adsabs/AstroCLIMB huggingface dataset:
Paper: Mapping Venus’s Gravity Field with the VERITAS Mission
Authors: Flavia Giuliani, Daniele Durante, Gael Cascioli, Fabrizio De Marchi, Luciano Iess, Erwan Mazarico, Suzanne Smrekar
Figure caption: Impact of uncertain knowledge of the Fourier expansion coefficients of the thermal tides model on the gravity field uncertainty spectrum. In all cases, Kaula regularization has been applied. In addition to the nominal case, three other scenarios are presented: uncertainties on the coefficients of 10%, 50%, and 100% with respect to the nominal value.
Paper: Mapping Venus’s Gravity Field with the VERITAS Mission
Authors: Flavia Giuliani, Daniele Durante, Gael Cascioli, Fabrizio De Marchi, Luciano Iess, Erwan Mazarico, Suzanne Smrekar
Figure caption: 90th percentile of gravity anomaly uncertainty on Venus’s surface. The black dot represents the required gravity anomaly uncertainty of 7 mGal at degree 95 (cumulative error) and compares this with the results from the nominal (four cycles) and extended (six cycles) mission.
Paper: Mapping Venus’s Gravity Field with the VERITAS Mission
Authors: Flavia Giuliani, Daniele Durante, Gael Cascioli, Fabrizio De Marchi, Luciano Iess, Erwan Mazarico, Suzanne Smrekar
Figure caption: Distribution of the VERITAS-derived degree strength (and equivalently spatial resolution) on the surface of Venus.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Areas of high thermal emission from Amirani as seen in Galileo NIMS observations of the flow field and surrounding area. Figure (a) shows a color mosaic produced from Galileo SSI images. The blue outline shows the area covered by NIMS observation 27i001cr, obtained on 2000 February 22 (b). The white outline shows the area covered by NIMS observation 31i001cr, obtained on 2001 August 6 (c). The NIMS images are created from three bands of NIMS data at 4.6967 μm (red channel), 1.5928 μm (green channel), and 1.3128 μm (blue channel). The red areas are regions of enhanced thermal emission. Figure (a) shows the locations of greatest thermal emission identified in 27i001cr (white numbers 1–5) and 31i001cr (black lettering, A, B, and C). There are distinct differences in the locations of thermal emission, especially in the north of the flow field (1, 2, and A). Thermal emission is also detected from Maui Patera, P61, P162, and Dusura Patera. Image from A. G. Davies et al. (2014).
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: (a) Io’s northern trailing hemisphere as imaged by JunoCam during orbit 57 (2023 December 30). The color portion uses the sunlit portion of JunoCam image 57C00022 (original resolution is 1.8 km per pixel). The grayscale portion at left covers areas seen in “Jupiter-shine” during orbit 57 by JunoCam. This area uses red filter framelets from three JunoCam observations (57C00022, 57C00023, and 57C00024), averaged to reduce noise. (b) JIRAM M-band mosaic from PJ55 sequence JRM_030. The original data has a pixel scale of 6.9 km. Hot spots visible during PJ55 in JIRAM data are labeled. A log stretch was used to accentuate fainter hot spots while preserving details within bright areas such as at Amaterasu Patera. (c) JIRAM L-band mosaic from PJ55 sequence JRM_030. The original data has a pixel scale of 6.9 km. Hot spots visible during PJ55 in JIRAM data are labeled.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: (a) Vivasvant Patera as seen by JunoCam (orbit 57; image 57C00022; 1.8 km pixel scale); (b) JIRAM M-band observation of Vivasvant Patera overlaid on the JunoCam observations (orbit 55; sequence JRM_029; 3.0 km pixel scale). A log stretch was used to accentuate fainter thermal structures while preserving details within bright areas within the Vivasvant patera floor. North is up.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: (a) JunoCam imagery of Kanehekili (center left) and Guaraci Fluctus (center right) and surrounding terrain. North is up. JunoCam images are from orbit 58 (2024 February 3; 58C00024 and 58C00025) and have original pixel scales of 1.0 and 1.6 km. (b) Preliminary updated geological map of Kanehekili Fluctus and Guaraci Fluctus with estimated areas of the low-albedo flow features. Base geologic map is from D. A. Williams et al. (2011), and units presented here are described therein. The most notable are purple areas, which represent various flow units, cross-hatched regions representing dark diffuse deposits, and slashed areas represent red or orange diffuse deposits. North is up.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: 3.5 μm (a) and 4.8 μm (b) spectral radiances from Kanehekili Fluctus and Guaraci Fluctus from JIRAM data up to and including PJ55 (2023 October 15). Also shown are spectral radiances from the Kanehekili region at similar wavelengths derived from JWST and Keck data (I. de Pater et al. 2025). JIRAM circular symbols with black borders denote emission angles >75°. These data combined constrain a powerful eruption at Kanehekili Fluctus that peaked in mid-2022. It is not possible to resolve Kanehekili Fluctus and Guaraci Fluctus in the JWST data: JIRAM and Keck data identify the eruption location.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Hot spots at Amirani (24.3°N, 115°W) observed in a composite of four JIRAM M-band images (a) taken during orbit 55 (2023 October 15). Original data with pixel scales ranging from 4.3 to 4.8 km. (b) shows the same JIRAM composite overlaid on Galileo SSI images acquired in 1999 July and 2000 February. A log stretch was used to accentuate fainter thermal structures while preserving details within bright areas within the Amirani flow field. North is up.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Examples of paterae with annular thermal structures: Monan Patera, Maui Patera, Chors Patera, Surt, Dazhbog Patera, and Tupan Patera. For each example, a JIRAM composite from orbit 55 is on the left while a visible-light composite from either Galileo SSI (Monan, Maui, and Tupan) or JunoCam (Chors, Surt, and Dazhbog) is on the right. M-band data from orbit 55 was used except for Dazhbog and Tupan, where the L-band composite was used. Alternating bright/dark columns of pixels are a camera artifact.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: Examples of paterae with uniform thermal structures: Amaterasu Patera, E Surya (P62), Dusura Patera, Sigurd Patera, Pajonn Patera, and Emakong Patera. For each example, a JIRAM composite from orbit 55 is on the left while a visible-light composite from either Galileo SSI (E Surya, Dusura, Sigurd, Pajonn, and Emakong) or JunoCam (Amaterasu) is on the right. M-band data from orbit 55 was used except for Amaterasu and Sigurd, where the L-band composite was used. For Amaterasu Patera in more detail, see Appendix C.
Paper: Hot Spot Detections and Volcanic Changes on Io during the Juno Epoch: Orbits PJ5 to PJ55
Authors: Jason E. Perry, Ashley Gerard Davies, David A. Williams, David M. Nelson
Figure caption: 4.8 μm spectral radiance from four northern trailing hemisphere paterae: Dazhbog, Amaterasu, Kinich Ahau, and Surt. Spectral radiances for these paterae are typically below 10 GW μm−1 except during brightenings, such as at Amaterasu in 2019 and 2023, and Surt in 2020. The hollow data points are measurements that include nonlinear/saturated pixels. These values should be treated as lower limits.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Density heat maps showing where debris is typically found over (a) 1 week, (b) 1 yr, (c) 1–4 yr, and (d) longer than 4 yr after the DART impact. Blue indicates no debris, and orange is a high density of debris. The color scale is logarithmic and truncated at a maximum of 50 particles to aid interpretation.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The fate of the ejecta over time, showing the number of particles that escape or impact with the primary or secondary. Impacts with the secondary generally only occur within the first year after the impact, while primary impacts or escapes can happen later.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The trajectory of a 70 cm radius debris particle with an initial ejection velocity of 7.8 cm s–1 surviving for the full 5 yr, plotted in an inertial frame with the x-axis aligned with the initial position of Dimorphos and the z-axis aligned with the system’s total angular momentum.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: A particle entering a long-term 1:3 resonance with Dimorphos. Eventually, the particle is perturbed out of this resonance before escaping the system.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: For the 4:1 resonant particle, the (a) eccentricity and (b) inclination of the particle over time. The effect of the resonance on eccentricity is apparent.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The instantaneous Keplerian orbit period of the particle, along with the 4:1 resonance with the stroboscopic orbit period of Dimorphos.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: For a long-surviving debris particle with 70 cm radius and an initial ejection velocity of 7.8 cm s–1, plots of (a) the eccentricity and (b) the inclination. This demonstrates a wide, eccentric, and inclined orbital history.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: For particles lasting at least 4 yr, the average and maximum periapsis velocity as a function of particle radius.
Paper: Fully Coherent Model of Dynamics around Binary Asteroids: Application to Didymos and the DART Impact
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The cumulative distribution of debris, expressed as the percent of remaining debris particles over time. Vertical lines correspond to perihelion passages of the Didymos system.
Paper: Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma
Authors: A. Cabra, X. Wang, M. Horányi
Figure caption: Patched charge model (X. Wang et al. 2016). Blue patches are charged due to direct exposure to plasma and/or UV, and red patches within a microcavity are charged by secondary electrons and/or photoelectrons induced by incoming electrons, ions, and/or photons.
Paper: Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma
Authors: A. Cabra, X. Wang, M. Horányi
Figure caption: (a) Schematic of the experimental setup in the CSWE chamber; (b) IEA I-V curves of ions with various energies at the location of the dust plate, showing a similar flux for all energies.
Paper: Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma
Authors: A. Cabra, X. Wang, M. Horányi
Figure caption: Potential as a function of distance from the glass plate for different ion energies.
Paper: Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma
Authors: A. Cabra, X. Wang, M. Horányi
Figure caption: Images of three simulants before and after exposure to the simulated solar wind plasma with the ion energy varying across a full range from 100 eV through 1000 eV in one trial. Mobilization areas in the JSC-1 images are highlighted in red circles.
Paper: Laboratory Study of Dust Mobilization on Airless Planetary Bodies in the Solar Wind Plasma
Authors: A. Cabra, X. Wang, M. Horányi
Figure caption: Mobility as a function of ion energy for three simulants.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: 53Mn–53Cr isochrons for two EC 002 fragments. An F-test for the slopes of the two isochrons gave an F value of 11.01, which is significantly higher than the critical value of 4.99 with significance level of 1%, strongly arguing for the different slopes of the two isochrons. The isochron of EC-2 is consistent with previous 26Al–26Mg and 53Mn–53Cr chronological studies (A. Anand et al. 2022; L. Fang et al. 2022; P. M. Reger et al. 2023). The isochron of EC-1 has a steeper slope and a lower intercept, giving a much older nominal crystallization age than all previous chronological results.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: Present-day ε53Cr value vs. 55Mn/52Cr value for chondrites. The shaded areas represent the present-day ε53Cr value evolving with a constant 55Mn/52Cr value from ε53CrSSi values of −0.37 ± 0.06 (light green) and −0.29 ± 0.05 (blue). The initial 53Mn/55Mn ratio of 7.71 × 10−6 suggested by P. M. Kruttasch et al. (2024) was used. The actual ε53Cr values of all chondrites plot above the light green area. The chondritic data are from K. Zhu et al. (2021).
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: Single-stage evolution curve of ε53Cr value in the solar system. The solar system age of 4568.14 Ma, ε53CrSSi value of −0.29 ± 0.05, and 53Mn/55MnSSi value of 7.71 × 10−6 were used (P. M. Kruttasch et al. 2024).
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: ε53Cr values plotted against the Cr contents of different separate minerals from two EC 002 samples. The plots do not plot along a straight line for either EC-1 or EC-2, indicating the robustness of the 53Mn–53Cr chronology of the EC 002 meteorite.
Paper: Highly Heterogeneous Parent Body of the Rare Andesitic Erg Chech 002 Meteorite Revealed by the Revisited Mn–Cr Isotopic Systematics
Authors: Bing Yang, Runlian Pang, Qing Wang, Anning Zhang, Wei Du, Liping Qin
Figure caption: Highly heterogeneous Cr isotopic compositions of the four EC 002 fragments. The data for EC-A and EC-Z are from A. Anand et al. (2022) and K. Zhu et al. (2022), respectively.
Paper: Exploring Mixing Thresholds in Asteroseismic Stellar Evolution Models
Authors: Lynn Buchele
Figure caption: Left: the top panel shows the test mode frequency over time. The inset zooms in to show some differences in the frequency evolution. The middle panel shows the numerical time derivative of the test frequency. The bottom panel shows the interpolation error as defined in Equation (2). The dark gray horizontal shading shows the 1σ range typical of frequencies of stars observed by Kepler. In all three panels, the vertical light gray shading indicates the range of profiles plotted in the right column. Right: hydrogen abundance profiles around the overshoot boundary for selected profiles from each track. In all three panels, the lighter colored lines correspond to younger models.
Paper: An Atlas of Spectroheliograms from 3641 to 6600 Å
Authors: P. Váradi Nagy, A. G. M. Pietrow
Figure caption: A set of four spectroheliograms with corresponding cube spectra from the atlas, and the instruments used to capture them. The respective spectroheliograms correspond to the location of the orange line on the spectrum. The solar disks are tuned to (a) Hα 6563 Å, (b) Ca II K 3934 Å, (c) He D3 5876 Å, and (d) Fe II 5169 Å. The instruments shown in panel (e) are the Sol’Ex (#1) and the SHG 700 (#2), with panel (f) showing the Sol’Ex mounted and scanning the solar disk.
Paper: Empirical Globular Cluster Ridgeline Construction on Gaia Data
Authors: Anett Simon-Zsók, László Molnár, Csilla Kalup, Meridith Joyce
Figure caption: The ridgeline determination workflow in case of globular cluster NGC 6397 as an example. (A): Primary ridgeline after applying the LOWESS algorithm along the Y-axis. (B): The CMD and the primary ridgeline in the transformed coordinate system. (C): The the X coordinate of the blue points are maximum value of the KDE in a bin. The Y coordinates are the median values for the bins. The orange line is the cubic interpolation along the blue points. (D): The final ridgeline after the rotating back to the original coordinate system.
Paper: The Nature of an Unidentified X-Ray Source in the 7 Ms Chandra Deep Field-South Catalog
Authors: Quinn P. Sullivan, Zhibo Yu, William N. Brandt, Bin Luo, Fan Zou
Figure caption: Top-left: composite image of XID 912 and its potential host galaxy XID 916 using JWST filters (F150W, F200W, and F277W). The yellow solid circle and cyan dashed circle show the 90% and the 1σ X-ray positional uncertainty of XID 912, respectively (B. Luo et al. 2017). We defined the red circle as our photometric aperture for the JWST filters. A 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 scale bar is in the upper right. Top-right: zoomed image centered on the reported position of XID 912 from B. Luo et al. (2017). All circle definitions are identical to those in the top-left panel. Bottom-left: best-fit SED using Model A assuming z = 0.105. Bottom-right: best-fit SED using Model B. No redshift was assumed.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XXIV. HD 27376 (41 Eri)
Authors: Richard Monier
Figure caption: Left: synthesis of the Hg II line at 3983.93 Å of HD 27376 A (observed spectrum in black, synthetic spectrum in red). Right: synthesis of the Xe II line at 4603.03 Å.
Paper: Candidate C III] Emission in a Massive, Compact, z ∼ 4.5 Galaxy
Authors: Alfonso Meléndez, Olivia Cooper, Hollis Akins, Caitlin M. Casey, Stephanie Urbano Stawinski, Marko Shuntov, Louise Paquereau, Jeyhan Kartaltepe, Maximilien Franco, Vasily Kokorev, Jake Magee, Mia Fong, Andreas Faisst, Crystal Martin
Figure caption: Top Left: ﹩1\mathop{.}\limits^{^{\prime\prime} }5\times 1\mathop{.}\limits^{^{\prime\prime} }5﹩ JWST F277W image of our target, with contours at even integer times the RMS starting at 40. Top Right: best-fit SED and probability distribution functions for photometric redshift and stellar mass. Bottom: MOSFIRE 1D spectrum in arbitrary units (upper) optimally extracted from the 2D spectrum (lower). We detect candidate C III] emission at 3.6σ. We calculate S/N from the integrated signal in the 1D spectrum around a small region centered on the peak, as measured via the Gaussian fit to the line. Errors were estimated by bootstrapping from observed error (gray shading) over the same region of the 1D spectrum, excluding sky lines.
Paper: NEIDSpecMatch: Stellar Parameter Estimation with NEID Spectra Using an Empirical Library
Authors: Te Han, Paul Robertson, Caleb I. Cañas, Gudmundur Stefansson, Shubham Kanodia, Joe P. Ninan, Jaime A. Alvarado-Montes, Chad F. Bender, Jiayin Dong, Rachel Fernandes, Arvind F. Gupta, Samuel Halverson, Daniel M. Krolikowski, Andrea S. J. Lin, Suvrath Mahadevan, Leonardo A. Paredes, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The NEIDSpecMatch library distribution and TIC 437229644 spectral fit (order index 102). Top left: 78 NEIDSpecMatch library stars in Teff, [Fe/H], and ﹩\mathrm{log}g﹩ space: archival parameters (blue) vs. cross-validation results (red line endpoints). Top right: residuals (recovered [Fe/H] − archival [Fe/H]) vs. archival [Fe/H]. Bottom: the composite spectrum (red) derived with 5 best-fit library star spectra (black, weighted by ci) plotted against the spectrum of TIC 437229644 (Target Spectrum).
Paper: JWST Observations of Potentially Hazardous Asteroid 2024 YR4
Authors: A. S. Rivkin, T. Mueller, E. MacLennan, B. Holler, A. Burdanov, J. de Wit, P. Pravec, M. Micheli, M. Devogele, L. Conversi, C. A. Thomas, D. Farnocchia, J. L. Dotson, L. Wheeler, H. Hammel, S. N. Milam, J. de Leon, A. Glantzberg
Figure caption: NEATM size determination for 2024 YR4. The MIRI measurements are shown as horizontal dashed lines (±1σ absolute flux uncertainty). The solid lines are NEATM model predictions at 10.0, 12.8, and 15.0 μm, considering the range of beaming parameters η compatible with the measured flux ratios for all 3 bands. The intersections of the vertical dotted lines with the x-axis indicate the corresponding size constraints for each band.
Paper: Stellar Parameters for over 50 Million Stars from SMSS DR4 and Gaia DR3
Authors: Yang Huang, Timothy C. Beers
Figure caption: Left panel: comparison of photometric metallicity estimates with those from GALAH DR4 (S. Buder et al. 2024). The color-coded contours represent stellar number density. The median offset and scatter in metallicity differences between GALAH DR4 and our photometric estimates are −0.02 dex and 0.12 dex, respectively. Right panel: comparison of photometric-metallicity estimates with high-resolution spectroscopic (HRS) metallicities from the GALAH DR4 database for dwarf (red squares) and giant (blue squares) stars. The small and large circles denote stars with carbon enhancements (+0.7 < [C/Fe] ≤ +2.0) and extreme carbon enhancements ([C/Fe] > +2.0), respectively. The central dashed line represents the one-to-one correspondence. The median offset and scatter in metallicity differences between the HRS and photometric estimates are −0.17 dex and 0.26 dex, respectively. When excluding carbon-enhanced metal-poor stars with [C/Fe] > +0.7, the median offset and scatter improve to −0.10 dex and 0.24 dex, respectively.