adsabs/AstroCLIMB huggingface dataset:
Paper: Contrast Reversal and Emergent Features on Pluto
Authors: Jason D. Hofgartner, Bonnie J. Buratti, Will M. Grundy, S. Alan Stern, Anne J. Verbiscer
Figure caption: Cloud or surface coating hypothesis for Pluto’s CEs. CE corresponds to the example CE in Figures 2 (largest and easternmost) and 6, and SP2 corresponds to a nearby Sputnik Planitia locality. The 95% statistical confidence intervals are smaller than the filled circles, and the two P_LORRI (19° solar phase angle) measurements of each locality are barely to not distinguishable. Hapke+haze photometric functions are shown using SP2 best-fit parameters and P_LORRI and P_HiPhase_HiRes incidence and azimuth angles (both angles are approximately constant; Table 2). Hapke+cloud+haze photometric functions are shown using best-fit SP2 surface/shallow subsurface and global haze and CE cloud parameters and P_LORRI and P_HiPhase_HiRes incidence and azimuth angles. Best-fit parameters for each locality, however, were determined using angles specific to each measurement. Optically thin scattering between the surface and global haze, by a cloud or surface coating, satisfactorily fits differences of an example CE on Pluto from its surroundings.
Paper: Spectral Trends across the Rings and Inner Moons of Uranus and Neptune from JWST NIRCam Images
Authors: M. M. Hedman, I. de Pater, R. J. Cartwright, M. El Moutamid, R. DeColibus, M. R. Showalter, M. S. Tiscareno, N. Rowe-Gurney, M. T. Roman, L. N. Fletcher, H. B. Hammel
Figure caption: Comparisons of the new JWST estimates of the reflectances of Miranda, Puck, and Proteus with previously published values. Note that in order to avoid complications associated with accounting for the moons’ opposition surges, these plots show reflectance estimates derived from observations taken at phase angles comparable to those observed by JWST. More specifically, for Uranus the plotted data from E. Karkoschka (2001a), J. M. Bauer et al. (2002), and R. J. Cartwright et al. (2020b) were all obtained at phase angles between 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9. These values are therefore all close to the phase angles of 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩8–2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9 observed by JWST. (Note that we only plot the UKIRT data from J. M. Bauer et al. 2002 because these had the tightest error bars, and the published brightness estimate from R. J. Cartwright et al.2020b includes a phase correction that we removed in this plot.) The Uranus data derived from C. Dumas et al. (2003), S. G. Gibbard et al. (2005), and S. Paradis et al. (2023) were obtained at phase angles between 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩6 and 2°, which are a bit lower than those observed by JWST. We chose not to correct these data for phase angle variations using the E. Karkoschka (2001a) formulae because there is not an obvious strong trend with phase angle among these observations. Similarly, the data for Proteus from C. Dumas et al. (2002, 2003), E. Molter et al. (2019), and M. Helfenbein et al. (2024) were obtained at phase angles between 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7 and 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9, which are generally comparable to the phase angle of 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩8 observed by JWST. Again, there is no obvious trend over the limited observed range of phase angles that would motivate a phase correction for these data.
Paper: Spectral Trends across the Rings and Inner Moons of Uranus and Neptune from JWST NIRCam Images
Authors: M. M. Hedman, I. de Pater, R. J. Cartwright, M. El Moutamid, R. DeColibus, M. R. Showalter, M. S. Tiscareno, N. Rowe-Gurney, M. T. Roman, L. N. Fletcher, H. B. Hammel
Figure caption: Plots of various spectral parameters of the rings and inner moons as functions of distance from their host planet. The rings and moons of Uranus are shown in green and the rings and moons of Neptune are shown in the blue. The top panel shows the spectral slope between 1.4 and 2.1 μm, which is defined such that blue slopes are positive and the red slopes are negative. The middle panel shows the depth of the 3 μm band, with larger values indicating a deeper band. Finally, the bottom panel shows the continuum slope across the two regions on either sides of the 3 μm band. The green and blue points just use the brightness data at 2.1 μm and 4.6 μm, respectively, while the lime points use the weighted average brightness of all three wavelengths in both regions.
Paper: Spectral Trends across the Rings and Inner Moons of Uranus and Neptune from JWST NIRCam Images
Authors: M. M. Hedman, I. de Pater, R. J. Cartwright, M. El Moutamid, R. DeColibus, M. R. Showalter, M. S. Tiscareno, N. Rowe-Gurney, M. T. Roman, L. N. Fletcher, H. B. Hammel
Figure caption: JWST NIRCam image showing Uranus’ rings and small moons. This is a cropped version of image jw02739011001_02105_00003_nrcb1_i2d.fits, which was obtained using the F140M filter and calibrated using the standard pipeline (H. Bushouse et al. 2025). All of the rings and moons considered in this paper are labeled and visible in this image. Unmarked bright spots are either background stars or instrumental artifacts. Note the moons appear smeared due to their motion over the course of the integration. Also note that the dusty μ and ν rings are just barely visible in this image because it has been stretched to better show the moons.
Paper: Spectral Trends across the Rings and Inner Moons of Uranus and Neptune from JWST NIRCam Images
Authors: M. M. Hedman, I. de Pater, R. J. Cartwright, M. El Moutamid, R. DeColibus, M. R. Showalter, M. S. Tiscareno, N. Rowe-Gurney, M. T. Roman, L. N. Fletcher, H. B. Hammel
Figure caption: Average background-subtracted brightness profiles of Uranus’ main rings derived from the NIRCam images. Different colored profiles correspond to data from different NIRCam filters, and the locations of the nine main rings and the dusty ζ ring are marked. The faint dotted and dashed lines show the versions of the profiles used to estimate the brightnesses of the ϵ and 6−δ rings, respectively. Note that these separate profiles deviate from the observed profiles most noticeably in the transition between the ϵ and δ rings.
Paper: Spectral Trends across the Rings and Inner Moons of Uranus and Neptune from JWST NIRCam Images
Authors: M. M. Hedman, I. de Pater, R. J. Cartwright, M. El Moutamid, R. DeColibus, M. R. Showalter, M. S. Tiscareno, N. Rowe-Gurney, M. T. Roman, L. N. Fletcher, H. B. Hammel
Figure caption: JWST NIRCam image showing Neptune’s rings and small moons. This is a cropped version of image jw02739004001_02105_00003_nrcb1_i2d.fits, which was obtained using the F140M filter and calibrated using the standard pipeline (H. Bushouse et al. 2025). All of the rings and moons considered in this paper are labeled and visible in this image. Unmarked bright spots are either background stars or instrumental artifacts. Note the moons appear smeared due to their motion over the course of the integration.
Paper: Spectral Trends across the Rings and Inner Moons of Uranus and Neptune from JWST NIRCam Images
Authors: M. M. Hedman, I. de Pater, R. J. Cartwright, M. El Moutamid, R. DeColibus, M. R. Showalter, M. S. Tiscareno, N. Rowe-Gurney, M. T. Roman, L. N. Fletcher, H. B. Hammel
Figure caption: Average background-subtracted brightness profiles of Neptune’s rings derived from the NIRCam images. Different colored profiles correspond to data from the different NIRCam filters, and the various rings are marked. The faint dotted and dashed lines show the versions of the profiles used to estimate the brightnesses of the Adams ring and the combined Le Verrier, Lassel, and Arago rings, respectively. Note that these separate profiles deviate from the observed profiles most noticeably in the transition between the Adams and Arago rings.
Paper: Spectral Trends across the Rings and Inner Moons of Uranus and Neptune from JWST NIRCam Images
Authors: M. M. Hedman, I. de Pater, R. J. Cartwright, M. El Moutamid, R. DeColibus, M. R. Showalter, M. S. Tiscareno, N. Rowe-Gurney, M. T. Roman, L. N. Fletcher, H. B. Hammel
Figure caption: Normalized spectra of the rings and inner moons of Uranus and Neptune. All spectra are normalized to have an average value of one between 1.4 and 2.1 μm in order to facilitate comparisons among the different spectra. Note that each data point corresponds to the average brightness over a range of wavelengths indicated by the vertical bands (see Table 2).
Paper: Spectral Trends across the Rings and Inner Moons of Uranus and Neptune from JWST NIRCam Images
Authors: M. M. Hedman, I. de Pater, R. J. Cartwright, M. El Moutamid, R. DeColibus, M. R. Showalter, M. S. Tiscareno, N. Rowe-Gurney, M. T. Roman, L. N. Fletcher, H. B. Hammel
Figure caption: Normalized spectra of the rings and inner moons of Uranus and Neptune. These spectra are again all normalized to have an average value of one between 1.4 and 2.1 μm, but have also been offset vertically to illustrate trends with distance from the two planets.
Paper: X-Ray-induced Photochemistry of Hydrocarbons: Implications for the Formation of Organic Haze in (Exo)Planetary Atmospheres
Authors: Salma Bejaoui, David Dubois, Slavomir Nemsak, Farid Salama
Figure caption: Ternary phase diagram of amorphous carbons as a function of hydrogen fraction and carbon bonding hybridization, adapted from W. Jacob & W. Möller (1993), J. E. Chiar et al. (2013). The gray-shaded region marks conditions where no stable films can be deposited. Characteristic regions of hydrocarbon polymers, a-C:H, sputtered a-C:H, tetrahedral hydrocarbon (ta-C:H), soot precursors, and soot are illustrated (W. Jacob & W. Möller 1993; J. E. Chiar et al. 2013; A. Baldelli et al. 2020). The three data points represent the structural characteristics of organics produced in this study from X-ray irradiated-CH4 (cyan), C2H4 (blue), and C2H6 (green).
Paper: X-Ray-induced Photochemistry of Hydrocarbons: Implications for the Formation of Organic Haze in (Exo)Planetary Atmospheres
Authors: Salma Bejaoui, David Dubois, Slavomir Nemsak, Farid Salama
Figure caption: XPS of methane (a), ethylene (b), and ethane (c) after 2 hr of the synchrotron broadband beam irradiation.
Paper: X-Ray-induced Photochemistry of Hydrocarbons: Implications for the Formation of Organic Haze in (Exo)Planetary Atmospheres
Authors: Salma Bejaoui, David Dubois, Slavomir Nemsak, Farid Salama
Figure caption: (a) Ambient pressure photoemission spectroscopy endstation (APPES) in the Advanced Light Source beamline 9.3.2 at Lawrence Berkeley National Laboratory, (b) monochromated spectrum of the X-rays at beamline 9.3.2 and the mass photoabsorption coefficients of CH4, C2H4, and C2H6 as a function of photon energy (A. V. Naumkin et al. 2000). (c) Schematic representation of the APPES facility used in the current study: a broadband beam parallel to the Si substrate is used for the irradiation experiment while a beam energy at 430 eV with 20∘ incidence is used for the spectroscopy experiment. (d) Photo of the Si substrate mounted on a precision stage with adjustments in x, y, z, and θ directions.
Paper: X-Ray-induced Photochemistry of Hydrocarbons: Implications for the Formation of Organic Haze in (Exo)Planetary Atmospheres
Authors: Salma Bejaoui, David Dubois, Slavomir Nemsak, Farid Salama
Figure caption: Variation of the percentages of C1s sp2 and sp3 band areas relative to the entire C1s band as a function of the irradiation time (dose) for methane, ethylene, and ethane irradiated with the broadband beam.
Paper: X-Ray-induced Photochemistry of Hydrocarbons: Implications for the Formation of Organic Haze in (Exo)Planetary Atmospheres
Authors: Salma Bejaoui, David Dubois, Slavomir Nemsak, Farid Salama
Figure caption: SIMS composition depth profile of C2H4 and C2H6 photoproducts deposited on Si substrates. Filled circles represent C2H6 photoproducts, while open circles correspond to C2H4 photoproducts. The profiles show the depth distribution of Si (yellow), C (red), H (blue), and O (green), measured using a primary ion beam energy of 1 keV.
Paper: X-Ray-induced Photochemistry of Hydrocarbons: Implications for the Formation of Organic Haze in (Exo)Planetary Atmospheres
Authors: Salma Bejaoui, David Dubois, Slavomir Nemsak, Farid Salama
Figure caption: XPS C1s spectra from control experiments. (a) “Gas + no irradiation” shows the C1s spectra after exposing the substrate to 100 mTorr of C2H4 for 2 hr without irradiation. (b) “Irradiation + no gas” shows the evolution of C1s spectra after irradiating the evacuated chamber (10−9 Torr) with the broadband beam for 2 hr. (c) “Gas + irradiation” shows the evolution of C1s spectra when irradiating 100 mTorr of C2H4 for 2 hr.
Paper: X-Ray-induced Photochemistry of Hydrocarbons: Implications for the Formation of Organic Haze in (Exo)Planetary Atmospheres
Authors: Salma Bejaoui, David Dubois, Slavomir Nemsak, Farid Salama
Figure caption: Variation of the C1s sp2 and sp3 band areas as a function of the irradiation time (dose) for methane, ethylene, and ethane irradiated with a broadband beam.
Paper: Survivability of Amino Acids in Lunar Soil
Authors: Li Hsia Yeo, Hannah McLain, Sophia Westerkamp, Danielle Simkus, Jennifer Holt, Jason McLain
Figure caption: Survivability of amino acids buried at different depths in lunar soil. Amino acids are sorted by functional group and displayed with increasing molecular weight within each group. Amino acids buried as little as 8 mm below the surface have an average of ∼95% survival rate. Each experimental trial was conducted in triplicate with error bars reflecting standard error.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Spectra of water ice of the four grain-size bins used in this study. Top: solid lines represent pure grain-size bins. Bottom: dashed lines represent 50%/50% by volume mixtures of several combinations of water ice grain sizes. Notice that there is minimal discrepancy between the grain-size mixtures, and it may therefore be challenging to discriminate visually without spectral mixture analysis. Measured temperatures for each sample are provided in the figure legend as well as in Table 1.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Glove box setup for the experiments conducted in this study. The LN2 dewar and gold standard are mounted on a linear stage that allows for the gold and sample to move into and out of the field of view of the spectrometer fiber-optic for measurements. Bottom-left inset: photograph of 50% <63 μm + 50% 250–500 μm water ice.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Block diagram of the CRONOS laboratory setup; dimensions are not necessarily to scale. All materials and equipment were given at least 30 minutes in the antechamber before moving into the main chamber, to ensure no atmosphere was exchanged between the two areas.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: 50%/50% vol. mixtures of epsomite and water ice for different grain aliquots, where “fine” is <63 μm, “small” is 63–250 μm, “medium” is 250–500 μm, and “large” is >500 μm. The reader is referred to Figure 3 of pure water ice as a reference to see the influence that water ice has on the mixed spectra shown in this figure.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: 50%/50% vol. mixtures of halite and water ice for different grain aliquots, where “fine” is <63 μm, “small” is 63–250 μm, “medium” is 250–500 μm, and “large” is >500 μm. The reader is referred to Figure 3 of pure water ice as a reference to see the influence that water ice has on the mixed spectra shown in this figure.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Spectra of epsomite of the four grain-size bins used in this study, acquired both under ambient (dashed lines) and cryogenic (solid lines) conditions. Fine structure in the spectral absorption features in the cryogenic spectra is expected and is characteristic of colder temperatures. Measured temperatures for each sample are provided in Table 1.
Paper: The Near-infrared Spectral Characteristics of Water Ice, Epsomite, and Halite Mixtures Relevant to Europa
Authors: Jodi R. Berdis, Carlie Wagoner, Akemi Takeuchi, Karl Hibbitts
Figure caption: Spectra of halite of the four grain-size bins used in this study, acquired both under ambient (dashed lines) and cryogenic (solid lines) conditions. Fine structure in the spectral absorption features in the cryogenic spectra is expected and is characteristic of colder temperatures. Measured temperatures for each sample are provided in Table 1.
Paper: Spectroscopy of the Hamburg Meteorite, Michigan H4
Authors: M. Darby Dyar, Laura B. Breitenfeld, Melissa D. Lane, Timothy Glotch, Roger Clark, Neil Pearson, Elizabeth C. Sklute, Molly C. McCanta, Amanda J. Hendrix, Brandon Weller, Morgan Schaller, Alexander Kling, Dylan McDougall
Figure caption: The blue spectrum is the measured sample, while the orange spectrum is the model fit (shown with rms value in Table 2). Mineral spectra used in the model fit are shown below the meteorite. The green spectrum is synthetic olivine (Fo80; M. D. Lane et al. 2011), dark turquoise is enstatite, light blue is pigeonite, and purple is albite. Mineral spectra are offset for clarity. Vertical lines are drawn at several wavelengths to emphasize features in the meteorite that are due to Fo80 olivine.
Paper: Spectroscopy of the Hamburg Meteorite, Michigan H4
Authors: M. Darby Dyar, Laura B. Breitenfeld, Melissa D. Lane, Timothy Glotch, Roger Clark, Neil Pearson, Elizabeth C. Sklute, Molly C. McCanta, Amanda J. Hendrix, Brandon Weller, Morgan Schaller, Alexander Kling, Dylan McDougall
Figure caption: (Top) Spectrum of the meteorite slab showing characteristic features. Data are combined at 2.5 μm, with shortward being from ASD and longward being Agilent spectra. (Bottom) Reflectance model fit (red line) to the reflectance spectrum of a Hamburg meteorite slab (black line). Abundances are given in wt%.
Paper: Spectroscopy of the Hamburg Meteorite, Michigan H4
Authors: M. Darby Dyar, Laura B. Breitenfeld, Melissa D. Lane, Timothy Glotch, Roger Clark, Neil Pearson, Elizabeth C. Sklute, Molly C. McCanta, Amanda J. Hendrix, Brandon Weller, Morgan Schaller, Alexander Kling, Dylan McDougall
Figure caption: Thermal emissivity spectra of the Hamburg meteorite (Michigan). The interior measurements are shown in blue (ambient pressure) and turquoise (vacuum), and the exterior fusion crust (vacuum) is shown in black.
Paper: Spectroscopy of the Hamburg Meteorite, Michigan H4
Authors: M. Darby Dyar, Laura B. Breitenfeld, Melissa D. Lane, Timothy Glotch, Roger Clark, Neil Pearson, Elizabeth C. Sklute, Molly C. McCanta, Amanda J. Hendrix, Brandon Weller, Morgan Schaller, Alexander Kling, Dylan McDougall
Figure caption: (Top) Sample cut for this study. Photos by B.W. Some crumbles were produced while slabbing this sample, and those loose pieces were handpicked into aliquots from the crust vs. the interior for use in spectroscopy. (Bottom) Chip loaned by Mike Farmer for VNIR studies.
Paper: Differentiation, the Exception, Not the Rule: Evidence for Full Miscibility in Sub-Neptune Interiors
Authors: Edward D. Young, Aaron Werlen, Sarah P. Marcum, Lars Stixrude, Cornelis P. Dullemond
Figure caption: Isobaric phase diagram for the MgSiO3–H2 binary system as determined by L. Stixrude & T. Gilmore (2025). The one- and two-phase regions outside and inside of the binodal are indicated. A region of metastable compositions for two coexisting phases exists between the binodal and spinodal curves. The compositions of two stable phases at approximately 3600 K are shown by way of example with a dashed tie line connecting them.
Paper: Differentiation, the Exception, Not the Rule: Evidence for Full Miscibility in Sub-Neptune Interiors
Authors: Edward D. Young, Aaron Werlen, Sarah P. Marcum, Lars Stixrude, Cornelis P. Dullemond
Figure caption: Gibbs free-energy-of-mixing surface, ﹩{\hat{G}}_{{\rm{mix}}}﹩, in the ternary system MgSiO3–Fe–H2 for T = 3500 K and P = 4 GPa. The heavy black lines show the spinodals denoting the regions of spontaneous decomposition into two phases. Points comprising the binodals are shown in blue connected by tie lines. The blue binodal points define the coexistence curves. Between the binodals and spinodals lies the region of metastability for two phases.
Paper: Differentiation, the Exception, Not the Rule: Evidence for Full Miscibility in Sub-Neptune Interiors
Authors: Edward D. Young, Aaron Werlen, Sarah P. Marcum, Lars Stixrude, Cornelis P. Dullemond
Figure caption: Images of initial and final conditions for the H2–MgSiO3 system illustrating complete miscibility at 4000 K and 3.5 GPa. The initial condition is composed of MgSiO3 melt overlaid by H2 gas. The final state is after 13.5 ps of model time. See Appendix B for details.
Paper: Differentiation, the Exception, Not the Rule: Evidence for Full Miscibility in Sub-Neptune Interiors
Authors: Edward D. Young, Aaron Werlen, Sarah P. Marcum, Lars Stixrude, Cornelis P. Dullemond
Figure caption: Images of initial and final conditions for the MgSiO3–H2 system illustrating immiscibility at 3000 K and 2.5 GPa. The initial condition is composed of MgSiO3 melt overlaid by H2 gas. The final state is after 16.5 ps of model time. Example SiO and H2O molecules in the gas phase that persist for significant intervals of model time are labeled.
Paper: Differentiation, the Exception, Not the Rule: Evidence for Full Miscibility in Sub-Neptune Interiors
Authors: Edward D. Young, Aaron Werlen, Sarah P. Marcum, Lars Stixrude, Cornelis P. Dullemond
Figure caption: Images of initial and final conditions for the MgSiO3–Fe system illustrating complete miscibility at 9000 K and 60 GPa. The final state is after 7 ps of model time. Time steps were 0.5 fs. The model consists of 76 Fe atoms, 18 Mg atoms, 18 Si atoms, and 54 O atoms.
Paper: Differentiation, the Exception, Not the Rule: Evidence for Full Miscibility in Sub-Neptune Interiors
Authors: Edward D. Young, Aaron Werlen, Sarah P. Marcum, Lars Stixrude, Cornelis P. Dullemond
Figure caption: The Gibbs free energy of the mixing surface for the MgSiO3–H2 system at 3591 K and 4 GPa as formulated by L. Stixrude & T. Gilmore (2025). The binodes for the melt and envelope phases at this T and P, as well as the tie line between them, are shown for clarity. Also shown are the positions of the spinodes where the curvature is zero.
Paper: Differentiation, the Exception, Not the Rule: Evidence for Full Miscibility in Sub-Neptune Interiors
Authors: Edward D. Young, Aaron Werlen, Sarah P. Marcum, Lars Stixrude, Cornelis P. Dullemond
Figure caption: Isobaric phase diagram for the Fe–H2 binary system based on Equation (4). The extrapolation of the low-P and low-T hydrogen solubility in liquid Fe metal is shown for comparison (H.-W. Zhang 2007; G. Jiang et al. 2011). Errors for the latter are derived by standard propagation of uncertainties.