adsabs/AstroCLIMB huggingface dataset:
Paper: Model of Double Asteroid Redirection Test Impact Ejecta Plume Observations
Authors: Andrew F. Cheng, S. D. Raducan, Eugene G. Fahnestock, Elisabetta Dotto, Vincenzo Della Corte, Angela M. Stickle
Figure caption: DART impact on Dimorphos is at the origin of Cartesian coordinates  x – y – z . LICIACube trajectory is dashed blue line in the  x – y  plane. LICIACube position is (x  s , y  s , 0) in distant approach. Didymos is crosshatched oval to left, and the Dimorphos orbit is dashed black arrow. The line of sight to the Dimorphos impact site is the red line defining the  y    b   axis. The plane of sky at Dimorphos seen from LICIACube is the  x    b  – z  plane (shaded), which is rotated around  z  from  x – z . Optical depth profiles calculated by Cheng et al. (2020) for image lines at constant z = 0. Optical depth profiles for image lines at constant z = z 0 in the plane of sky given here. The DART impact ejecta cone is shown in yellow; it is a hollow cone with negligibly thin walls. The cone axis is  y , with ejecta angle α. The ejecta cone crossing and the closest approach c/a of LICIACube trajectory are indicated by blue dots.
Paper: Model of Double Asteroid Redirection Test Impact Ejecta Plume Observations
Authors: Andrew F. Cheng, S. D. Raducan, Eugene G. Fahnestock, Elisabetta Dotto, Vincenzo Della Corte, Angela M. Stickle
Figure caption: Ejecta plume extinction optical depths at two times, 1 and 10 s after DART impact, in target case basalt C2, showing rapid evolution and clearing of plume opacity for ﹩\left|b\right|\lesssim 80\,{\rm{m}}﹩.
Paper: Model of Double Asteroid Redirection Test Impact Ejecta Plume Observations
Authors: Andrew F. Cheng, S. D. Raducan, Eugene G. Fahnestock, Elisabetta Dotto, Vincenzo Della Corte, Angela M. Stickle
Figure caption: Cumulative mass M ejected above velocity v, for three target cases from Housen & Holsapple (2011). Target cases Basalt C2 and SFA C7 are strength-controlled at high and moderate strength, respectively. Case C5 is gravity-controlled.
Paper: Model of Double Asteroid Redirection Test Impact Ejecta Plume Observations
Authors: Andrew F. Cheng, S. D. Raducan, Eugene G. Fahnestock, Elisabetta Dotto, Vincenzo Della Corte, Angela M. Stickle
Figure caption:  x–y plane showing ejecta cone and ejection angle α. The dashed arrow is the line of sight (LOS) from LICIACube at (x  s , y  s ). LICIACUbe is inside the ejecta cone with LOS angle ξ > 0 and b distance > 0, where b is the distance in the plane of sky along the  x    b   direction of Figure 1.
Paper: Double Asteroid Redirection Test (DART): Structural and Dynamic Interactions between Asteroidal Elements of Binary Asteroid (65803) Didymos
Authors: Masatoshi Hirabayashi, Fabio Ferrari, Martin Jutzi, Ryota Nakano, Sabina D. Raducan, Paul Sánchez, Stefania Soldini, Yun Zhang, Olivier S. Barnouin, Derek C. Richardson, Patrick Michel, Elisabetta Dotto, Alessandro Rossi, Andrew R. Rivkin
Figure caption: Reshaping-driven orbital perturbation. The green lines give the original orbit, i.e., the preimpact orbit; the blue lines show perturbed orbits driven by the DART impact without reshaping; and the red lines describe those induced by the DART impact and the reshaping process. (a) Preimpact orbit. (b) DART impact causing orbital perturbation without reshaping. (c) Nonnegligible reshaping happening to Dimorphos and Didymos. The shapes enclosed by black solid lines are the original shapes, while those enclosed by red solid lines are the deformed shapes. (d) Reshaping-driven orbital perturbation.
Paper: Double Asteroid Redirection Test (DART): Structural and Dynamic Interactions between Asteroidal Elements of Binary Asteroid (65803) Didymos
Authors: Masatoshi Hirabayashi, Fabio Ferrari, Martin Jutzi, Ryota Nakano, Sabina D. Raducan, Paul Sánchez, Stefania Soldini, Yun Zhang, Olivier S. Barnouin, Derek C. Richardson, Patrick Michel, Elisabetta Dotto, Alessandro Rossi, Andrew R. Rivkin
Figure caption: Low-speed particle collisions on Didymos under different surface conditions. (a) Large rocks are dominant on the surface, and low-speed collisions do not affect the conditions. (b) A surface layer with small, highly cohesive particles (≥5 Pa) is unaffected by low-speed collisions. (c) Low-speed collisions on a small, low-cohesive surface (<5 Pa) may induce surface disturbance.
Paper: Double Asteroid Redirection Test (DART): Structural and Dynamic Interactions between Asteroidal Elements of Binary Asteroid (65803) Didymos
Authors: Masatoshi Hirabayashi, Fabio Ferrari, Martin Jutzi, Ryota Nakano, Sabina D. Raducan, Paul Sánchez, Stefania Soldini, Yun Zhang, Olivier S. Barnouin, Derek C. Richardson, Patrick Michel, Elisabetta Dotto, Alessandro Rossi, Andrew R. Rivkin
Figure caption: Variations in ejecta cone geometry driven by a sloping surface and the spacecraft shape. (a) Nominal case generating axisymmetric cone geometry. (b) Ejecta cone facing outward. (c) Ejecta cone facing inward and eventually crossing Didymos.
Paper: Double Asteroid Redirection Test (DART): Structural and Dynamic Interactions between Asteroidal Elements of Binary Asteroid (65803) Didymos
Authors: Masatoshi Hirabayashi, Fabio Ferrari, Martin Jutzi, Ryota Nakano, Sabina D. Raducan, Paul Sánchez, Stefania Soldini, Yun Zhang, Olivier S. Barnouin, Derek C. Richardson, Patrick Michel, Elisabetta Dotto, Alessandro Rossi, Andrew R. Rivkin
Figure caption: Potential reshaping modes of Didymos, depending on different internal structures. The horizontal axis shows the spin rate, increasing to the right. (a) Homogeneous weak structure. (b) Homogeneous strong structure. (c) Heterogeneous structure. The top layer in light gray consists of weaker structures, while the interior in dark gray is made of stronger structures. The critical spin period in which the reshaping occurs is conceptual in this schematic and depends on the existing strength.
Paper: Spectral Rotational Characterization of the Didymos System prior to the DART Impact 
Authors: Simone Ieva, E. Mazzotta Epifani, D. Perna, M. Dall'Ora, V. Petropoulou, J. D. P. Deshapriya, P. H. Hasselmann, A. Rossi, G. Poggiali, J. R. Brucato, M. Pajola, A. Lucchetti, S. L. Ivanovski, P. Palumbo, V. Della Corte, A. Zinzi, A. S. Rivkin, C. A. Thomas, J. de León, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, B. Cotugno, G. Cremonese, V. Di Tana, I. Gai, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: Comparison between a representative set of spectra collected during our observations in 2021 (#1, #5, and #8) together with previously observed spectra of the Didymos system retrieved from the literature. (Left) Spectrum #1 together with the one observed by J. de León in 2019 in red (JDL19). (Middle) #5 together with one from Binzel et al. (2004) in green. (Right) spectrum #8 with one retrieved by de León et al. (2010) in cyan.
Paper: Spectral Rotational Characterization of the Didymos System prior to the DART Impact 
Authors: Simone Ieva, E. Mazzotta Epifani, D. Perna, M. Dall'Ora, V. Petropoulou, J. D. P. Deshapriya, P. H. Hasselmann, A. Rossi, G. Poggiali, J. R. Brucato, M. Pajola, A. Lucchetti, S. L. Ivanovski, P. Palumbo, V. Della Corte, A. Zinzi, A. S. Rivkin, C. A. Thomas, J. de León, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, B. Cotugno, G. Cremonese, V. Di Tana, I. Gai, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: Spectral slopes for spectra observed during the night of 2021 February 15 (in yellow) and February 23 (in orange) alongside their Julian date (JD). We show JD computed for the first night below the same quantity for the second night. We also remark in red the beginning and end of the only mutual event observed during the nights, the primary eclipse. In light red we report the current uncertainty on the occurrence of the event (±8 minutes).
Paper: Spectral Rotational Characterization of the Didymos System prior to the DART Impact 
Authors: Simone Ieva, E. Mazzotta Epifani, D. Perna, M. Dall'Ora, V. Petropoulou, J. D. P. Deshapriya, P. H. Hasselmann, A. Rossi, G. Poggiali, J. R. Brucato, M. Pajola, A. Lucchetti, S. L. Ivanovski, P. Palumbo, V. Della Corte, A. Zinzi, A. S. Rivkin, C. A. Thomas, J. de León, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, B. Cotugno, G. Cremonese, V. Di Tana, I. Gai, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: Comparison between three representative Didymos spectra observed at TNG during the 2021 observational window (#1, #5 and #8) with their best meteorite analog, selected among the 50 best fits retrieved using the M4AST tool. The tool was used to compare our data with the whole RELAB database, selecting the ones with a lower χ 2 value that better mimic the overall spectral behavior.
Paper: Spectral Rotational Characterization of the Didymos System prior to the DART Impact 
Authors: Simone Ieva, E. Mazzotta Epifani, D. Perna, M. Dall'Ora, V. Petropoulou, J. D. P. Deshapriya, P. H. Hasselmann, A. Rossi, G. Poggiali, J. R. Brucato, M. Pajola, A. Lucchetti, S. L. Ivanovski, P. Palumbo, V. Della Corte, A. Zinzi, A. S. Rivkin, C. A. Thomas, J. de León, E. Dotto, M. Amoroso, I. Bertini, A. Capannolo, B. Cotugno, G. Cremonese, V. Di Tana, I. Gai, G. Impresario, M. Lavagna, A. Meneghin, F. Miglioretti, D. Modenini, S. Pirrotta, E. Simioni, S. Simonetti, P. Tortora, M. Zannoni, G. Zanotti
Figure caption: Spectral slopes computed for the 2021 data set considered in this work vs. the fractional rotational phase, assigned based on the primary lightcurve. For simplicity, 0 is assigned to the first spectrum available (#1). Spectra acquired during the nights of February 15 and February 23 are represented in yellow and orange, respectively.
Paper: Arecibo S-band Radar Characterization of Local-scale Heterogeneities within Mercury’s North Polar Deposits
Authors: Edgard G. Rivera-Valentín, Heather M. Meyer, Patrick A. Taylor, Erwan Mazarico, Sriram S. Bhiravarasu, Anne K. Virkki, Michael C. Nolan, Nancy L. Chabot, Jon D. Giorgini
Figure caption:  S-band delay-Doppler image of Mercury from 2019 July 19 as total OC and SC backscatter with pixel values in units of standard deviations above the noise baseline (i.e., linear z-scores). The color map is clipped such that z-scores < 0 map to black and z-scores > 100 map to white. On the left, we plot the OC (black) and SC (gray) radar cross-section density in units of dB (i.e., logarithmic) as a function of delay in units of μs.
Paper: Arecibo S-band Radar Characterization of Local-scale Heterogeneities within Mercury’s North Polar Deposits
Authors: Edgard G. Rivera-Valentín, Heather M. Meyer, Patrick A. Taylor, Erwan Mazarico, Sriram S. Bhiravarasu, Anne K. Virkki, Michael C. Nolan, Nancy L. Chabot, Jon D. Giorgini
Figure caption: SC radar backscatter coefficient map of the northern terrains in polar stereographic projection generated over the six-day observing campaign. Radar backscatter is in units of z-score. The map is limited to latitudes >75°N. The “big five” craters in the area, Prokofiev, Kandinsky, Tolkien, Chesterton, and Tryggvadóttir, are labeled in yellow.
Paper: Thermophysical Investigation of Asteroid Surfaces. II. Factors Influencing Grain Size
Authors: Eric M. MacLennan, Joshua P. Emery
Figure caption: Meteorite thermal conductivity as a function of porosity (top; Table 2) and specific heat capacity as a function of temperature (bottom; Table 3). Dashed lines from this work show linear fits in the top panel and parabola fits through the origin in the bottom panel, with gray regions representing 95% confidence to the fits. The dashed–dotted line through the Campo del Cielo datum in the top panel assumes a slope of 0.3. Note the break in the y-axis in the top panel.
Paper: Thermophysical Investigation of Asteroid Surfaces. II. Factors Influencing Grain Size
Authors: Eric M. MacLennan, Joshua P. Emery
Figure caption: Top: histogram distributions of thermal skin depths, grouped by rotation period. Thermal inertia (middle) and regolith grain size (bottom) are shown as a function of thermal skin depth, with colors indicating rotation period bin defined in the top panel. Dashed lines in the middle and bottom panels show proportionality relationships between the skin depth and thermal inertia or grain size, as shown in each panel. The dashed–dotted–dotted lines indicate where the grain size is equal to the skin depth and three times the skin depth.
Paper: Thermophysical Investigation of Asteroid Surfaces. II. Factors Influencing Grain Size
Authors: Eric M. MacLennan, Joshua P. Emery
Figure caption: Spacecraft images of the regolith on Eros, Itokawa, Bennu, and Ryugu acquired by the NEAR, Hayabusa, OSIRIS-REx, and Hayabusa 2 missions, respectively.
Paper: Thermophysical Investigation of Asteroid Surfaces. II. Factors Influencing Grain Size
Authors: Eric M. MacLennan, Joshua P. Emery
Figure caption: Multilinear model fit M-4, shown by colored points, and the grain size data set, shown by black dots, as a function of asteroid diameter (left) and rotation period (right). The colored bars at the top of each panel indicate the 1σ range in uncertainty in the break point between the two segments.
Paper: Thermophysical Investigation of Asteroid Surfaces. II. Factors Influencing Grain Size
Authors: Eric M. MacLennan, Joshua P. Emery
Figure caption: Geometric albedo (p  V ) vs. slope parameter (G  V ) grouped by spectral type for all asteroids in this study. The top panel (filled symbols) shows the objects classified on the basis of spectral or color data and family membership, when applicable. The bottom panel (open symbols) shows the objects classified only on the basis of albedo.
Paper: Thermophysical Investigation of Asteroid Surfaces. II. Factors Influencing Grain Size
Authors: Eric M. MacLennan, Joshua P. Emery
Figure caption: Grain size model residual distributions for different compositional groups and the group means and standard deviations (bottom right panel). Unfilled histograms and open circles in the bottom right panel indicate that objects with assumed spectral classification are included. The filled gray histogram and the black line in the top right panel are for M-types and metal-rich asteroids, respectively. The dotted horizontal line at 0ϕ in each panel is shown for comparison purposes. Note the change in the y-axis range in the middle three panels.
Paper: Thermophysical Investigation of Asteroid Surfaces. II. Factors Influencing Grain Size
Authors: Eric M. MacLennan, Joshua P. Emery
Figure caption: Regolith grain sizes of NEAs as a function of (a) aphelion distance, (b) perihelion distance, (c) asteroid diameter, and (d) rotation period. Symbol colors indicate spectral type as noted in the top left panel and are consistent with previous figures. The open symbols are objects with an inferred spectral type (see text), and gray dots are MBAs.
Paper: N-body Interactions will be Detectable in the HR-8799 System within 5 yr with VLTI-GRAVITY
Authors: Sofia Covarrubias, Sarah Blunt, and Jason J. Wang
Figure caption: The absolute difference between using an approximate Keplerian multi-body solver (Lacour et al. 2021) vs. an N-body solver for each body in the HR-8799 system. Data shows that smaller-separation planets will deviate by up to a quarter of a milliarcsecond from the previous Kepler calculations within five years; enough to be detected by high-precision instruments such as VLTI-GRAVITY.
Paper: The White Dwarf Mass versus X-Ray Temperature Relationship of Dwarf Novae, Revisited
Authors: Koji Mukai, and Kristiina Byckling
Figure caption: The maximum temperatures of the X-ray emitting plasma (kTmax) in seven dwarf novae (Byckling et al. 2010) are plotted against their MWD (Pala et al. 2022). Crosses indicate MWD from older literature. The blue curve shows kTs, Kep, the expected temperature in case of strong shock from a Keplerian flow; red lines are the mean trend as determined by these data.
Paper: The Young Binary DQ Tau Produces Another X-Ray Flare Near Periastron
Authors: Konstantin V. Getman, Vitaly V. Akimkin, Nicole Arulanantham, Ágnes Kóspál, Dmitry A. Semenov, Grigorii V. Smirnov-Pinchukov, and Sierk E. van Terwisga
Figure caption: Swift-XRT-UVOT lightcurves near 2021 December 05 periastron passage are compared to previous archived Swift, and XMM/Chandra X-ray (Getman et al. 2011) data. X-ray “characteristic” level is marked by the dotted lines. X-ray luminosity is for the [0.5–8] keV band assuming the new Gaia-based distance d = 195 pc.
Paper: Eight-year Full-depth unWISE Coadds
Authors: Aaron M. Meisner, Dustin Lang, Edward F. Schlafly, and David J. Schlegel
Figure caption: A 4.′1 × 4.′4 region of sky at high Galactic latitude (bgal ≈ 41.°6) centered on (α, δ) ≈ (150.°1106, 1.°3678). At left is a W2 coadd combining all pre-hibernation WISE imaging, and at right is a W2 coadd that incorporates all available WISE and NEOWISE data ranging from early 2010 through late 2020. The coadd at right benefits from ∼8× more total exposure time than the one at left. The grayscale stretch is the same in both cases. Red circles label the locations of ≥5σ sources detected using the crowdsource cataloging software (Schlafly et al. 2019, 2018). Averaging over the ∼2.4 square degree unWISE tile from which these cutouts have been extracted (coadd_id = 1497p015), the 8 yr (1 yr) source density is 4.1 (1.8) per square arcminute, a factor of 2.3× increase.
Paper: Expected FU Ori Outburst Amplitudes from the Optical to the Mid-infrared
Authors: Lynne A. Hillenbrand, and Antonio C. Rodriguez
Figure caption: Top panels: Bright-state spectral energy distribution for an accretion disk-dominated FU Ori type system, accreting at ﹩\dot{M}={10}^{-5}\,{M}_{\odot }﹩ yr−1 (magenta), compared to composite spectral energy distributions (green) for passive + accretion disk systems having low-state accretion rates of ﹩\dot{M}={10}^{-8},{10}^{-7},{10}^{-6}\,{M}_{\odot }﹩ yr−1. In each panel, the same underlying stellar photosphere (navy blue), and passive dust reprocessing disk (cyan) are shown, along with the active gaseous accretion disk (orange); the assumed distance is d = 800 pc. Bottom panels: Expected wavelength-dependent amplitude of an accretion outburst, calculated simply as the flux ratio of the magenta and the green curves, converted to magnitudes. As the low-state accretion rate increases, the outburst amplitudes decrease, and the wavelength dependence of the brightening steepens.
Paper: NGC 1605 is not a Binary Cluster
Authors: Friedrich Anders, Alfred Castro-Ginard, Juan Casado, Carme Jordi, and Lola Balaguer-Núñez
Figure caption: Results of the manual analysis of the putative binary cluster NGC 1605. In each panel, members of NGC 1605 and Can Batlló 1 are highlighted in blue and orange, respectively. Bottom left panel: Sky distribution of Gaia EDR3 stars (G < 19), with average proper motions of the two clusters indicated by arrows. Upper left panel: Proper motion diagram. Top middle: Parallax vs. magnitude. Top right: density profile (including a King profile with rc = 2′, rt = 10′ for comparison). Bottom right panel: Color–magnitude diagram. Also shown are two PARSEC isochrones (blue: log age = 8.3, [M/H] = −0.2, AV = 2.6 mag, d = 2.75 kpc; orange: log age = 8.25, [M/H] = −0.4, AV = 2.8 mag, d = 2.86 kpc).
Paper: Low-resolution Optical Spectroscopy of Recently Discovered Accreting-only Symbiotic Star THA 15–31
Authors: Jaroslav Merc, Stéphane Charbonnel, Olivier Garde, Pascal Le Dû, Lionel Mulato, Thomas Petit, and Rudolf Gális
Figure caption: Low-resolution spectroscopy of THA 15–31. Panel A: De-reddened spectrum of THA 15–31 (green line) together with the intrinsic spectrum of M6 III star (red line; Fluks et al. 1994). Bottom part (blue line) shows the difference between the observed spectrum and spectrum of M6 III star. The identification of strongest emission lines is given in the figure. Panel B: Comparison of the two optical spectra of studied system. Our spectrum and the X-Shooter spectrum are shown in green and orange, respectively.
Paper: Increasing Accretion in the Young Eruptive Star EX Lup
Authors: Á. Kóspál, E. Fiorellino, P. Ábrahám, T. Giannini, and B. Nisini
Figure caption: Top: Optical and near-infrared light curves of EX Lup obtained with the REM telescope (circles) and by the ASAS-SN survey (asterisks) in 2022 February–March. Bottom left: Observed color–magnitude diagrams (dots) compared to the interstellar reddening law for AV = 0.5 mag and R = 3.1 based on Cardelli et al. (1989). Bottom center: Near-infrared color–color diagram. Darker/lighter colors indicate earlier/later data points. The asterisk mark the outburst colors from 2008 April. Bottom right: Lomb–Scargle periodograms. Colors mark the filters as in the top panel. For comparison, we marked the period obtained from radial velocity studies (Kóspál et al. 2014).(The data used to create this figure are available.)
Paper: Yonder: A Python Package for Data Denoising and Reconstruction
Authors: Peng Chen, and Rafael S. de Souza
Figure caption: Example of the effects of measurement errors on mock data. Top left: scatter plot of the error-free data; top right: scatter plot with the noisy mock data and respective error bars; bottom left: scatter plot of the noisy mock data, with arrows pointing from the data to the predicted position by yonder; bottom right: scatter plot of the denoised data.
Paper: A Brightness Classification Boundary in the Kuiper Belt Population
Authors: Kevin J. Napier, and Fred C. Adams
Figure caption: (Top) Inclination vs. eccentricity of all known solar system objects with q > 29 au. Objects with H < 4.5 are displayed as large red circles, objects with 4.5 ≤ H ≤ 5.65 are displayed as medium green circles, and objects with H > 5.65 are displayed as small black circles. The curves depict lines of constant reduced Kozai action ﹩{ \mathcal H }\equiv 1-\cos \,i\sqrt{1-{e}^{2}}﹩, which provides a measure of the dynamical excitation of an orbit. (Bottom) Rolling p-value derived from a 2d KS test in ﹩\sin \,i﹩ vs. e as a function of the H-magnitude cutoff dividing the objects in the top plot into two populations. There is a well-defined minimum at H = 5.65.
Paper: Revisiting HST/FGS Astrometry of ϵ Eridani  
Authors: G. Fritz Benedict
Figure caption: Perturbation to ϵ Eri due to component b. Blue (•) indicates normal NP of FGS 1r measures on the final orbit, derived using RV orbit priors from the GaussFit model. The NP average 3–4 observations of ϵ Eri acquired during each observational sequence (typically 40 minutes). Open circles show the normal point residuals to the final orbit. Upper right insert contains the Llop-Sayson et al. (2021) RV and the GaussFit model orbit that provided the orbit priors. Upper left insert contains the orbit parameters derived from RV and astrometry. That combination reduced the errors of the input orbit parameter priors by factors of ∼3.
Paper: Modifying the Free Energy in Skye
Authors: Adam S. Jermyn, and F. X. Timmes
Figure caption: The absolute difference in the adiabatic temperature gradient ∇ad computed with the Skye EOS using the BC22 and PC10 prescriptions is shown for an even-mass mixture of 12C and 16O as a function of density and temperature.