, M, additional, Rahvar, S, additional, and Snodgrass, C, additional
Published: 2019
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46. Mutual approximations between the five main moons of Uranus

Author: Santos-Filho, S, primary, Assafin, M, additional, Morgado, B E, additional, Vieira-Martins, R, additional, Camargo, J I B, additional, Gomes-Júnior, A R, additional, and Benedetti-Rossi, G, additional
Published: 2019
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47. The first observed stellar occultations by the irregular satellite Phoebe (Saturn IX) and improved rotational period.

Author: Gomes-Júnior, A R, Assafin, M, Braga-Ribas, F, Benedetti-Rossi, G, Morgado, B E, Camargo, J I B, Vieira-Martins, R, Desmars, J, Sicardy, B, Barry, T, Campbell-White, J, Fernández-Lajús, E, Giles, D, Hanna, W, Hayamizu, T, Hirose, T, De Horta, A, Horvat, R, Hosoi, K, and Jehin, E
Subjects: OCCULTATIONS (Astronomy), NATURAL satellites, LIGHT curves, LONGITUDE, ROTATIONAL motion
Abstract: We report six stellar occultations by Phoebe (Saturn IX), an irregular satellite of Saturn, obtained between mid-2017 and mid-2019. The 2017 July 6 event was the first stellar occultation by an irregular satellite ever observed. The occultation chords were compared to a 3D shape model of the satellite obtained from Cassini observations. The rotation period available in the literature led to a sub-observer point at the moment of the observed occultations where the chords could not fit the 3D model. A procedure was developed to identify the correct sub-observer longitude. It allowed us to obtain the rotation period with improved precision compared to the currently known value from literature. We show that the difference between the observed and the predicted sub-observer longitude suggests two possible solutions for the rotation period. By comparing these values with recently observed rotational light curves and single-chord stellar occultations, we can identify the best solution for Phoebe's rotational period as 9.27365 ± 0.00002 h. From the stellar occultations, we also obtained six geocentric astrometric positions in the ICRS as realized by the Gaia DR2 with uncertainties at the 1-mas level. [ABSTRACT FROM AUTHOR]
Published: 2020
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48. The PHEMU15 catalogue and astrometric results of the Jupiter's Galilean satellite mutual occultation and eclipse observations made in 2014–2015

Author: Saquet, E, primary, Emelyanov, N, additional, Robert, V, additional, Arlot, J-E, additional, Anbazhagan, P, additional, Baillié, K, additional, Bardecker, J, additional, Berezhnoy, A A, additional, Bretton, M, additional, Campos, F, additional, Capannoli, L, additional, Carry, B, additional, Castet, M, additional, Charbonnier, Y, additional, Chernikov, M M, additional, Christou, A, additional, Colas, F, additional, Coliac, J-F, additional, Dangl, G, additional, Dechambre, O, additional, Delcroix, M, additional, Dias-Oliveira, A, additional, Drillaud, C, additional, Duchemin, Y, additional, Dunford, R, additional, Dupouy, P, additional, Ellington, C, additional, Fabre, P, additional, Filippov, V A, additional, Finnegan, J, additional, Foglia, S, additional, Font, D, additional, Gaillard, B, additional, Galli, G, additional, Garlitz, J, additional, Gasmi, A, additional, Gaspar, H S, additional, Gault, D, additional, Gazeas, K, additional, George, T, additional, Gorda, S Y, additional, Gorshanov, D L, additional, Gualdoni, C, additional, Guhl, K, additional, Halir, K, additional, Hanna, W, additional, Henry, X, additional, Herald, D, additional, Houdin, G, additional, Ito, Y, additional, Izmailov, I S, additional, Jacobsen, J, additional, Jones, A, additional, Kamoun, S, additional, Kardasis, E, additional, Karimov, A M, additional, Khovritchev, M Y, additional, Kulikova, A M, additional, Laborde, J, additional, Lainey, V, additional, Lavayssiere, M, additional, Le Guen, P, additional, Leroy, A, additional, Loader, B, additional, Lopez, O C, additional, Lyashenko, A Y, additional, Lyssenko, P G, additional, Machado, D I, additional, Maigurova, N, additional, Manek, J, additional, Marchini, A, additional, Midavaine, T, additional, Montier, J, additional, Morgado, B E, additional, Naumov, K N, additional, Nedelcu, A, additional, Newman, J, additional, Ohlert, J M, additional, Oksanen, A, additional, Pavlov, H, additional, Petrescu, E, additional, Pomazan, A, additional, Popescu, M, additional, Pratt, A, additional, Raskhozhev, V N, additional, Resch, J-M, additional, Robilliard, D, additional, Roschina, E, additional, Rothenberg, E, additional, Rottenborn, M, additional, Rusov, S A, additional, Saby, F, additional, Saya, L F, additional, Selvakumar, G, additional, Signoret, F, additional, Slesarenko, V Y, additional, Sokov, E N, additional, Soldateschi, J, additional, Sonka, A, additional, Soulie, G, additional, Talbot, J, additional, Tejfel, V G, additional, Thuillot, W, additional, Timerson, B, additional, Toma, R, additional, Torsellini, S, additional, Trabuco, L L, additional, Traverse, P, additional, Tsamis, V, additional, Unwin, M, additional, Abbeel, F Van Den, additional, Vandenbruaene, H, additional, Vasundhara, R, additional, Velikodsky, Y I, additional, Vienne, A, additional, Vilar, J, additional, Vugnon, J-M, additional, Wuensche, N, additional, and Zeleny, P, additional
Published: 2017
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49. Size and Shape of Chariklo from Multi-epoch Stellar Occultations

Author: Leiva, R., primary, Sicardy, B., additional, Camargo, J. I. B., additional, Ortiz, J.-L., additional, Desmars, J., additional, Bérard, D., additional, Lellouch, E., additional, Meza, E., additional, Kervella, P., additional, Snodgrass, C., additional, Duffard, R., additional, Morales, N., additional, Gomes-Júnior, A. R., additional, Benedetti-Rossi, G., additional, Vieira-Martins, R., additional, Braga-Ribas, F., additional, Assafin, M., additional, Morgado, B. E., additional, Colas, F., additional, De Witt, C., additional, Sickafoose, A. A., additional, Breytenbach, H., additional, Dauvergne, J.-L., additional, Schoenau, P., additional, Maquet, L., additional, Bath, K.-L., additional, Bode, H.-J., additional, Cool, A., additional, Lade, B., additional, Kerr, S., additional, and Herald, D., additional
Published: 2017
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50. New orbits of irregular satellites designed for the predictions of stellar occultations up to 2020, based on thousands of new observations

Author: Gomes-Júnior, A. R., primary, Assafin, M., additional, Beauvalet, L., additional, Desmars, J., additional, Vieira-Martins, R., additional, Camargo, J. I. B., additional, Morgado, B. E., additional, and Braga-Ribas, F., additional
Published: 2016
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