adsabs/AstroCLIMB huggingface dataset:
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: Period search tool output plot for (98943) Torifune. This search was performed in an interval from 5.010 to 5.035 hr, with a coefficient p (period step) of 0.2. Each obtained period is represented as a black circle, with the red line representing a 10% threshold from the lowest χ2 obtained. The presence of five values under this threshold is an indicator that more data will refine the period value.
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: Pole solution statistical quality for (98943) Torifune. The values of λ and β are shaded by its ﹩{\chi }_{{\rm{red}}}^{2}﹩ value, while the best solution (λ = 280∘, β = 85∘ with ﹩{\chi }_{{\rm{red}}}^{2}=1.04﹩) is plotted as a white square. The red border represents the solutions that are within a 3σ level of uncertainty from the best solution of 4.88%.
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 comparison between the spectrum of Torifune and the spectrum of a sample from the Chateau Renard (L6) meteorite, chip pulse laser irradiated (sample ID: OC-TXH-011-A80, file C1OC 11A80; left) and Appley Bridge (LL6) meteorite, chip pulse laser irradiated (sample ID: OC-TXH-012-A40, file C1OC 12A40; right). All spectra are normalized at 1.25 μm.
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 comparison between the spectrum of Torifune and the Sq type (left) and the S, Q, and L types (middle) as they were defined by Bus–DeMeo taxonomy (F. E. DeMeo et al. 2009). Right: comparison between the visible spectrum of Torifune obtained with GTC and the spectrophotometric data obtained with TCS. All spectra are normalized at 0.55 μm.
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: Graphical representation of the fit between four light curves and the best obtained model for Torifune. The observed data are plotted as red circles, while the shape model is plotted as a solid blue line for each observation. The geometry is described by its solar phase angle α (defined as the angle between the Sun, the asteroid, and the observer) and its aspect angle θ (defined as the angle between the rotation axis and the asteroid—observer direction). The reference Julian Day is 2459909.000000.
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 simultaneous light curves obtained with g, r, i, and zs filters. The observations were performed with TCS/MuSCAT2. The data corresponding to (g − r) for the night of 2022 December 23 have a low SNR owing to the magnitude limit of the instrument.
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 extrapolated light curves observed around the stellar occultation event (marked by the black line) observed by K. Arimatsu et al. (2024). The red circles correspond to the observations obtained on March 4, the blue plus signs are data obtained on March 5, and the green diamonds are the photometric values obtained on 2023 March 6.
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 (g − r), (r − i), (i − zs) color–color diagram of the 155 objects with known spectral classification, used as training data. The values corresponding to Torifune are shown in magenta. The title shows the classification according to the KNN and RF algorithms. The results corresponding to two observing nights are shown to allow the comparison of Torifune's position.
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: BAR vs. Band I center for a sample of 48 ordinary chondrites computed by T. L. Dunn et al. (2010). The dashed-line region encloses the obtained values. Horizontal lines separate the regions mostly occupied by H, L, and LL ordinary chordates, as labeled in the plot. The red circle corresponds to the computed BAR and Band I center values of Torifune.
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: Obtained shape model of (98943) Torifune. Top left: north pole view (Y-axis = 0∘). Bottom left: south pole view (Y-axis = 180∘). Top right: equatorial view with Z-axis rotated 0∘. Bottom right: equatorial view with Z-axis rotated 90∘.
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 folded light curve for a period of P = 5.021516 ± 0.000106 hr. We selected the data with phase angles between 4∘ and 23∘. The reference Julian day is 2460286.642715431.
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: (a) The third-order moment profiles for haze (black) and mist of condensed species (red). (b) Radius profiles of aerosols (black) and cloud droplets (red). (c) Opacity profiles at 0.671 μm for haze (black) and total (red). The Huygens/DISR vertical profile from L. R. Doose et al. (2016) is plotted for comparison (dashed black line). (d) Temperature profile predicted by the Titan PCM (solid line) compared to the Huygens/HASI vertical profile from M. Fulchignoni et al. (2005; dashed line). All profiles correspond to the time and latitude of Huygens’ landing (LS = 305°; 10°S). The two horizontal lines represent the altitude of the modeled DHL (4 Pa) and the main haze layer (1.5 × 103 Pa). The altitude scale on the right axis is approximate.
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: Seasonal evolution of methane cloud opacity at 0.671 μm predicted by the Titan PCM, in zonal mean. The field corresponds to the average over the last five simulated years. Opacity peaks correspond to the presence of large methane clouds in the atmospheric column. The black contours indicate the maximum methane surface precipitation (>0.1 mm T﹩{}_{\mathrm{day}}^{-1}﹩).
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: modeled vertical profile of the methane-mixing ratio, in zonal and diurnal average, at LS = 305° and 10°S. The vertical profiles from Huygens’ observations are shown in color for comparison (H. B. Niemann et al. 2010; T. Gautier et al. 2024). Bottom: methane cloud extinction at 0.671 μm as a function of latitude and altitude, averaged zonally, for LS = 27.56°. The meridional stream function is displayed as black contours, indicating the ascending currents of circulation.
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: modeled latitudinal mixing ratios of methane in the troposphere (solid line) and the stratosphere (dashed line). Bottom: meridional mass fluxes of methane in the Titan PCM, below 10 km (black), between 10 and 40 km (red), and above 40 km (blue). Positive flux values indicate a northward flux, while negative values indicate a southward flux. The left panels represent the average during the northern summer and the right panels during the southern summer. The figures show no latitudinal variation in methane quantity in the stratosphere and a higher quantity of methane in the troposphere during the summer.
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: Ethane mole fraction predicted by the Titan PCM at the north pole (black line) and south pole (red line) for (a) southern winter and (b) northern winter. Mole fractions computed using CIRS data have been plotted with their error bar at the same periods for comparison (C. Mathé et al. 2020; S. Vinatier et al. 2020). The altitude scale on the right axis is approximate.
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: Left: seasonal evolution of modeled methane evaporation at the surface, in zonal and diurnal average. Right: map of modeled amount of methane, in zonal and annual average, in the atmosphere below 25 km, as a function of latitude. The meridional stream function is shown as black contours.
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: Annual and zonal average of the atmospheric extinction coefficient at 0.671 μm. The extinction above 80 km corresponds to the extinction of the main haze layer composed of dry aerosols (see Figure 2). The extinction between 20 and 60 km is associated with the mist of condensate. Peaks of extinction below 25 km correspond to methane clouds, as described in Section 4.1.
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: Tropospheric temperature profiles in the Titan PCM, averaged zonally and diurnally, around the season of the Huygens’ landing. Three latitudes are show: the equator in black, the north pole (85°N) in red, and the south pole (85°S) in blue. The vertical profile from HASI (M. Fulchignoni et al. 2005) is plotted for comparison in black dotted lines. The altitude scale on the right axis is approximate.
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: Temporal evolution of the mass fraction of trace compound condensates (C2H2, C2H6, and HCN) modeled by the Titan PCM between 60 and 350 km.
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: (a) Annual variation in surface opacity (λ = 0.671 μm) predicted by the Titan PCM. (b) Corresponding variation in surface temperature. The black crosses represent the maximum insolation received by the surface.
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: Latitudinal surface temperature predicted by the Titan PCM in black (a) in the middle of the northern winter, (b) at the early northern spring, (c) and at the northern summer solstice. For comparison, the CIRS profiles from D. E. Jennings et al. (2019) are plotted in red.
Paper: FindPOTATOs: Minor Planet Observation Linking Software
Authors: C. R. Nugent, Nicole J. Tan, James M. Bauer
Figure caption: NEAT surveyed the sky using a cadence of three images, or frame triplets. The average number of sources in each frame was 728 but varied widely from frame to frame, due to the unique characteristics of the TriCam cameras. The frame with the least sources contained 78 sources, the frame with the most contained 13,319. Therefore, there was significant runtime variation between frame triplets. The runtime per frame triplet generally increased with the number of tracklets found. Frame triplets with zero tracklets found can take tens of seconds to process.
Paper: FindPOTATOs: Minor Planet Observation Linking Software
Authors: C. R. Nugent, Nicole J. Tan, James M. Bauer
Figure caption: Sample diagnostic test images. Top: a real tracklet, from an example data set provided to users based on Catalina Sky Survey data from the MPC. For the three detections in this tracklet, the diagnostic image shows their magnitudes (left), their positions on the sky (middle), and an SDSS image of the same region of sky (right). This last frame allows users to visually verify that the tracklet does not overlap with stationary sources, such as stars. Bottom: a spurious tracklet, where the SDSS image indicates that one of the detections is not a moving object, but a star. This tracklet should not be submitted to the MPC and indicates that the data should undergo further cleaning.
Paper: FindPOTATOs: Minor Planet Observation Linking Software
Authors: C. R. Nugent, Nicole J. Tan, James M. Bauer
Figure caption: The previous two detections in a tracklet (solid black circles) and assumed linear motion are used to predict the position of the next detection in the tracklet (black dotted circle). The code searches around the predicted position, using one of two calculated radii. A minimum search radius (gray dotted circle), min_search_radius, is a parameter set by the user, and is always searched. A secondary radius is also derived from the min_tracklet_angle. This parameter allows tracklets to curve. A curving tracklet may fall outside the min_search_radius and require a larger search radius (blue dotted circle) is then used to find subsequent detections.
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: One-third of the measured median adhesive forces of syn-IOM aggregates plotted against the median radius of constituent grains. The black dashed line represents the fitted line.
Paper: FindPOTATOs: Minor Planet Observation Linking Software
Authors: C. R. Nugent, Nicole J. Tan, James M. Bauer
Figure caption: Schematic of FindPOTATOs.
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: Graphical representation of the fit between the rest of the light curves and the best obtained model for (98943) Torifune. The observed data are plotted as red circles, while the shape model is plotted as a solid blue line for each of the observations. The geometry is described by its solar phase angle α and its aspect angle θ. The reference Julian Day is 2459909.000000.
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: Comparison between the spectrum of (98943) Torifune reported in this work and the one presented by J. Geem et al. (2023). Both spectra were normalized at 1.25 μm.
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 comparison between the spectra of (99843) Torifune and (25143) Itokawa (R. P. Binzel et al. 2001). All spectra are normalized at 0.55 μm.
Paper: Prospectivity Modeling of the NASA VIPER Landing Site at Mons Mouton near the Lunar South Pole
Authors: Joshua Coyan, Matt Siegler, Jose Martinez-Comacho, Ross Beyer, Mark Shirley
Figure caption: (a) Ice stability regions (ISRs): this map uses a gradient of blues to indicate ice stability, with the darkest blue marking areas where ice is stable and exists at the surface. Moderate blue indicates ice stability from surface down to 20 cm, and lightest blue signifies ice stability greater than 85 cm. Unshaded regions denote areas that are dry (no ice stability in the top 1 m). (b) Maximum temperature map: illustrated with a spectrum of warm to cool colors, this map shows areas of high temperatures in yellows and oranges, while cooler temperatures are represented by blues and purples. (c) PSR map calculated from the DEM and passage of the Sun over 76 yr to determine the permanently shadowed areas shown as red-filled in areas. (d) Slope: derived from the SfS DEM, this map displays shallow slopes in greens and yellows, while areas in orange and red indicate slopes that exceed the 15° threshold, marking them too steep for the rover.
Paper: Prospectivity Modeling of the NASA VIPER Landing Site at Mons Mouton near the Lunar South Pole
Authors: Joshua Coyan, Matt Siegler, Jose Martinez-Comacho, Ross Beyer, Mark Shirley
Figure caption: (a) Curvature map: this is a zoomed-in view of the study area and highlights topographical curvature, with convex elevations illuminated in lighter shades of gray and concave depressions marked in darker shades. As in Figure 2(c), the red polygons represent PSRs. (b) Aspect map: this map indicates the orientation of slopes, with warm hues like yellows and oranges denoting northeastern-facing slopes and cooler tones such as blues and purples signifying southwestern-facing slopes, the latter of which are more likely to preserve ice in this location. (c) Distance to PSR map: this map quantifies the Euclidean distance to the nearest PSRs, using a color gradient where greens indicate proximity to PSRs and warmer colors represent greater distances. (d) PSR density map: created through sliding-window analysis, this map employs a 1000 m circular window to traverse the PSR data set, revealing local variations in PSR density across the landscape.
Paper: Prospectivity Modeling of the NASA VIPER Landing Site at Mons Mouton near the Lunar South Pole
Authors: Joshua Coyan, Matt Siegler, Jose Martinez-Comacho, Ross Beyer, Mark Shirley
Figure caption: This final prospectivity map synthesizes eight evidence layers: ISRs, maximum temperature, PSRs, slope, curvature, aspect, distance to PSRs, and density of PSRs. The color gradient signifies prospectivity levels, with cool tones indicating higher potential and warm tones suggesting lower potential. Specifically, dark blue areas are deemed highly prospective, light blue suggests favorable conditions, yellow denotes permissive regions, and red areas are considered nonprospective.
Paper: Prospectivity Modeling of the NASA VIPER Landing Site at Mons Mouton near the Lunar South Pole
Authors: Joshua Coyan, Matt Siegler, Jose Martinez-Comacho, Ross Beyer, Mark Shirley
Figure caption: The figure illustrates the diverse potential types of deposits of lunar water ice, ranging from fluid inclusions within minerals to layers within discrete strata, scattered accumulations, and surficial deposits within the confines of PSRs. The water ice may exist as chunky fragments, occupy the spaces between soil particles, or form a delicate frost along the edges of granules (modified from D. Hurley et al. 2021 and G. Heiken et al. 1991).