adsabs/AstroCLIMB huggingface dataset:
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: H2O/O2 column density ratio derived from MCMC fits to retrieved aurora brightnesses. The dashed gray line shows the weighted average of the individual points and the shaded gray region shows the asymmetric uncertainty of the weighted average. This average column density ratio of 0.10﹩{}_{-0.04}^{+0.05}﹩ matches the upper limit found by de Kleer et al. (2023) for the same date.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Illustration of the two types of meshes–quasi-uniform mesh (a) and variable-resolution mesh (b) used in the MPAS-A simulations.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Temporally averaged maps in MPAS-A (first column), ExoCAM (second column), LMD-G (third column), and UM (fourth column). Panels (a)–(d): SST (kelvin); panels (e)–(h): column-integrated cloud water path (log10(kilogram per square meter)); panels (i)–(l): planetary albedo; panels (m)–(p): TOA OLR (watt per square meter); and panels (q)–(t): long-wave cloud radiative effect (watt per square meter). Maps are heliocentric, with the orange dot denoting the substellar point. The dayside (nightside) average values are marked at the center (right) of each panel.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Total horizontal winds ((a)–(d)), divergent component ((e)–(h)), and rotational component ((i)–(l)) at 940 hPa in the four models. The vertical wind is shown in colors (meter per second), with red (blue) representing upward (downward) flows.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Dayside (left) and nightside (right) average profiles of temperature ((a) and (b)), relative humidity ((c) and (d)), liquid cloud mixing ratio ((e) and (f)), and ice cloud mixing ratio ((g) and (h)). The shaded area denotes the standard deviation.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Transit spectra at the west ((a) and (b)) and east ((c) and (d)) terminators. Left column: comparisons between the three models—ExoCAM, LMD-G, and MPAS-A (60_10 km case). Right column: comparisons between simulations with different resolutions. The shaded area denotes the standard deviation.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Temporally averaged cloud fraction in the four models, calculated using two methods. Panels (a)–(d): cloud water path threshold (cloud fraction = 1 when cloud water path > 0.02 kg m−2 and 0 otherwise); panels (e)–(h): parameterized using relative humidity (Equations (1) and (2)). Dayside (nightside) average values are marked at the center (right) of each panel.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Total horizontal winds at 940 hPa with convection parameterization turned on (a) and off (b) for the 120 km horizontal-resolution case. The vertical wind is shown in colors (meter per second), with red (blue) representing upward (downward) flows.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Dayside average profiles of liquid (a) and ice (b) clouds. The dashed lines denote the sensitivity experiments with subgrid convection parameterization turned off.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Same as Figure 4 but for the MPAS-A simulations with different grid resolutions.
Paper: Simulated Climate of TRAPPIST-1e Using MPAS-A and Comparisons with Other GCMs
Authors: Lixiang Gu, Jun Yang, Mingyu Yan
Figure caption: Phase-curve comparison between (a) four models: ExoCAM, LMD-G, UM, and MPAS-A (60_10 km case) and (b) MPAS-A simulations with five different resolutions. The shaded area denotes the standard deviation.
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Disk-integrated brightness of Ganymede’s [O I] 630.0 nm aurora (Table 2) as a function of distance from the plasma sheet midplane. The black points are the observations with error bars showing the combined random and systematic uncertainties. The gray line is a fit of Equation (5) with B 0 = (136 ± 4) R and the scale height H fixed to 2.78 R J (Bagenal & Delamere 2011). The shaded gray region shows the uncertainty in the peak brightness (B 0) of the fit. The fit shows that the brightness exhibits a moderate correlation with distance from the plasma sheet midplane and has an expected peak brightness of about 136 R if the oscillation is due to localized variations in plasma density. In this figure, the timing of the observations moves from right to left: Ganymede was above the plasma sheet midplane at the start of the observations and moved through the center to below the sheet by the end of the night.
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Calibrated images of Ganymede’s [O I] 630.0 nm auroral emission displayed in 20 R contours. To better reveal the spatial variability, we smoothed the data using a Gaussian kernel with an FWHM of 0.″5 approximating typical seeing conditions for the morning of 2021 June 8 UTC. The time in the upper left of each image is the UTC time at the start of the observation; the annotation in the lower right is the distance to the plasma sheet centrifugal equator and is positive when Ganymede is above the midplane and negative when it is below. As Ganymede moved vertically through the plasma sheet, the hemisphere closest to the midplane exhibited the brightest aurora. From approximately 14:00 to 14:45 UTC, Ganymede is within ±0.5 R J, and the brightness is more evenly distributed across the disk. Ganymede passed through the highest-density plasma midplane at 14:20 UTC, so the top two rows display data when Ganymede was above the midplane (with enhanced brightness at southern latitudes), and the bottom row displays data when Ganymede was below the midplane (with enhanced brightness at northern latitudes). Because of the blurring effect of atmospheric seeing, the calibrated brightness distribution of the individual pixels is lower than the disk-averaged value reported in de Kleer et al. (2023) and Table 1, which assume all emission originates from a disk with Ganymede’s solid angular size. The white grid shows the physical size and orientation of Ganymede, with north pointing upward (for more details on this observing geometry, see Figure 2).(The data used to create this figure are available.)
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Hemispheric observing geometry of Ganymede on 2021 June 8 between 12:58 and 15:08 UTC. Due to the geometry of eclipse observations, the line of sight intersected near the center of the sub-Jovian hemisphere. The subobserver longitude changed over the duration of the observations by ±2.3° from the central longitude in this projection. Labels mark latitude and planetocentric east longitude; the thicker black line shows the prime meridian. The dashed black lines show the locations of the auroral ovals (Duling et al. 2022), marking the boundary between the open and closed field lines of Ganymede’s magnetic field. In this view the leading hemisphere is on the left and the trailing hemisphere is on the right. Ganymede surface map courtesy of the United States Geological Survey (USGS 2020).
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Line-of-sight observing geometry of Ganymede during eclipse by Jupiter on 2021 June 8 UTC. The inset axis shows a zoom-in on the Jovian system with the positions and orbits of the other Galilean satellites. Earth’s position relative to Jupiter allowed us to observe Ganymede as it passed into Jupiter’s umbra. We retrieved the positions of planets and their orbital elements using JPL Horizons, and we have exaggerated the physical sizes of the planets and Jupiter’s umbra (but not the relative spacing of the orbits) for illustrative purposes.
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Ratio of Ganymede’s [O I] 630.0 nm auroral emission between its dusk and dawn hemispheres out to an angular distance of 2.25 R  G . The horizontal dashed gray line indicates a ratio of 1 (equal average brightness between hemispheres), and the vertical dashed gray line shows where Ganymede passed through the center of the plasma sheet. The horizontal line is a best-fit constant and the shaded gray area shows the uncertainty in the fit.
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Ratio of Ganymede’s [O I] 630.0 nm auroral emission between its northern and southern hemispheres out to an angular distance of 2.25 R  G . The horizontal dashed gray line indicates a ratio of 1 (equal average brightness between hemispheres), and the vertical dashed gray line shows where Ganymede passed through the center of the plasma sheet. The diagonal line shows the expected brightness ratio due to asymmetric flux tube electron column densities (Equation (6)).
Paper: Short-timescale Spatial Variability of Ganymede’s Optical Aurora
Authors: Zachariah Milby, Katherine de Kleer, Carl Schmidt, François Leblanc
Figure caption: Geometric relationships relevant to the retrieval of electron properties. Ganymede orbits Jupiter at a distance of r G. However, because of the tilt of the magnetic field rotation axis Ω m relative to the Joviographic rotation axis Ω, Ganymede’s distance d from the centrifugal equator varies over the approximately 10 hr magnetospheric rotation period of Jupiter. See Phipps & Bagenal (2021) for a detailed description of this geometry. Image credits: Jupiter (JPL 2001), Ganymede (USGS 2020).
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Top: illustration of the angle ψ, which describes a TNO’s position relative to Neptune when the TNO is at perihelion. Bottom: example evolution of resonant (colored) and nonresonant (gray) particles with q = 33 au in a–ψ space for the 2:1, 7:3, and 5:2 resonances in the circular restricted three-body problem (Sun + Neptune + massless test particles). Within each panel, individual resonant particles are given distinct colors; note the clear islands traced out by the resonant particles.
Paper: Uranus’s Influence on Neptune’s Exterior Mean-motion Resonances
Authors: Severance Graham, Kathryn Volk
Figure caption: Relative strength of the N:1 (black), N:2 (pink), and N:3 (yellow) resonances with Neptune for low-inclination particles with q = 33 au in a model of the current solar system (with the Sun and all four giant planets as perturbers). Our strength metric is normalized to the largest value across all resonances and is a measure of how confined test particles are to each resonance (see the Appendix).
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: Maximum detectable range in the ecliptic plane for nominal thermal model parameters. At a point on one of the contours, the flux from an asteroid of the specified diameter, with the nominal thermal model parameters, is equal to the 5σ detection threshold for the ecliptic latitude/longitude of the line of sight from the telescope to the target. The gray shaded regions are excluded because the solar elongation angle is less than 45° or greater than 120°.
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: Sample of 1000 potentially hazardous orbits with MOID < 0.01 au. (a) and (b) Relative probability of impact, logarithmic color scale. (c) and (d) Impact speed.
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: NEO Surveyor 5 yr survey completeness as a function of hazard for a 140 m diameter asteroid in a random sample of 1000 PHA orbits.
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: Detector geometry for each of the two wave bands. Gray squares represent the light-collecting area of the four detector arrays. The tracklets labeled 1–5 are described in the main text.
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: Survey completeness for NEOs larger than 140 m vs. time, as predicted by the detailed NSS time-domain simulation (blue; from Mainzer et al. 2023) and this model (red).
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: For an impact that occurs at the end of a 10 yr survey, (a) 10th, 50th, and 90th percentile warning times as a function of impact energy, derived from a sample of 1000 orbits, and (b) probability of no warning.
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: (a) Observing geometry. (b) Asteroid flux for 140 m diameter as a function of solar longitude and range for the NC2 band, as predicted by the nominal NEATM model. The gray regions are excluded by the NEO Surveyor observing constraints.
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: Probability of prior discovery of impactor with energy exceeding the value on the x-axis. The wavy structure in the curves is an artifact from the discrete sampling of the asteroid diameter distribution (Figure 14(a)).
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: 5σ detection sensitivity (units: microjanskys) as a function of ecliptic latitude and longitude for (a) the NC1 channel and (b) the NC2 channel.
Paper: Asteroid Impact Hazard Warning from the Near-Earth Object Surveyor Mission
Authors: Oliver Lay, Joe Masiero, Tommy Grav, Amy Mainzer, Frank Masci, Edward Wright
Figure caption: Two NEO orbits with the same orbital elements, except the left panel has inclination = 0°, and the right panel has inclination = 60°.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) ShadowCam mosaic of the Faustini PSR composed of images acquired during 2023 January and February. The Sun direction is to the right. (b) Geomorphic map highlighting terrain features within the PSR. Axes are distances from the South Pole (left sides of panels are the poleward side). The larger white box is the location of the ShadowCam image in Figures 4 and 14, and smaller white boxes are locations of Figure 10(a)–(b), 10(c)–(d), and 10(e)–(f) (left to right). The lunar nearside is toward the top of the panel.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) A portion of the ShadowCam mosaic in Figure 1 showing the boundary (thin white line) between the Middle (top) and Lower (bottom) units corresponding to the −2740 m contour. Colored dashed boxes are crater count areas on the Middle and Lower units. The white box is the location of panel (b), showing an enlarged view of the unit boundary with EHT visible on the Middle unit (upper half). (c) CSFDs of the three count areas in panel (a) and Figure 6(a), with absolute model age isochrons (solid) from G. Neukum et al. (2001) and the saturation equilibrium line (dashed) from N. J. Trask (1966). Marker colors reflect the respective colors of the mapped units in Figure 1 and 6 containing the count areas. (d) Elevation profile, with location shown as a yellow line in panel (a). EHT is observed above ∼−2740 m elevation. Count areas correspond to the relatively flat areas of the profile on the Middle and Lower units.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: Shaded relief maps of the floor of Faustini crater derived from the 20 m pixel−1 DEM (M. K. Barker et al. 2023) showing (a) elevation, (b) slope, (c) roughness, and (d) roughness filtered with a Gaussian-weighted moving average. Contours are elevations −2740 and −2710 m. The white box in panel (a) is the location of Figure 5.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) Locations of craters associated with boulders on an elevation map of the Faustini floor with unit boundaries from Figure 1. Craters are categorized by number of boulders from low (<5) to high (>100) and plotted in panel (b) as histograms for each of the units. (c) Mini-RF δCPR from C. I. Fassett et al. (2024) of the Faustini floor, with crater locations marked in panel (d) showing elevated CPR values where craters with boulders are identified.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) Shaded relief of Faustini floor showing areas used to mask the surface roughness (20 m pixel−1 VRM) for the Upper, Middle, and Lower units in Figure 1 to show (b) the distribution of roughness values for these units. Boundaries are based on −2710 and −2740 m elevation contours, with the central mound included in the Middle unit, though it extends above −2710 m. The white boxes are the crater count areas used for Figure 8.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) ShadowCam image M15308992S; (b) elevation profile across Faustini floor. The location of the image is shown in Figure 1(b). The line in panel (a) shows the location of the elevation profile. Black arrows denote the wall/floor contacts, and gray arrows are the locations of transitions between Upper and Middle (right) and between Middle and Lower (left) morphologic units in Figures 1(b) and 6(a).
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: Scatter plots of surface roughness indices (a) TRI and (b) VRM vs. slope using the 20 m pixel−1 DEM from M. K. Barker et al. (2023) for the region in Figure 1(b).
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) Portion of ShadowCam mosaic, colorized with elevation in panel (b), showing a broad ridge dissecting the Lower unit. Portions of the ridge appear bounded by lobate scarps (white arrows). See Figure 3(a) for location.
Paper: The Faustini Permanently Shadowed Region on the Moon
Authors: Jean-Pierre Williams, Prasun Mahanti, Mark S. Robinson, Robert V. Wagner, Marley Chertok, Norbert Schörghofer, Erwan Mazarico, Brett W. Denevi, Shuai Li, David A. Paige
Figure caption: (a) RGB composite of VRM derived from 20, 40, and 80 m pixel−1 DEMs highlighting roughness at different length scales; (b) unit boundaries from Figures 1 and 6 are shown in white for reference.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as C-types. Plotted are (1) Ceres (DeMeo et al. 2009; black open squares), CM2 chondrite Murchison (<63 μm, heated to 500°C; red line), L5 chondrite Tsarev (<40 μm, laser irradiated; blue line), and brachinite Brachina (<63 μm, cleaned with HCl; green line). The Ceres spectrum was normalized to unity at 0.55 μm and then multiplied by 0.1132 (Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ. Even though brachinite is not spectrally similar to C-types, it is classified as a C-type because the other given options (X, Xe, Xk, Xn) are much worse spectral matches.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as B-types. Plotted are (2) Pallas (DeMeo et al. 2009; black open squares), CV3 chondrite Allende (125–500 μm; red line), CM1 chondrite MET 01070 (<75 μm; blue line), and lunar meteorite (anorth) ALHA81005 (chip; green line). The Pallas spectrum was normalized to unity at 0.55 μm and then multiplied by 0.1587 (Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ.
Paper: Testing the Bus–DeMeo Asteroid Taxonomy Using Meteorite Spectra
Authors: Thomas H. Burbine, Iman Khanani, Deepika Kumawat, Ahlay Hussain, Sydney M. Wallace, M. Darby Dyar
Figure caption: Reflectance spectra of objects classified as K-types. Plotted are (221) Eos (DeMeo et al. 2009; black open squares), CM2 chondrite LEW 87148 (<125 μm; red line), CV3 chondrite ALH 84028 (<125 μm; blue line), and R3 chondrite PRE 95411 (<125 μm; green line). The Eos spectrum was normalized to unity at 0.55 μm and then multiplied by 0.1400 (IRAS albedo; Tedesco et al. 2004). The error bars for the asteroid spectrum are 1σ.