adsabs/AstroCLIMB huggingface dataset:
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Color index c–o defined as a difference between magnitudes in cyan and orange ATLAS filters (abscissa) and slope of the phase curve (ordinate) for asteroids (i) that are nominally members of the Erigone family and (ii) for which the available photometric data allow us to determine their rotation state (i.e., sidereal rotation period and pole orientation). The distinct cluster of black points characterized by a small color index and large slope corresponds to Erigone family members with low albedo (these are listed in Table 1). Importantly, DJ—shown as a black square—appears to belong to this group. Additionally, there are five asteroids, identified by their numbers, clearly separated from the main cluster by having larger color index and smaller slope values. These are likely interlopers with high albedo and affinity to S-taxonomic class. As a result, we disregard them in our further analysis. The underlying red and blue points are known asteroids of S and C taxonomic class, respectively, projected onto these axes (compare with Figure 4 in J. Ďurech et al. 2020).
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Model prediction of the C parameter distribution dM(C; p) determined from test simulations, in which all asteroids were given the same absolute magnitude value H (color-coded with labels) and the parameters p were the best-fit set from the Yarkovsky/YORP chronology method. The latter used only H ≤ 17.5 Erigone dark members with their WISE-determined sizes. Here in each magnitude class we assigned sizes from H and 0.054 albedo value, and we pushed the tested H values beyond the 17.5 limit. In the simulations with H ≤ 17.5 we recover the two-hump dM(C; p) distribution fitting the data (gray symbols), but runs with H ≥ 17.5 result in a single-peaked dM(C; p) distribution due to asteroids performing a random walk in aP related to a quickly decreasing YORP cycle timescale with size. This transition at approximately 1 km size is indeed seen in the distribution of family members in the (aP, H) plane (bottom left panel of Figure 2).
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Two modeled fragment SFDs compared to the observed Erigone family SFD. The latter is the gold curve, and it comes from Figure 4. The modeled fragment SFDs come from D. D. Durda et al. (2007). For the red curve, defined as “Basalt_5_45_1.8,” a 100 km diameter solid basalt target was hit at 5 km s−1 at a 45∘ impact angle, with the logarithm of the target-to-projectile mass ratio being 1.8 (i.e., a 25 km diameter projectile). For the blue curve “Basalt_6_30_2.2,” a 100 km diameter target was hit at 6 km s−1 at a 30∘ impact angle by an 18 km diameter projectile. The fragment SFDs from both runs were scaled to fit the observed Erigone family SFD. For the red curve the net mass in the fragment SFD, excluding the largest remnant, is 57% of the parent body, which we estimate was 80.5 km in diameter, while for the blue curve the values are 60% and 82.5 km, respectively.
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Solid curves indicate our model crater SFDs for various target strength values Y (as shown by the labels). The black line corresponds to the empirical crater surface saturation, as 10% of the geometric saturation (S. Marchi et al. 2015). Observed crater SFDs for Bennu, Ryugu, and Mathilde are given for sake of comparison (yellow, green, and gray, respectively; data from C. R. Chapman et al. 1999; W. F. Bottke et al. 2020).
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Collisional evolution of the Erigone family SFD. The green curve represents the main-belt SFD as formulated by W. F. Bottke et al. (2020). The blue curve is our estimate of the initial Erigone family SFD. The black curve is the observed Erigone family SFD determined using absolute magnitudes and the family’s median albedo (red curve in Figure 4). The red curve shows the Erigone family SFD after 280 Myr of collisional evolution.
Paper: A Pre-flyby View on the Origin of Asteroid Donaldjohanson, a Target of the NASA Lucy Mission
Authors: Simone Marchi, David Vokrouhlický, David Nesvorný, William F. Bottke, Josef Ďurech, Harold F. Levison
Figure caption: Expected DJ surface coverage from the Lucy flyby. The best resolution is about 10 m pixel−1 (H. A. Weaver et al. 2023; the term “res” indicates a resolution element and corresponds to 3 L’LORRI pixels). Craters as small as 100 m in diameter could be resolved on about one-third of the imaged surface. However, we stress that this image assumes a spherical target, which may not be realistic.
Paper: Informed Design of a Gravity Science Experiment for the Future Geophysical Investigation of the Uranian Moons
Authors: Valerio Filice, Gael Cascioli, Sébastien Le Maistre, Rose-Marie Baland, Antony Trinh, Erwan Mazarico, Sander Goossens
Figure caption: Ariel's expected uncertainty on the MoI and k2 Love number as a function of the maximum estimated degree and order gravity field. The observation settings are the same as those of Figure 14. The effects of Ariel's position and/or Uranus gravity errors on the geodetic parameters of interest are tested. The black dashed line in the k2 panels represents the true value of Ariel's Love number. Ariel's position is here fitted with an a priori uncertainty of 500 m along the three Cartesian coordinates (“Ephemerides case”). The influence of the errors of Uranus gravity is modeled by assuming an a priori of 30% of the current uncertainty estimates on GM, J2, and J4.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Coverage map for THUNDER’s science goals, broken down by instrument/mode: (a) vis–IR spectrometer, (b) SAR coverage, and (c) altimetry. The total amount of coverage by instrument/mode is listed in the top row, enclosed by black boxes. All other rows correspond to each objective, with the minimum coverage needed per instrument per objective listed above polygons showing the map area required to meet science goals. The northern mare are outlined in the top left-hand corner of each map, for orientation on Titan’s surface.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Schematic showing the two end members for the state of Titan's ice shell. (a) Convecting ice shell, with a thick convective layer underlying a thin conducting layer. (b) Purely conductive ice shell, made up of only a thin conductive layer. Note that only the features we aim to test here are present in the graphic; the existence of clathrate layers, finer-scale interior shell structures, and any further solid layers may certainly be present within Titan, but are not depicted.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Plot of measured and theoretical admittance. Solid line shows admittance from measured Titan gravity field with associated uncertainties (D. Durante et al. 2019). Dashed lines show theoretical admittance curves for an uncompensated, thin, and elastic ice shell (green), and pure Airy isostatic end members, indicative of a thicker, viscoelastic shell (purple), with varying ice shell thickness (R. Akiba et al. 2022).
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: Martian gravity data (A. Genova et al. 2016) (a) expanded to spherical harmonic degree 5, per current knowledge of Titan's gravity field (D. Durante et al. 2019), and (b) expanded to spherical harmonic degree 20, matching THUNDER's highest possible gravity field resolution.
Paper: THUNDER: A Titan Orbiter Mission Concept for the New Frontiers Program Designed at the JPL Planetary Science Summer School
Authors: Cassandra Seltzer, Rudi Lien, Brandon T. Radzom, Ella Mullikin, Kimberly Bott, Gwendolyn Brouwer, David G. Burtt, Chloe Gentgen, Jewel Abbate, Victor Gandarillas, Austin P. Green, Tristen Head, Jonathon R. Hill, Jennifer N. Larson, Nicholas J. Montiel, M. Regina A. Moreno, Nicholas L. Wagner, Piyumi Wijesekara, James Tuttle Keane, Alfred E. Nash, Jennifer Scully
Figure caption: THUNDER mission logo.
Paper: Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System
Authors: F. L. Rommel, E. Fernández-Valenzuela, B. C. N. Proudfoot, J. L. Ortiz, B. E. Morgado, B. Sicardy, N. Morales, F. Braga-Ribas, J. Desmars, R. Vieira-Martins, B. J. Holler, Y. Kilic, W. Grundy, J. L. Rizos, J. I. B. Camargo, G. Benedetti-Rossi, A. Gomes-Júnior, M. Assafin, P. Santos-Sanz, M. Kretlow, M. Vara-Lubiano, R. Leiva, D. A. Ragozzine, R. Duffard, H. Kučáková, K. Hornoch, V. Nikitin, T. Santana-Ros, O. Canales-Moreno, D. Lafuente-Aznar, S. Calavia-Belloc, C. Perelló, A. Selva, F. Organero, L. A. Hernandez, I. de la Cueva, M. Yuste-Moreno, E. García-Navarro, J. E. Donate-Lucas, L. Izquierdo-Carrión, R. Iglesias-Marzoa, E. Lacruz, R. Gonçalves, B. Staels, R. Goossens, A. Henden, G. Walker, J. A. Reyes, S. Pastor, S. Kaspi, M. Skrutskie, A. J. Verbiscer, P. Martinez, P. André, J. L. Maestre, F. J. Aceituno, P. Bacci, M. Maestripieri, M. D. Grazia, A. J. Castro-Tirado, I. Pérez-Garcia, E. J. Fernández García, E. Fernández, S. Messner, G. Scarfi, H. Mikuž, J. Prat, P. Martorell, D. Nardiello, V. Nascimbeni, R. Sfair, P. B. Siqueira, V. Lattari, L. Liberato, T. F. L. L. Pinheiro, T. de Santana, C. L. Pereira, M. A. Alava-Amat, F. Ciabattari, H. González-Rodriguez, C. Schnabel
Figure caption: Green lines present the predicted shadow path's northern and southern limits, with the 1σ uncertainties in gray, for the stellar occultations recorded on (a) 2021 March 28, (b) 2023 February 17, and (c) 2023 June 24. The red lines show the predicted center for Huya’s shadow path. The green markers depict the stations with positive detections of the primary component, the blue markers represent observatories that recorded only the satellite, and the observatory denoted by the purple marker in (a) recorded both components of the binary system. The red markers depict stations that recorded negative detections, inconclusive results are shown in black, and bad weather (or technical problems) are in orange. In panel (c), the extensive distribution of observers over a large area reduces the ability to distinguish individual markers in regions with a higher observer density. Maps were generated by the Occultation Portal web page described in Y. Kilic et al. (2022).
Paper: Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System
Authors: F. L. Rommel, E. Fernández-Valenzuela, B. C. N. Proudfoot, J. L. Ortiz, B. E. Morgado, B. Sicardy, N. Morales, F. Braga-Ribas, J. Desmars, R. Vieira-Martins, B. J. Holler, Y. Kilic, W. Grundy, J. L. Rizos, J. I. B. Camargo, G. Benedetti-Rossi, A. Gomes-Júnior, M. Assafin, P. Santos-Sanz, M. Kretlow, M. Vara-Lubiano, R. Leiva, D. A. Ragozzine, R. Duffard, H. Kučáková, K. Hornoch, V. Nikitin, T. Santana-Ros, O. Canales-Moreno, D. Lafuente-Aznar, S. Calavia-Belloc, C. Perelló, A. Selva, F. Organero, L. A. Hernandez, I. de la Cueva, M. Yuste-Moreno, E. García-Navarro, J. E. Donate-Lucas, L. Izquierdo-Carrión, R. Iglesias-Marzoa, E. Lacruz, R. Gonçalves, B. Staels, R. Goossens, A. Henden, G. Walker, J. A. Reyes, S. Pastor, S. Kaspi, M. Skrutskie, A. J. Verbiscer, P. Martinez, P. André, J. L. Maestre, F. J. Aceituno, P. Bacci, M. Maestripieri, M. D. Grazia, A. J. Castro-Tirado, I. Pérez-Garcia, E. J. Fernández García, E. Fernández, S. Messner, G. Scarfi, H. Mikuž, J. Prat, P. Martorell, D. Nardiello, V. Nascimbeni, R. Sfair, P. B. Siqueira, V. Lattari, L. Liberato, T. F. L. L. Pinheiro, T. de Santana, C. L. Pereira, M. A. Alava-Amat, F. Ciabattari, H. González-Rodriguez, C. Schnabel
Figure caption: Objects’ densities as a function of diameter. The square marks the location of Huya using the published primary diameter (P. Santos-Sanz et al. 2022) and the density derived in this work. Quaoar’s density is from C. Kiss et al. (2024). Other densities and primary diameters are from W. M. Grundy et al. (2019) and references therein.
Paper: Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System
Authors: F. L. Rommel, E. Fernández-Valenzuela, B. C. N. Proudfoot, J. L. Ortiz, B. E. Morgado, B. Sicardy, N. Morales, F. Braga-Ribas, J. Desmars, R. Vieira-Martins, B. J. Holler, Y. Kilic, W. Grundy, J. L. Rizos, J. I. B. Camargo, G. Benedetti-Rossi, A. Gomes-Júnior, M. Assafin, P. Santos-Sanz, M. Kretlow, M. Vara-Lubiano, R. Leiva, D. A. Ragozzine, R. Duffard, H. Kučáková, K. Hornoch, V. Nikitin, T. Santana-Ros, O. Canales-Moreno, D. Lafuente-Aznar, S. Calavia-Belloc, C. Perelló, A. Selva, F. Organero, L. A. Hernandez, I. de la Cueva, M. Yuste-Moreno, E. García-Navarro, J. E. Donate-Lucas, L. Izquierdo-Carrión, R. Iglesias-Marzoa, E. Lacruz, R. Gonçalves, B. Staels, R. Goossens, A. Henden, G. Walker, J. A. Reyes, S. Pastor, S. Kaspi, M. Skrutskie, A. J. Verbiscer, P. Martinez, P. André, J. L. Maestre, F. J. Aceituno, P. Bacci, M. Maestripieri, M. D. Grazia, A. J. Castro-Tirado, I. Pérez-Garcia, E. J. Fernández García, E. Fernández, S. Messner, G. Scarfi, H. Mikuž, J. Prat, P. Martorell, D. Nardiello, V. Nascimbeni, R. Sfair, P. B. Siqueira, V. Lattari, L. Liberato, T. F. L. L. Pinheiro, T. de Santana, C. L. Pereira, M. A. Alava-Amat, F. Ciabattari, H. González-Rodriguez, C. Schnabel
Figure caption: Stellar occultation by Huya on 2023 June 24 with the location of the stations that had inconclusive results indicated by gray dotted lines, the positive detections represented by colorful solid lines, and the red segments denoting the 1σ uncertainties. The light-green segments represent the exposure times recorded at the Belesta Observatory, corresponding to the closest negative chord to the north of the observed profile. The dark-green dashes indicate the exposure times captured at the Albox station, which corresponds to the closest negative chord to the south of the observed limb. The white space between the dashes reflects the readout time between exposures at both stations. The black ellipse is the best limb solution using the (a) 2023 Free and (b) 2023 Restrict approaches, respectively. The gray region represents the 1σ uncertainty for each limb determination approach. The direction of the shadow’s movement is indicated by the black arrow.
Paper: Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System
Authors: F. L. Rommel, E. Fernández-Valenzuela, B. C. N. Proudfoot, J. L. Ortiz, B. E. Morgado, B. Sicardy, N. Morales, F. Braga-Ribas, J. Desmars, R. Vieira-Martins, B. J. Holler, Y. Kilic, W. Grundy, J. L. Rizos, J. I. B. Camargo, G. Benedetti-Rossi, A. Gomes-Júnior, M. Assafin, P. Santos-Sanz, M. Kretlow, M. Vara-Lubiano, R. Leiva, D. A. Ragozzine, R. Duffard, H. Kučáková, K. Hornoch, V. Nikitin, T. Santana-Ros, O. Canales-Moreno, D. Lafuente-Aznar, S. Calavia-Belloc, C. Perelló, A. Selva, F. Organero, L. A. Hernandez, I. de la Cueva, M. Yuste-Moreno, E. García-Navarro, J. E. Donate-Lucas, L. Izquierdo-Carrión, R. Iglesias-Marzoa, E. Lacruz, R. Gonçalves, B. Staels, R. Goossens, A. Henden, G. Walker, J. A. Reyes, S. Pastor, S. Kaspi, M. Skrutskie, A. J. Verbiscer, P. Martinez, P. André, J. L. Maestre, F. J. Aceituno, P. Bacci, M. Maestripieri, M. D. Grazia, A. J. Castro-Tirado, I. Pérez-Garcia, E. J. Fernández García, E. Fernández, S. Messner, G. Scarfi, H. Mikuž, J. Prat, P. Martorell, D. Nardiello, V. Nascimbeni, R. Sfair, P. B. Siqueira, V. Lattari, L. Liberato, T. F. L. L. Pinheiro, T. de Santana, C. L. Pereira, M. A. Alava-Amat, F. Ciabattari, H. González-Rodriguez, C. Schnabel
Figure caption: Occultation light curves of the Huya system as recorded on (a) 2021 March 28, (b) 2023 February 17, and (c) 2023 June 24. Black dots and lines represent the observed data. The red dotted lines show the synthetic light-curve model (see text).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System
Authors: F. L. Rommel, E. Fernández-Valenzuela, B. C. N. Proudfoot, J. L. Ortiz, B. E. Morgado, B. Sicardy, N. Morales, F. Braga-Ribas, J. Desmars, R. Vieira-Martins, B. J. Holler, Y. Kilic, W. Grundy, J. L. Rizos, J. I. B. Camargo, G. Benedetti-Rossi, A. Gomes-Júnior, M. Assafin, P. Santos-Sanz, M. Kretlow, M. Vara-Lubiano, R. Leiva, D. A. Ragozzine, R. Duffard, H. Kučáková, K. Hornoch, V. Nikitin, T. Santana-Ros, O. Canales-Moreno, D. Lafuente-Aznar, S. Calavia-Belloc, C. Perelló, A. Selva, F. Organero, L. A. Hernandez, I. de la Cueva, M. Yuste-Moreno, E. García-Navarro, J. E. Donate-Lucas, L. Izquierdo-Carrión, R. Iglesias-Marzoa, E. Lacruz, R. Gonçalves, B. Staels, R. Goossens, A. Henden, G. Walker, J. A. Reyes, S. Pastor, S. Kaspi, M. Skrutskie, A. J. Verbiscer, P. Martinez, P. André, J. L. Maestre, F. J. Aceituno, P. Bacci, M. Maestripieri, M. D. Grazia, A. J. Castro-Tirado, I. Pérez-Garcia, E. J. Fernández García, E. Fernández, S. Messner, G. Scarfi, H. Mikuž, J. Prat, P. Martorell, D. Nardiello, V. Nascimbeni, R. Sfair, P. B. Siqueira, V. Lattari, L. Liberato, T. F. L. L. Pinheiro, T. de Santana, C. L. Pereira, M. A. Alava-Amat, F. Ciabattari, H. González-Rodriguez, C. Schnabel
Figure caption: Stellar occultations by the Huya system observed on (a) 2021 March 28, (b) 2023 February 17, and (c) 2023 June 24, as analyzed in this study. Positive chords are presented by solid lines in colors with error bars in red segments. Close negative exposures are presented by darker-green segments, and other negative data sets are presented in light-green dashed–dotted lines. Inconclusive results are represented by dotted gray lines. The blue star marks the Huya predicted position on 2023 February 17. The black ellipse is the best solution for the primary, and the shadow region represents the 1σ uncertainty. Dotted and dashed circles show the solutions for the satellite detections (see text). The black arrow shows the direction of the shadow movement.
Paper: Stellar Occultation Observations of (38628) Huya and Its Satellite: A Detailed Look into the System
Authors: F. L. Rommel, E. Fernández-Valenzuela, B. C. N. Proudfoot, J. L. Ortiz, B. E. Morgado, B. Sicardy, N. Morales, F. Braga-Ribas, J. Desmars, R. Vieira-Martins, B. J. Holler, Y. Kilic, W. Grundy, J. L. Rizos, J. I. B. Camargo, G. Benedetti-Rossi, A. Gomes-Júnior, M. Assafin, P. Santos-Sanz, M. Kretlow, M. Vara-Lubiano, R. Leiva, D. A. Ragozzine, R. Duffard, H. Kučáková, K. Hornoch, V. Nikitin, T. Santana-Ros, O. Canales-Moreno, D. Lafuente-Aznar, S. Calavia-Belloc, C. Perelló, A. Selva, F. Organero, L. A. Hernandez, I. de la Cueva, M. Yuste-Moreno, E. García-Navarro, J. E. Donate-Lucas, L. Izquierdo-Carrión, R. Iglesias-Marzoa, E. Lacruz, R. Gonçalves, B. Staels, R. Goossens, A. Henden, G. Walker, J. A. Reyes, S. Pastor, S. Kaspi, M. Skrutskie, A. J. Verbiscer, P. Martinez, P. André, J. L. Maestre, F. J. Aceituno, P. Bacci, M. Maestripieri, M. D. Grazia, A. J. Castro-Tirado, I. Pérez-Garcia, E. J. Fernández García, E. Fernández, S. Messner, G. Scarfi, H. Mikuž, J. Prat, P. Martorell, D. Nardiello, V. Nascimbeni, R. Sfair, P. B. Siqueira, V. Lattari, L. Liberato, T. F. L. L. Pinheiro, T. de Santana, C. L. Pereira, M. A. Alava-Amat, F. Ciabattari, H. González-Rodriguez, C. Schnabel
Figure caption: Huya’s limb as observed during the stellar occultation in 2019 March 28 (P. Santos-Sanz et al. 2022). The dashed green line shows the negative data set observed from the QOS Observatory in Ukraine. The solid, colorful lines represent the observed positive LCs, following the same definition as in the original publication. Black segments represent the published uncertainties in the star dis- and reappearance instants. The black ellipse represents the 2019 Restrict limb solution presented in Table 3. The gray area shows the solution’s 3σ uncertainty.