adsabs/AstroCLIMB huggingface dataset:
Paper: The Case for a New Frontiers–Class Uranus Orbiter: System Science at an Underexplored and Unique World with a Mid-scale Mission
Authors: Ian J. Cohen, Chloe Beddingfield, Robert Chancia, Gina DiBraccio, Matthew Hedman, Shannon MacKenzie, Barry Mauk, Kunio M. Sayanagi, Krista M. Soderlund, Elizabeth Turtle, Caitlin Ahrens, Christopher S. Arridge, Shawn M. Brooks, Emma Bunce, Sebastien Charnoz, Athena Coustenis, Robert A. Dillman, Soumyo Dutta, Leigh N. Fletcher, Rebecca Harbison, Ravit Helled, Richard Holme, Lauren Jozwiak, Yasumasa Kasaba, Peter Kollmann, Statia Luszcz-Cook, Kathleen Mandt, Olivier Mousis, Alessandro Mura, Go Murakami, Marzia Parisi, Abigail Rymer, Sabine Stanley, Katrin Stephan, Ronald J. Vervack, Jr., Michael H. Wong, Peter Wurz
Figure caption: Example of an instrument complement that would enable a broad, cross-disciplinary science return for a New Frontiers–class Uranus orbiter mission. White rows indicate a notional baseline payload that may be feasible given realistic cost and power constraints; gray rows provide additional high-impact instruments that could be included if resources and operations allow. Duty cycles and operations would be dependent on the mission and spacecraft designs.
Paper: The Case for a New Frontiers–Class Uranus Orbiter: System Science at an Underexplored and Unique World with a Mid-scale Mission
Authors: Ian J. Cohen, Chloe Beddingfield, Robert Chancia, Gina DiBraccio, Matthew Hedman, Shannon MacKenzie, Barry Mauk, Kunio M. Sayanagi, Krista M. Soderlund, Elizabeth Turtle, Caitlin Ahrens, Christopher S. Arridge, Shawn M. Brooks, Emma Bunce, Sebastien Charnoz, Athena Coustenis, Robert A. Dillman, Soumyo Dutta, Leigh N. Fletcher, Rebecca Harbison, Ravit Helled, Richard Holme, Lauren Jozwiak, Yasumasa Kasaba, Peter Kollmann, Statia Luszcz-Cook, Kathleen Mandt, Olivier Mousis, Alessandro Mura, Go Murakami, Marzia Parisi, Abigail Rymer, Sabine Stanley, Katrin Stephan, Ronald J. Vervack, Jr., Michael H. Wong, Peter Wurz
Figure caption: Voyager 2 images revealed surface features that have raised multiple mysteries regarding the composition, evolution, formation, and structure of the classical Uranian satellites. (Images from NASA/JPL)
Paper: The Case for a New Frontiers–Class Uranus Orbiter: System Science at an Underexplored and Unique World with a Mid-scale Mission
Authors: Ian J. Cohen, Chloe Beddingfield, Robert Chancia, Gina DiBraccio, Matthew Hedman, Shannon MacKenzie, Barry Mauk, Kunio M. Sayanagi, Krista M. Soderlund, Elizabeth Turtle, Caitlin Ahrens, Christopher S. Arridge, Shawn M. Brooks, Emma Bunce, Sebastien Charnoz, Athena Coustenis, Robert A. Dillman, Soumyo Dutta, Leigh N. Fletcher, Rebecca Harbison, Ravit Helled, Richard Holme, Lauren Jozwiak, Yasumasa Kasaba, Peter Kollmann, Statia Luszcz-Cook, Kathleen Mandt, Olivier Mousis, Alessandro Mura, Go Murakami, Marzia Parisi, Abigail Rymer, Sabine Stanley, Katrin Stephan, Ronald J. Vervack, Jr., Michael H. Wong, Peter Wurz
Figure caption: Remote observations of Uranus in the (a)–(b) near-infrared (from de Pater et al. 2015 and Sromovsky et al. (2015), respectively) have shown the Uranian atmosphere to be much more interesting than the (c) classic Voyager 2 image (NASA/JPL). It remains unclear whether (d) a three-layer overturning meridional circulation model accurately describes Uranus’s zonal and meridional circulation patterns (adapted from Sromovsky et al. 2014).
Paper: The Case for a New Frontiers–Class Uranus Orbiter: System Science at an Underexplored and Unique World with a Mid-scale Mission
Authors: Ian J. Cohen, Chloe Beddingfield, Robert Chancia, Gina DiBraccio, Matthew Hedman, Shannon MacKenzie, Barry Mauk, Kunio M. Sayanagi, Krista M. Soderlund, Elizabeth Turtle, Caitlin Ahrens, Christopher S. Arridge, Shawn M. Brooks, Emma Bunce, Sebastien Charnoz, Athena Coustenis, Robert A. Dillman, Soumyo Dutta, Leigh N. Fletcher, Rebecca Harbison, Ravit Helled, Richard Holme, Lauren Jozwiak, Yasumasa Kasaba, Peter Kollmann, Statia Luszcz-Cook, Kathleen Mandt, Olivier Mousis, Alessandro Mura, Go Murakami, Marzia Parisi, Abigail Rymer, Sabine Stanley, Katrin Stephan, Ronald J. Vervack, Jr., Michael H. Wong, Peter Wurz
Figure caption: It remains unclear why the Uranian ring–moon system shown here is so dynamically full and apparently haphazard.
Paper: The Case for a New Frontiers–Class Uranus Orbiter: System Science at an Underexplored and Unique World with a Mid-scale Mission
Authors: Ian J. Cohen, Chloe Beddingfield, Robert Chancia, Gina DiBraccio, Matthew Hedman, Shannon MacKenzie, Barry Mauk, Kunio M. Sayanagi, Krista M. Soderlund, Elizabeth Turtle, Caitlin Ahrens, Christopher S. Arridge, Shawn M. Brooks, Emma Bunce, Sebastien Charnoz, Athena Coustenis, Robert A. Dillman, Soumyo Dutta, Leigh N. Fletcher, Rebecca Harbison, Ravit Helled, Richard Holme, Lauren Jozwiak, Yasumasa Kasaba, Peter Kollmann, Statia Luszcz-Cook, Kathleen Mandt, Olivier Mousis, Alessandro Mura, Go Murakami, Marzia Parisi, Abigail Rymer, Sabine Stanley, Katrin Stephan, Ronald J. Vervack, Jr., Michael H. Wong, Peter Wurz
Figure caption: Mapping of the potential science objectives of a New Frontiers–class Uranus orbiter mission to different measurement types. This underscores the broad, cross-disciplinary science that can be achieved given that many instruments can provide observations relevant to multiple aspects of the science investigation.
Paper: Uranus’s and Neptune’s Stratospheric Water Abundance and Vertical Profile from Herschel-HIFI 
Authors: N. A. Teanby, P. G. J. Irwin, M. Sylvestre, C. A. Nixon, M. A. Cordiner
Figure caption: Generation of disk-averaged synthetic spectra for (a–d) Uranus and (e–h) Neptune. (a, e) Synthetic 1000 × 1000 pixel image covering the on- and off-disk regions, with lines of latitude (black lines spaced by 15°) and line-of-sight velocity (colors) assuming Helled et al. (2010) rotation rates and solid-body rotation. (b, f) Synthetic single-pixel radiance spectra for on-disk points with emission angles e = 0°, 60°, and 90° and limb spectra with tangent altitudes of 100, 200, and 300 km above the 1 bar pressure level. There is significant radiance emitted off the planet limbs, especially for the 556.936 GHz water emission line. (c, g) Radiance as a function of impact parameter x (offset from planet center) for water emission line center at 556.936 GHz and wing regions indicated in panels (b) and (f) with colored vertical bars. The dashed vertical line indicates a radius of 1 bar pressure level. At around ∼1000 km off the planet limb the emitted radiance becomes negligible. Grid spacing of synthetic spectra is indicated by Δx. (d, h) Composite line-to-continuum ratio spectra from combining contributions from 106 image pixels with Airy disk weighting.
Paper: Uranus’s and Neptune’s Stratospheric Water Abundance and Vertical Profile from Herschel-HIFI 
Authors: N. A. Teanby, P. G. J. Irwin, M. Sylvestre, C. A. Nixon, M. A. Cordiner
Figure caption: Herschel-HIFI water emission line disk-averaged HRS and WBS observations of (a) Uranus and (b) Neptune. DSB spectra have been converted to line-to-continuum ratio, with horizontal and vertical polarizations averaged together to give a single spectrum for each planet. HRS spectra have been binned at 0.6 MHz (0.3 MHz sample spacing) to increase signal-to-noise ratio. The error bar indicates mean 1σ uncertainty. HRS and WBS spectra are consistent to within errors. Insets show orientation of Uranus and Neptune during the observations with a 1″ scale bar. Water emission lines are broadened by Doppler shift induced by planetary rotation. The data behind this figure are available.(The data used to create this figure are available.)
Paper: Uranus’s and Neptune’s Stratospheric Water Abundance and Vertical Profile from Herschel-HIFI 
Authors: N. A. Teanby, P. G. J. Irwin, M. Sylvestre, C. A. Nixon, M. A. Cordiner
Figure caption: Fitted water profiles to observed HIFI HRS line-to-continuum spectra for (a, b) Uranus and (c, d) Neptune using the nominal temperature profile. (a, c) The black line shows observed spectra with 1σ error envelope in gray. Colored lines in panels (a) and (c) correspond to synthetic spectra generated with best-fitting water profiles shown in panels (b) and (d). MP17 = Moses & Poppe (2017) profiles; L19 = Lara et al. (2019) profiles. Profiles shown with solid lines provide excellent fits to observed spectra that are indistinguishable from the best-fitting profile at 4σ significance, whereas dashed lines produce significantly worse fits and can be rejected with 4σ significance. For Uranus, all profiles fit observations well except the 1 mbar step. For Neptune, the 0.3 and 0.6 mbar step and scaled Moses & Poppe (2017) profiles produce significantly better fits (Table 2).
Paper: Uranus’s and Neptune’s Stratospheric Water Abundance and Vertical Profile from Herschel-HIFI 
Authors: N. A. Teanby, P. G. J. Irwin, M. Sylvestre, C. A. Nixon, M. A. Cordiner
Figure caption: Uranus and Neptune atmospheric temperature profiles, including estimated uncertainties. The nominal profile for each planet is indicated by the solid line, whereas hot and cold profiles are indicated by extremes of the uncertainty envelopes. Note that for Uranus the low-temperature envelope includes upper atmosphere cooling (Melin et al. 2011; Trafton et al. 2021) in addition to measurement uncertainties. Black lines indicate temperature at 100% relative humidity for 1, 10, and 100 ppb water vapor. For colder atmospheric temperature, SVP is exceeded and condensation occurs. On Uranus the condensation level is ∼0.03 mbar, and on Neptune it is ∼1 mbar because of the warmer stratosphere. The data behind this figure are available.(The data used to create this figure are available.)
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Map of spatial coverage of the data sets used in this study. The black dotted line shows the useful spatial coverage of the VLT/SPHERE observation. The colored outlines show the total area observed in each NIMS data set (see Table 2). The shaded orange region shows the area of the “E6” observation where NIMS has full spectral coverage of the SPHERE wavelength range, which is used for full spectral modeling. Regions with extreme emission and incidence angles (>75°) have large residual photometric errors and so are not used in this study or shown on this map. The background visible-light reference image of Europa is from Becker (2013). 0° west is the sub-Jovian longitude, and 180° west is the anti-Jovian longitude.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Image-cleaning process for IFS data. The top images show observations of Europa at 1.37 μm, the wavelength where the striping pattern is the worst. The bottom images show the observations’ corresponding Fourier transform magnitudes on a logarithmic scale. The frequencies that cause the striping pattern in the raw image (the bright dots away from the center of the Fourier transform) are set to zero to remove the artificial pattern. The image is then despiked to remove any extreme bright or dark pixels, which are replaced by interpolated values.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Mask used to remove unwanted frequencies from the Fourier transform of IFS data. The mask is multiplied with the Fourier transform (see Equation (1)), so white areas (=1) are kept and black areas (=0) are removed.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Normalized 1.50 μm/1.36  μm spectral ratio for SPHERE and NIMS observations. The NIMS data are a combination of the data sets in Table 2; in regions where the observations overlap, the median reflectance value is used. Blue areas in the map indicate stronger absorption at 1.50 μm, generally implying a higher water-ice abundance, and red areas indicate reduced water-ice abundance. The graph on the left shows reflectance spectra for a range of water-ice grain sizes (darker lines indicate smaller ice grains; see Figure 8) normalized to unity at 1.36 μm. The choice of ratio wavelengths measures the full relative depth of the 1.5 μm absorption and produces a map ratio that is mainly affected by ice abundance (rather than grain size).
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Summary of different photometric models (top) and images of Europa at 1.65 μm with the photometric correction applied (bottom). The subsolar point is marked by the blue circle, the subobserver point is marked by the yellow cross, and the outline of the modeled disk is given by the large yellow circle. This Europa observation has a solar phase angle of 9.7°, and the final photometric model (panel (d)) combines the Oren−Nayar model (with surface roughness σ = 33°) and a diffraction model (with r airy = 10 pixels).
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Fit result for spectra from Powys Regio and Dyfed Regio. The left column shows the observed spectrum (red) and the “family” of MCMC fitted spectra (black). The right column shows the violin plots for the fitted posterior abundance distributions, where the shaded region shows the full posterior distribution of abundance values. The horizontal width of the shaded region shows the shape of the posterior distribution (where wider areas are more likely and narrower areas are less likely), and the vertical height of the shaded region shows the full range of simulated abundance values. The black dot shows the median best-estimate abundance, and the black line gives the 1σ uncertainty around this estimate. Numerical values are provided in the Appendix.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Hydrated sulfuric acid spatial distribution for the SPHERE and NIMS data sets. The values shown here are the best estimates that are calculated as the median of the posterior abundance distribution for each location. The acid abundance is highest toward the trailing apex (270° west, 0° north) and lower toward the leading hemisphere and high latitudes. The slight increase in acid abundance toward the edge of the SPHERE data set is likely to be caused by residual errors from the photometric correction. The typical uncertainty on the abundance values is ±10 percentage points for SPHERE and ±7 percentage points for NIMS.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Corner plot showing relationship between endmember percentage abundances for the SPHERE fit in Powys Regio. The shaded 2D histograms give the posterior abundance distribution, with brighter colors indicating a higher density. In low-density regions toward the edge of the distribution, individual points of the distribution are plotted. For clarity, some endmembers have been combined. Circular distributions imply no strong correlation between the abundance distributions of the two endmembers, whereas skewed distributions imply a correlation between the abundances of those endmembers.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: IRDIS two-color observation of Europa (left), and simulated visible-light reference image of Europa from Becker (2013; right). The two-color IRDIS observation is produced using the K1 filter at 2.1 μm (filter width 0.051 μm), shown in yellow, and the K2 filter at 2.251 μm (width 0.055 μm), shown in blue. Water ice has a broad absorption band around 2 μm, so the blue areas are icy and yellow areas are dominated by non-icy species.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Example endmembers used for spectral modeling. The shaded areas show the spectral range covered by the SPHERE IFS instrument and the two IRDIS filters, and the dots show the reflectance in the IFS spectral bins. The NIMS spectra used in this study cover the whole spectral range shown in this figure.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Water-ice spatial distributions for SPHERE (top) and NIMS (bottom). The total water-ice abundance (left) is lowest toward the trailing apex and highest at high latitudes, where abundances are >50%. The grain size column (right) shows the ice size endmember with the highest individual abundance. The ice grain size varies with longitude, with larger (300 μm–1 mm) grains more abundant on the trailing hemisphere and smaller grains (100–300 μm) more abundant on the leading hemisphere.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Brightness curves for different photometric models of Europa with a solar phase angle of 9.7°. The final photometric model (“O-N + diffraction”) has surface roughness σ = 33° and r airy = 10 pixels.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Spatial distribution of sulfate salt abundances. The top rows show best-estimate abundances (median of posterior distribution), and the bottom rows show the 1σ lower bound of the posterior abundance distributions. Lower bounds close to zero suggest that the specific endmember cannot be confidently detected. Abundance values less than 0.5% are shown in black. Note the different abundance scale for each salt species.
Paper: Compositional Mapping of Europa Using MCMC Modeling of Near-IR VLT/SPHERE and Galileo/NIMS Observations
Authors: Oliver King, Leigh N. Fletcher, Nicolas Ligier
Figure caption: Spatial distribution of chlorine-bearing salt abundances. As with Figure 13, the top rows show the best-estimate abundances, and the bottom rows show 1σ lower bounds. Abundance values less than 0.5% are shown in black. Note the different abundance scale for each salt species.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Contour plots of the zonal-mean T (K), U (m s−1), and PV (107 m2 s−1K kg−1) for (a, c, e; left column) latitude vs. time on a fixed pressure surface (0.1 hPa) and (b, d, f; right column) pressure vs. time for averages over a latitude band (70°–90°S for T and PV and 40°–60°S for U), for the whole year. Dotted lines represent the timing of solstices, dashed lines represent the timing of equinoxes, and the solid line in panel b depicts the stratopause, which lies above the plotted region in southern summer.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Zonally averaged temperature from CIRS (A–C) and TitanWRF (D–F) at southern fall equinox (left), southern midfall (middle), and southern winter solstice (right). Values are only shown here and in the following figures for the 10 hPa–0.001 hPa range to focus on behavior in the stratosphere and mesosphere.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Zonally averaged zonal wind from CIRS (A–C) and TitanWRF (D–F) at southern fall equinox (left), southern midfall (middle), and southern winter solstice (right). Missing data in CIRS observations are due to the breakdown of gradient wind balance near the equator.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: TitanWRF pairs of T (K) contours and MMC (kg m−1 s−1) color shading (positive values indicate clockwise rotation) shown from southern fall equinox to late southern winter.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Annual evolution of the polar temperature (70°–90° average) for the northern (blue) and southern (red) hemispheres, at 0.1 hPa from a multiyear extension of the TitanWRF simulation (additional four years). Thick lines represent the four-year average; the shaded region (SH) and thin blue lines (NH) represent the maximum and minimum temperatures over the four years.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Annual evolution of polar temperature (70°–90° average) for the northern (blue) and southern (red) hemispheres, at (a) 0.1, (b) 1, and (c) 10 hPa. TitanWRF is shown with solid curves and Cassini CIRS observations with crosses.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Zonally averaged absolute value of the scaled Ertel potential vorticity (107 m2 s−1K kg−1) from CIRS (A–C) and TitanWRF (D–F) at southern fall equinox (left), southern midfall (middle), and southern winter solstice (right). EPV values are first calculated on isentropic surfaces and then interpolated to pressure surfaces that can lead to the appearance of regions of undefined data in both observations and model output.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Annual evolution of zonally averaged U (m s−1) averaged between 40°–60° north (blue) and south (red) (a), and PV (107 m2 s−1K kg−1) averaged between 70°–90° north (blue) and south (red) (b) shown for a full year at the 0.1 hPa pressure level. TitanWRF is shown with solid curves and Cassini CIRS observations with crosses.
Paper: Winter Weakening of Titan's Stratospheric Polar Vortices
Authors: J. Shultis, D. W. Waugh, A. D. Toigo, C. E. Newman, N. A. Teanby, J. Sharkey
Figure caption: Vertical velocity (cm s−1, color fill) and temperature (K, contour lines) as a function of solar longitude and latitude on a 0.1 hPa constant pressure surface from the TitanWRF simulation. The thick black line represents the location of the zero value of the stream function at this pressure.
Paper: Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Authors: David J. Stevenson, Peter Bodenheimer, Jack J. Lissauer, Gennaro D'Angelo
Figure caption: Planet’s structure and composition at the end of Phase IV, t = 3.14 × 106 yr. The structure variables (P, ρ, T) and the heavy-element mass fraction (Z) are displayed on the left, and the interior distributions of silicates, water, and H–He are shown on the right. The core region (as defined herein) is also indicated.