adsabs/AstroCLIMB huggingface dataset:
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: A comparison of the Keplerian orbit solution and the observational data. The black ellipses are approximately to scale and show the shape of Huya and its satellite during the 2023 June 24 occultation. Colored crosses show relative astrometry at the various epochs of observation. Black lines connect the observations to the position predicted by the Keplerian model. Colored ellipses show the orbit during the first observation in that calendar year. The differences in apparent orbit over time show the changing opening angle of the satellite’s orbit (see Section 4).
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: Target star flux ratio (red) with uncertainties (gray) as a function of time for the three data sets that place the best constraints on the presence of rings around Huya (see text). The vertical black line presents the prediction instant for the Huya occultation at each site and the green dashed line shows the 3σ detection level on each light curve.(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: Ring radial width as a function of ring apparent opacity (﹩p^{\prime} ﹩), considering the data dispersion and exposure time of each data set (see text). The data points represent the known rings around small bodies.
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: A corner plot of the MCMC chains from the satellite orbit fit. The two-dimensional contour plots show the joint posterior distributions for each pair of parameters, and the histograms at the top of each column show the marginal posteriors of each parameter. Black points show individual samples from the MCMC chains.
Paper: A Case Study of Interstellar Material Delivery: α Centauri
Authors: Cole R. Gregg, Paul A. Wiegert
Figure caption: The arrival times at the solar system of the α Cen material. The left figure shows all close approaches while the right zooms into the time of peak intensity. The green line shows the effective cross section of the solar system (the solid angle subtended by our Oort cloud as seen from α Cen).
Paper: A Case Study of Interstellar Material Delivery: α Centauri
Authors: Cole R. Gregg, Paul A. Wiegert
Figure caption: The ejection velocity distribution from our simulations, adapted from Figure 6 of C. A. L. Bailer-Jones et al. (2018; their red-dashed line). The right panel is our recreation of the C. A. L. Bailer-Jones et al. (2018) figure, showing the cumulative distribution of ejection velocities caused from a binary star system with masses 1 M⊙ and 0.1 M⊙ on a circular orbit of with 10 au separation.
Paper: Ariel’s Medial Grooves: Spreading Centers on a Candidate Ocean World
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Lauren M. Jozwiak, Tom A. Nordheim, G. Wes Patterson
Figure caption: (a) Orthorectified Voyager 2 ISS image c2684539 (V. I. S. Team 1988, 995 m pixel−1) showing the locations of Ariel's three identified medial grooves, Unnamed, Sprite, and Leprechaun Valles. The chasmata in this area are labeled in white. See Figure 1 for latitude and longitude information for these features. (b) A digital elevation model (DEM) showing the topography of the region covered in panel (a). White arrows show locations of the marginal valleys. See Sections 2.1 and A.1 in C. B. Beddingfield et al. (2022) for discussion on how this DEM was generated. The spatial resolution of the DEM is 995 m pixel−1. White dots are associated with reseau points in panels (a) and (b). Topographic profiles show the following: A–A′: axial troughs with raised rims making up the medial groove called Sprite Vallis. B–B′: the bowed-up chasma floor and bounding marginal valleys of Pixie Chasma. C–C′: subparallel ridges bounding the medial groove called Leprechaun Vallis. D–D′: a full profile across the chasma-medial groove system of Brownie Chasma and Sprite Vallis.
Paper: Ariel’s Medial Grooves: Spreading Centers on a Candidate Ocean World
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Lauren M. Jozwiak, Tom A. Nordheim, G. Wes Patterson
Figure caption: Hypothesized formation models for Ariel's chasma-medial groove systems. (a) In the axial eruption model proposed by B. A. Smith et al. (1986), viscous material welled up along the centers of valley floors and flowed laterally, embaying the bases of adjacent chasmata walls. This figure panel is a digitized version of Figure 11(a) in S. Croft & L. Soderblom (1991). (b) In the lava tube eruption model, proposed by S. Croft & L. Soderblom (1991), confined-lava tube-fed flows took place along the chasma floors (Time 1). As pressures increased in the lava tubes, expansion occurred, and as the pressures subsided, the roofs collapsed, producing medial grooves (Time 2). This figure panel is a digitized version of Figure 11(b) in S. Croft & L. Soderblom (1991). (c) In the spreading center model, Ariel's surface fractures (Time 1), and then warm and buoyant subsurface ice wells up into the gap (Time 2). As the newly resurfaced crust moves away from spreading center, it cools, thickens, and therefore subsides due to a reduction in buoyancy with age, temperature, thickness, and therefore distance from the spreading center.
Paper: Ariel’s Medial Grooves: Spreading Centers on a Candidate Ocean World
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Lauren M. Jozwiak, Tom A. Nordheim, G. Wes Patterson
Figure caption: Possible configurations of Ariel's Cratered Plains before (left) and after (right) spreading occurred, creating Ariel's Pixie Group of chasmata, forming the smooth materials units, and offsetting Kra Chasma (yellow). The Cratered Plains boundaries (red) are based on geologic mapping by S. Croft & L. Soderblom (1991) and visual identification of chasma rims in ISS images. These borders are inferred (dashed red) in regions where the boundaries are difficult to identify with certainty due either to low image resolutions or the terrain being close to the terminator. The base Ariel mosaic is from S. Croft & L. Soderblom (1991). Our reconstruction focuses on removing the young chasma floors, examining the offset of the Kra Chasma segments, and aligning the similarly shaped chasma walls. See Figure 1 for geologic feature labels.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Left: échelle diagram similar to Figure 14(c), but for a model (the moderate central density interface model) including a discontinuous sound speed between the atmosphere and envelope polytropes. m = 0 modes for ℓ = 0–3 are shown, with the ℓ = 1, 3 sequences offset horizontally by 0.05 mHz for clarity. The vertical dashed line shows Δν; the dotted line is Δν + 0.05 mHz. Right: naive FFTs of the frequency differences for each échelle sequence show a variety of peaks that may be difficult to disentangle if seen in the data. Vertical lines show the expected periodicities induced by the acoustic radius/depth of the core/break based on knowledge of this interior model. At face value, the multiple structures at play would make this spectrum difficult to uniquely interpret; here, techniques like the one discussed in Section 4.3 can be used.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Density and sound speed profiles (a), profiles of the acoustic radius (b), and ℓ = 1, m = 0 échelle diagrams (c) for a grid of interface models. The density jump amplitude is fixed at αjump = 2, and colors map to the assumed core boundary location. For legibility, the échelle diagrams are offset from the first by multiples of 0.05 mHz. Vertical dotted lines show the asymptotic equal frequency spacing Δν given by Equation (11), also offset horizontally. The periodicity imprinted on the frequency spacings is diagnostic of the acoustic radius of the interface (solid circles and dotted lines in panel (b), which translates into the “period” (units mHz, nonlinear right axis of panel (b)) of the bumping signature. Dividing by Δν provides the equivalent spacing in terms of radial order, which matches the bumping in the calculated spectrum (vertical bars in panel (c)).
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: An example of exploiting observations of modes of different ℓ to distinguish core structure from near-surface effects. Top: the difference in outer and inner phase shifts as estimated from the ℓ = 0, 1 spectra of the moderate ρc interface model; see Equation (14) and the discussion in the text. Filled and open points show ℓ = 0 and ℓ = 1, respectively, and cubic spline interpolants are shown in the dashed curves. Middle: the difference (α − δ)0 − (α − δ)1 ≃ δ1 − δ0 calculated by differencing the interpolating functions. Bottom: an FFT of δ1 − δ0 used to extract the period that remains in the inner phase shifts. The clear peak matches the inverse acoustic radius of the core calculated from the interior model.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Gravity moments (upper panels) and core properties (lower panels; core density enhancement vs. core radius) for Uranus models in three scenarios constrained by progressively more information. Gray samples in the background are the permissive starting sample loosely constrained to J2 and J4. The “UOP gravity” distribution (left panels, color map) benefits from more precise gravity moments from a Uranus orbiter as estimated by M. Parisi et al. (2024) (see main text for details). The seismology sample (right panels, color map) folds in a hypothetical seismic constraint in the form of a resonance between the ﹩{}_{2}^{2}f﹩ mode and the 6 ring. Colors correspond to log likelihood using the same scale as Figure 7 (top).
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Similar to Figure 12, but here the seismology sample (right panels, color map) posits a resonance between the 6 ring and the higher degree ℓ = m = 9 f-mode. Here, upper panels show the core density enhancement vs. core radius, and lower panels show the wind decay depth vs. deep spin period. In this scenario, the single seismology data point would do little to constrain Uranus’s core structure, but would directly constrain Uranus’s bulk rotation.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Perturbations to the zonal gravity moments J2n induced by the wind according to thermogravitational wind balance, assuming the observed wind speeds are constant on cylinders before applying exponential decay as a function of radial depth from the surface, shown as a function of the e-folding depth H. Square symbols designate the true retrieved depth and associated harmonics ﹩{J}_{2n}^{{\rm{winds}}}﹩ for each model. The vertical axis switches to a linear scale between −10−9 and +10−9 (shaded region).
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Polynomial least-squares fits to the wind-induced components of J2, J4, and J6 as a function of wind depth and bulk spin period. These reflect the results of full TGWE calculations (see Section 2.1.1) for ∼1000 interface models fit to J2 and ρ1 alone. Bottom panels with histograms to the right show that the magnitude of the residuals are typically ≲​​​​​​5 ppm in J2, ≲1 ppm in J4, and ≲0.1 ppm in J6.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Corner diagram for gradient models constrained by gravity and ρ1.
Paper: Setting the Stage for Uranian Seismology from Rings and Radial Velocities
Authors: Christopher R. Mankovich, A. James Friedson, Marzia Parisi, Stephen Markham, Janosz W. Dewberry, James Fuller, Matthew M. Hedman, Alex Akins, Mark D. Hofstadter
Figure caption: Corner diagram for interface models constrained by gravity and ρ1.
Paper: The New Titan Planetary Climate Model. II. Titan’s Haze and Cloud Cycles
Authors: Bruno de Batz de Trenquelléon, Pascal Rannou, Jérémie Burgalat, Sébastien Lebonnois, Jan Vatant d'Ollone
Figure caption: Haze distribution for (a) the vernal equinox (LS = 0∘), (b) the northern spring (LS = 60∘), (c) the northern summer (LS = 120∘), (d) the fall equinox (LS = 180∘), (e) the northern fall (LS = 240∘), and (f) the northern winter (LS = 300∘). The field presented is the extinction coefficient of aerosols at 0.671 μm, in zonal and diurnal average. The meridional stream function is shown as black contours (the solid line is clockwise rotation and the dashed line is counterclockwise).
Paper: The New Titan Planetary Climate Model. II. Titan’s Haze and Cloud Cycles
Authors: Bruno de Batz de Trenquelléon, Pascal Rannou, Jérémie Burgalat, Sébastien Lebonnois, Jan Vatant d'Ollone
Figure caption: Map of haze extinction as a function of time and altitude at the equator as predicted in the Titan PCM. The field shows the extinction coefficient of aerosols at 0.671 μm. The white stars represent the position of the DHL, identified as the local maximum of the vertical extinction profile. The white and black vertical dotted lines represent, respectively, the period of the equinox and the reappearance of the DHL. This figure can be directly compared to Figure 15 of B. Seignovert et al. (2021).
Paper: The New Titan Planetary Climate Model. II. Titan’s Haze and Cloud Cycles
Authors: Bruno de Batz de Trenquelléon, Pascal Rannou, Jérémie Burgalat, Sébastien Lebonnois, Jan Vatant d'Ollone
Figure caption: Top: size distribution of aerosols used in the Titan PCM, derived from the 2D model of P. Rannou et al. (2004) and J. Burgalat & P. Rannou (2017) utilizing a bin representation. This distribution, characterized by a combination of power laws, is parameterized using only two variables: the normalization factor C0 and the mean aerosol radius rc. Bottom: intermoment function associated to the size distribution used in the Titan PCM. The function is presented for the interval k ∈ [−2; 6] containing all the orders necessary for the development of the microphysical laws.
Paper: Surface Energy of Insoluble Organic Matter Simulant: Evaluation Based on Adhesive Force Measured by Centrifugal and Impact Separation Methods
Authors: Yuuya Nagaashi, Yoshihiro Furukawa, Akiko M. Nakamura
Figure caption: Electron microscope images of syn-IOM fractions. The upper left and right images for grain size acquisition show fractions of synthesized at 80°C and 200°C, respectively. The high-resolution images at the lower left and lower right are a fraction of synthesized at 200°C and a fraction after the former has experienced heating at 120°C to reduce adsorbed water.
Paper: Surface Energy of Insoluble Organic Matter Simulant: Evaluation Based on Adhesive Force Measured by Centrifugal and Impact Separation Methods
Authors: Yuuya Nagaashi, Yoshihiro Furukawa, Akiko M. Nakamura
Figure caption: Constituent grain size distribution of syn-IOM fractions seen in electron microscope images.
Paper: Surface Energy of Insoluble Organic Matter Simulant: Evaluation Based on Adhesive Force Measured by Centrifugal and Impact Separation Methods
Authors: Yuuya Nagaashi, Yoshihiro Furukawa, Akiko M. Nakamura
Figure caption: Measured adhesive forces of the syn-IOM aggregates. The dashed curves are the fitted curves according to Equation (2).
Paper: Surface Energy of Insoluble Organic Matter Simulant: Evaluation Based on Adhesive Force Measured by Centrifugal and Impact Separation Methods
Authors: Yuuya Nagaashi, Yoshihiro Furukawa, Akiko M. Nakamura
Figure caption: TG-DTA results. Left: the TG-DTA result of the syn-IOM fraction synthesized at 200°C. Right: the TG-DTA result of the same fraction after cooling and exposure to air to reabsorb water, following the initial TG-DTA on the left.
Paper: Surface Energy of Insoluble Organic Matter Simulant: Evaluation Based on Adhesive Force Measured by Centrifugal and Impact Separation Methods
Authors: Yuuya Nagaashi, Yoshihiro Furukawa, Akiko M. Nakamura
Figure caption: Examples of waveforms of applied impact accelerations and microscope images after applying each acceleration.
Paper: Surface Energy of Insoluble Organic Matter Simulant: Evaluation Based on Adhesive Force Measured by Centrifugal and Impact Separation Methods
Authors: Yuuya Nagaashi, Yoshihiro Furukawa, Akiko M. Nakamura
Figure caption: Configuration of adhesive force measurements using the impact separation method. (A), (B) Overall view of the apparatus before and after impact. (C) Schematic diagram of the adhesive force measurement.
Paper: Ground-based Characterization of (98943) Torifune 2001 CC21, the Target of the Hayabusa2# Space Mission 
Authors: Marcel M. Popescu, Eri Tatsumi, Javier Licandro, Miguel R. Alarcon, Javier Rodríguez Rodríguez, Miquel Serra-Ricart, Julia de León, Joaquín Fernandez Martin, David Morate, Gabriel N. Simion, Bogdan Alexandru Dumitru, Daniel Nicolae Berteşteanu, George Pantelimon Prodan, Masatoshi Hirabayashi
Figure caption: The reduced magnitude Vred as a function of phase angle α. Each of the blue points represents the average of the observations made with an instrument during a night. The log of these observations is shown in Tabel 7. The fitted red curve corresponds to the {H, G} model where H = 18.846 and G = 0.294, while the red dashed curve represents the {H, G1, G2} model where H = 18.706, G1 = 0.259, and G2 = 0.372.