adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: Upper panel: distribution of detected pixel clusters (red polygons) overlaid on the Galileo/SSI basemap (adopted from M. Malaska et al. 2018, 2024). Inset: the yellow box shows the locational context of the investigated image on the United States Geological Survey (USGS) Voyager and Galileo/SSI global mosaic at a resolution of 500 m pixel−1 (the USGS’s Voyager and Galileo/SSI global mosaic can be accessed at https://astrogeology.usgs.gov/search/map/europa_voyager_galileo_ssi_global_mosaic_500m). Note that the average spectrum of each pixel cluster is provided in Appendix Figure 10. Bottom panel: a portion of the geologic map of the same region on Europa (adopted from E. J. Leonard et al. 2024). The violet color shaded feature represents the band unit, while linear features include the cycloid (aqua blue line), linear band (navy blue line), depression margin (wider black line), and ridges/troughs (narrow black lines). The dark green asterisk symbol represents microchaos features. Refer to E. J. Leonard et al. (2024) for details of the map elements. The detected pixel clusters in the upper panel correlate with microchaos, linear, and band geologic units in the bottom panel.
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: An example of the noise removal routine applied to the NIMS scan. Left panel: spectral denoising using despiking approach applied to the Minnaert-corrected spectrum (black dots). The black arrow indicates a random noise spike near ∼2.3 μm that was removed in the despiked spectrum (red line). Any black dot (Minnaert-corrected data point) not coinciding with the red line (despiked spectrum) is considered a noise artifact and was removed and replaced during the despiking step. Right panel: radiation noise removal via spatial smoothing applied to the despiked spectrum (black dots). The black arrow indicates a singleband noise artifact near ∼2.2 μm that was treated in the final smoothed spectrum (blue line). Any black dot (despiked data point) not aligned with the blue line (spatially smoothed spectrum) is considered radiation noise and was corrected during the radiation removal step. Inset is the figure with a zoom on the ∼2.05–2.40 μm region. The x, y coordinates are the location of the pixel in NIMS observation 11ENCYCLOD01A of M. Malaska et al. (2024).
Paper: Detection of an NH3 Absorption Band at 2.2 μm on Europa
Authors: A. Emran
Figure caption: Upper panel: locational distribution of detected pixels (red polygons) and some regions of nondetected pixels (indigo polygons) using fifth-degree polynomial continuum fit from Galileo/NIMS observation 11ENCYCLOD01A overlaid on the Galileo/SSI basemap (M. Malaska et al. 2018, 2024). Middle panel: the continuum fits to the average reflectance spectra of detected pixels (left subplot) and some nondetected pixels (right subplot) in the NIMS scan. Lower panel: the continuum-removed average spectra along with associated standard errors against the continuum baseline for detected pixels (left subplot) and some nondetected pixels (right subplot). For detected pixels, the reflectance and standard error values at 2.19–2.21 μm fall clearly below the continuum baseline, which confirms the feature exceeds the noise level.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: Model images of a 1200 K, dawn-centered Na source. Top Row: modeled radiance at TAA = 0° (left), 90° (middle), and 290° (right). Second row: column density (N) taken from the model at the same TAAs. Third Row: approximated column density (﹩\widetilde{N}﹩) determined by the inverse of Equation (6). The color scales for the second and third rows are the same. Bottom row: ﹩\widetilde{N}/N﹩. Regions with no Na present are shown in light gray. The stretch of the colorbar in the last row is not symmetric for values greater than and less than 1.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: Same as Figure 9, using a 50,000 K, dawn-centered Ca source.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: Altitude profiles over Mercury’s north pole for 1200 K sources that are uniform over the dayside northern hemisphere (red) and the dayside southern hemisphere (blue).
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: HST and VLA X- and Ku-band observations on April 6–7. The observing geometry from Earth only allowed hemispherical coverage of the planet, so that the two hemispheres are separated by 24 hr, or 2.5 Jovian rotations. The top row shows the red and blue filter composite of the HST observations, the middle row shows the VLA X-band observations centered around 10 GHz with a 4 GHz bandwidth, and the bottom row shows the VLA Ku-band observations centered around 15 GHz with a 6 GHz bandwidth. A Gaussian filter was used for the Ku-band data to remove any nonzonal large-scale structure (see Appendix B). The red outline indicates where we have simultaneous coverage across all six Juno frequencies.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Nadir probing weighting functions that indicate the pressure range over which the thermal emission is integrated for the indicated frequencies. The Juno frequencies are presented on the left-hand side, while the VLA frequencies are shown on the right-hand side, with lower frequencies probing deeper into the planet. The weighting functions are based on the mean tropical atmosphere of Jupiter that we retrieved from the PJ19 data (see Figure 7) coupled to a dry adiabat (C. Moeckel et al. 2023). Note that we do not include the absorption of alkali metals as found by A. Bhattacharya et al. (2023), which will add more absorption for C1.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: HST and VLA observations taken during Juno’s PJ19 encounter. The top panel shows the HST observations, while the bottom panel contains a VLA composite made of the three frequency bands (see Figures 2 and 3). Each frequency corresponds to a color channel: red hues (X band/10 GHz) show warm brightness temperatures, regions depleted in ammonia, and probing deepest into the atmosphere. Green/yellow colors (Ku band/15 GHz) show the structure under the ammonia ice clouds, and white and blue colors (K band/20 GHz) probe highest to the pressures around the ammonia ice clouds. The dark regions north of the equator correspond to the coldest brightness temperatures on the planet—the ammonia plumes as part of the equatorially trapped Rossby wave (A. J. Friedson 2005).
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Same as Figure 2, but for the observations on April 8–9. The middle row shows the VLA K-band observations around 20 GHz with a 4 GHz wide bandwidth, and the bottom row shows the K-band observations around 24 GHz with a 4 GHz bandwidth. This bottom panel was heavily filtered and should be considered qualitative.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Deconvolved PJ19 Juno observations that map out the nadir brightness temperature distribution for the six channels. The channel numbers are increasing left to right. The color bar for each panel is appended to the top of the plot. The resolution is set by the size of the individual beams and the number of overlapping observations (C. Moeckel et al. 2025). The lower frequencies cover less area owing to the larger beam size and therefore dictate the region over which we have full frequency coverage. These maps were independently produced, analyzed, and published by S. J. Bolton et al. (2021).
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: The best spectral matches to Europa’s leading hemisphere in the visible. The magnesium sulfate epsomite model and hydrated sulfuric acid model match the best and then meridianiite. The infrared is best matched by the NaCl brines because that portion of the spectrum of the disk-integrated leading hemisphere is dominated by water ice. It is also likely the match of sulfuric acid hydrate in the infrared would improve with different sample preparations and smaller grain sizes.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Visible-infrared Spectra of keV Electron Irradiated Cryogenic Salts with Implications for Europa Surface Composition
Authors: C. A. Hibbitts, K. Stockstill-Cahill, E. Lloyd, E. Gloesener, M. Choukroun, C. Paranicas, R. N. Clark
Figure caption: The best spectral matches to Europa’s trailing hemisphere in the visible are again consistent with hydrated magnesium sulfate but also a mixture of NaCl and partially hydrated MgCl2. However, MgCl2·nH2O significantly mismatches in the shortwave. An additional material absorbing at 0.6 μm continues to be needed.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Doomed Worlds. II. Reassessing Suggestions of Orbital Decay for TrES-5 b
Authors: Marvin Rothmeier, Elisabeth R. Adams, Karsten Schindler, André Beck, Brian Jackson, Jeffrey P. Morgenthaler, Amanda A. Sickafoose, Malia Barker, Luigi Mancini, John Southworth, Daniel Evans, Alfred Krabbe
Figure caption: Timing residuals of a linear versus a quadratic model after adding new data (2007–2024). Top: O  − C midtimes assuming a linear ephemeris. New midtimes derived from TESS light curves are shown in green, while new ground-based observations are in blue. Literature midtimes compiled by E. S. Ivshina & J. N. Winn (2022) are in black, and those from the ETD are in gray. Middle: evolution of ΔBICLQ. The red curve represents the value calculated using Equation (6), while the blue curve depicts the quasi-analytic estimate of B. Jackson et al. (2023), which is the trajectory ΔBIC would be expected to take with observations at these epochs if the best-fit ﹩\dot{P}﹩ corresponded to real orbital decay. Both are accompanied by shaded regions indicating their expected 1σ variations (Equation (7)). The calculation begins only after three data points are available, reflecting the parameter fitting requirements of the quadratic model. Bottom: final observed ΔBICLQ (red line, calculated using all data points; see right end of red curve in middle panel) compared to the final observed ΔBICLQ that results after omitting each individual data point.
Paper: Doomed Worlds. II. Reassessing Suggestions of Orbital Decay for TrES-5 b
Authors: Marvin Rothmeier, Elisabeth R. Adams, Karsten Schindler, André Beck, Brian Jackson, Jeffrey P. Morgenthaler, Amanda A. Sickafoose, Malia Barker, Luigi Mancini, John Southworth, Daniel Evans, Alfred Krabbe
Figure caption: Lomb–Scargle periodograms (N. R. Lomb 1976; J. D. Scargle 1982) for all 280 midtimes used in this work (top) and for a subset of midtimes derived solely from TESS observations (bottom). The full dataset exhibits much higher levels of noise, with one signal (at 5.2 days) above a nominal 0.1% FAP. This peak, however, has only a marginal (2σ) detection in amplitude and is not seen using just the TESS data. Green dashed vertical lines highlight locally significant peaks, none of which are consistent between the full dataset and the TESS subset. The TESS data also do not evince any significant periods with an FAP less than 70%.
Paper: Doomed Worlds. II. Reassessing Suggestions of Orbital Decay for TrES-5 b
Authors: Marvin Rothmeier, Elisabeth R. Adams, Karsten Schindler, André Beck, Brian Jackson, Jeffrey P. Morgenthaler, Amanda A. Sickafoose, Malia Barker, Luigi Mancini, John Southworth, Daniel Evans, Alfred Krabbe
Figure caption: Left: joint-fit transit model of 14 new ground-based observations, as numbered in Table 3. Right: residuals from the model fit to each light curve. Transits and models were normalized to 1 for out-of-transit flux and then offset by 0.05 for display.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: The fractions fesc (blue), fhit (magenta), and fion (red) as a function of Mercury’s TAA. The solid lines include radiation pressure; radiation pressure is turned off for the dashed lines. The black dotted line indicates aphelion. (a) Na atoms are ejected isotropically from Mercury at 2 km s−1. (b) Na atoms are ejected isotropically at 4 km s−1. (c) Source is a 1200 K Maxwellian flux distribution isotropic on Mercury’s dayside. (d) Source is a 3500 K Maxwellian flux distribution centered on Mercury’s dawn equatorial point. The y-axes in panels (a) and (c) have gaps to highlight the behavior of the curves at values near zero and one.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: Trajectories of Na atoms ejected isotropically in the equatorial plane from Mercury’s dayside. Top row: TAA = 0°. Middle row: TAA = 90°. Bottom row: TAA = 290°. Left pair of panels: v0 = 2 km s−1. Right pair of panels: v0 = 4 km s−1. For each pair of panels, the left panel shows escaping trajectories and the right shows bound trajectories. Escaping trajectories that cross the SML are shown in black and those that do not cross the SML are shown in red. Blue trajectories begin and end on the dayside. Magenta trajectories begin on the dayside and end on the nightside.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: (a) Radiation acceleration (ar) for Na (red), Mg (magenta), and Ca (blue) as a function of radial velocity relative to the Sun (vρ⊙) at a solar distance of 0.39 au. The dotted lines show ±10 km s−1, Mercury’s minimum and maximum radial velocity relative to the Sun. (b) ar of the same species as a function of Mercury’s true anomaly angle (TAA) for an atom at rest relative to Mercury. The scale on the left shows the magnitude of the ar near Mercury. The scale on the right shows for both (a) and (b) the ratio of the radiation acceleration to the surface gravitational acceleration.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: (a) The photoionization lifetime τion (black), and mean residence times τesc (blue) and τhit (magenta) for atoms to reach escape speed or return to the surface, respectively, for atoms ejected from the surface at 4 km s−1. (b) Fractions of atoms along escaping trajectories that reach escape speed (blue) and along bound trajectories that return to the surface (magenta).
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: The fractions fesc (blue), fhit (magenta), and fion (red) as a function of Mercury’s TAA. Solid lines include radiation pressure; radiation pressure is not included in the models shown by the dashed lines. The dotted line indicates aphelion. (a) Ca atoms are ejected isotropically from Mercury at 2 km s−1. (b) Ca atoms are ejected isotropically at 4 km s−1. (c) Source is a 3500 K Maxwellian flux distribution centered on Mercury’s dawn equatorial point. (d) Source is a 50,000 K Maxwellian flux distribution centered on Mercury’s dawn equatorial point.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: (a) vρ⊙ of an atom initially at rest relative to Mercury as functions of TAA and time since the atom was launched from the surface. The black line represents t = 0 s, with lighter shades of red indicating longer travel times from 10 to 120 minutes. The only force acting on the atom is radiation pressure. (b) ar as functions of time and TAA acting on the same atom.
Paper: Seasonal Effects of the Changing Photon Scattering Rates on Mercury’s Exospheric Structure
Authors: Matthew H. Burger, Rosemary M. Killen, Ronald J. Vervack, Orenthal J. Tucker, Liam S. Morrissey, Daniel W. Savin
Figure caption: The Ca radiance as a function of altitude. (a) A 3500 K source is shown in red, a 50,000 K source in blue, and the sum of the two profiles is the solid black line. The dotted line indicates the approximate 1 kR detection limit for Ca by UVVS. (b) Same as (a) with a 5000 K source in place of a 3500 K source.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Ammonia abundance anomalies that fit the brightness temperature anomalies in Figure 8. The rightmost panel shows the (near-)simultaneous HST observations obtained within 2 hr of the flyby, and the panels to the left show slices in pressure, with the pressure indicated in the upper left corner. The ammonia variability peaks just below the clouds and decreases with depth. Most features extend down to about 6 bars, where the water is expected to condense out, with the anticylone in the northern hemisphere and the ammonia plume at the interface between the NEB and EZ the two notable exceptions. The dynamics in the SEB and EZ appear to be mostly located at altitudes above 2 bars, while the NEB shows significant variations down to 6 bars.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Zoom-in on the cloud and subcloud structure captured during the flyby focusing on the region with full coverage across all six Juno frequencies as shown by the outline. Panels are arranged left to right in order of decreasing pressure: from ∼2 bars at Juno C5, to ∼0.7 bars for the HST reflected light, down to ∼0.5 bars at Juno C6. Comparing Channel 5 with the VLA observations that probe the same depths, we can see that Juno passed just east of an extended cold region that appears to be part of the plume–hot spot system at the northern edge of the EZ. Furthermore, we can see that Juno flew over a particularly variable region in the NEB. The VLA observations also show that variability indeed peaks around 1 bar, with observations probing a bit higher in the atmosphere showing much less contrast (Ku and K bands).
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Retrieved ammonia abundance based on all zonally averaged Juno observables for PJ19 (see Equation (1)). We median-filtered this map for visualization purposes only to remove small-scale fluctuations.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Longitudinal brightness temperature anomalies in the Juno data after subtracting the zonal mean atmospheric brightness temperature at each frequency. The contours show temperature anomalies that are larger than 2 K for both cold and warm anomalies superimposed on the HST image to show correlation with the cloud tops. C6–C3 probe from the ammonia ice cloud down to the water cloud base, while C2 and C1 probe mostly below the cloud-forming regions.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: PJ19 observations compared to the mean atmosphere composed of the average of PJ1–12 (C. Moeckel et al. 2023). The PJ19 observations are used to build up the reference atmosphere for our analysis. The retrieved nadir brightness temperature is shown on the left-hand side, while the limb-darkening coefficient, p, is shown on the right-hand side. The colors correspond to the channels, with the channels probing deepest into the planet shown at the bottom of the figure (see Figure 1 for the pressures probed by the frequencies).
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: The left panel displays the residuals after subtracting the mean of the PJ19 observations. We remapped the structure to be centered around the minimum emission angle to highlight its dependence on the emission angle and longitude. We calculated the running median over 20° latitude to reveal the systematic brightening toward the limb, attributed to the increased synchrotron contribution. We chose a window size of 20° to ensure that it was twice as large as the typical extent of the zones and belts. In the right panel, the residual structure after removing the median is depicted. Although the majority of the atmospheric signal is attenuated, the structure at 15°N persists, indicating a deep-seated origin for this feature.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: 3D rendering of the longitudinal ammonia anomaly (Figure 9) in the Jovian tropics, where red regions are ammonia depletion causing warm brightness temperature anomalies, while blue regions correspond to ammonia enhancements. The relative shallow atmospheric variations in the SEB are shown in the upper left corner, the EZ in the center, and the NEB and the vortex at its northern boundary in the lower right corner. Processes that shape the atmosphere are highlighted, and approximate pressure levels are indicated.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Same as Figure 12, but for Channel 2.
Paper: Jupiter’s Tropical Atmosphere: Shallow Weather, Deep Plumes, and Vortices
Authors: Chris Moeckel, Imke de Pater, Robert, J. Sault, Bryan Butler
Figure caption: Same as Figure 12, but for Channel 3.