adsabs/AstroCLIMB huggingface dataset:
Paper: The Effects of Early Collisional Evolution on Amorphous Water Ice Bodies
Authors: Jordan K. Steckloff, Gal Sarid, Brandon C. Johnson
Figure caption: Tracer thermal profiles and locations in colliding bodies. We plot the thermal profiles for 5 of the 49,212 tracers in our simulation of two 100 km bodies at 50 K colliding at 3 km s−1. Left: tracers in different parts of the body experience very different thermal profiles. Minor numerical artifacts are visible from the tracer passing through different grid cells, producing a sawtooth pattern in some of the profiles. Tracers are identified by tracer number and the fraction of that tracer’s initial AWI that is crystallized. Right: we trace the tracers to their original locations in the bodies at the moment of impact. Colors denote the fraction of each tracer’s initial AWI that crystallizes during the impact process.
Paper: The Effects of Early Collisional Evolution on Amorphous Water Ice Bodies
Authors: Jordan K. Steckloff, Gal Sarid, Brandon C. Johnson
Figure caption: AWI crystallization fraction provenance for two 100 km objects striking each other at 50 K initial temperature. The amount of AWI that crystallizes is highly sensitive to impact speed. Left: at 2 km s−1, minimal AWI is crystallized, mostly near the point of contact. Middle: this region of crystallization expands at 3 km s−1. Right: at 4 km s−1, the objects nearly fully crystallize. The “spike” near the symmetry axis (most visible in the 3 km s−1 case) is most likely a numerical artifact that results from the extremely small cell volumes near the axis of symmetry. Ultimately, their volumes are very small and thus do not significantly affect our results.
Paper: The Effects of Early Collisional Evolution on Amorphous Water Ice Bodies
Authors: Jordan K. Steckloff, Gal Sarid, Brandon C. Johnson
Figure caption: Fraction of initial AWI that remains uncrystallized and fully crystallizes as a function of initial object temperature. The crystallization dynamics of AWI depends weakly on the initial temperatures of the colliding objects. Above ∼80 K, this dependence becomes significant; however, such initial temperatures would be characteristic of objects interior to the proto-EKB, suggesting that such initial temperatures are unlikely.
Paper: The Effects of Early Collisional Evolution on Amorphous Water Ice Bodies
Authors: Jordan K. Steckloff, Gal Sarid, Brandon C. Johnson
Figure caption: Crystallization timescale of AWI as a function of temperature. This is the AWI crystallization timescale from Kouchi et al. (1994), showing that the timescale of AWI crystallization is highly temperature dependent.
Paper: The Effects of Early Collisional Evolution on Amorphous Water Ice Bodies
Authors: Jordan K. Steckloff, Gal Sarid, Brandon C. Johnson
Figure caption: Fraction of initial AWI that remains uncrystallized and fully crystallizes during impact between 100 and 10 km objects as a function of impact speed for different initial temperatures. The crystallization dynamics of AWI is highly sensitive to impact speed across all temperatures considered. The total amount of AWI that crystallizes is much lower than impacts between 100 km objects, as the impactor penetrates and crystallizes material to a depth comparable to its own size. Thus, the majority of the target is unaffected. Nevertheless, such smaller impactors are much more common than the larger, catastrophic impacts.
Paper: The Effects of Early Collisional Evolution on Amorphous Water Ice Bodies
Authors: Jordan K. Steckloff, Gal Sarid, Brandon C. Johnson
Figure caption: AWI crystallization fraction provenance for 10 km impactors striking 100 km targets at 50 K initial temperature. The amount of AWI that crystallizes is again highly sensitive to impact speed. Left: at 2 km s−1, minimal AWI is crystallized. Middle: at 3 km s−1, the impactor is partially crystallized, along with a comparable volume of the target. Right: at 4 km s−1, the impactor is nearly fully crystallized, and fully crystallized a volume of the target comparable in volume to the impactor. In all cases, AWI crystallization is localized to the impact site itself, with negligible AWI crystallization observed distal to the impact site.
Paper: The Effects of Early Collisional Evolution on Amorphous Water Ice Bodies
Authors: Jordan K. Steckloff, Gal Sarid, Brandon C. Johnson
Figure caption: Fraction of initial AWI that remains uncrystallized and fully crystallizes as a function of impact speed for different initial temperatures. The crystallization dynamics of AWI is highly sensitive to impact speed across all temperatures considered. The amount of AWI that crystallizes is particularly sensitive to the range of expected impact speeds between icy bodies during planet migration of 2–4 km s−1 (Morbidelli & Rickman 2015).
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Relative I/F differences between RT-IPGP-2022 simulations with recommended and modified atmospheric input parameters for the T–P profile and CH4, C2H2, and HCN VMR. Atmospheric transmission windows are shaded in gray.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Comparison between RT-IPGP-2016 and RT-IPGP-2022 input parameters. (a) Pressure–temperature profiles, (b) gas volume mixing ratio profiles, (c) aerosol single-scattering albedos for two altitude regimes, (d) aerosol single-scattering phase functions at 2.53 μm, and (e) aerosol extinction profiles.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: (a) Pixel footprints of the VIMS CM_1481624349_1 cube superimposed on the color-coded photometrically calibrated mosaic of Karkoschka & Schröder (2016) and the f-values/color correspondence, and (b) I/F of the VIMS CM_1481624349_1 cube at 2.018 μm. Pixels used for the endmember extraction are highlighted in red.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Fits between our model and the HLS endmember spectrum in atmospheric bands. The first three rows show the best fits for different aerosol fractal dimensions D  f  and the last row for the RT-IPGP-2016 model. Simulated and observed spectra are shown with their 2σ error bars. Best-fitting ﹩{\chi }_{\mathrm{red}}^{2}﹩ is given and associated F  h  and F  m  values with 2σ uncertainties are given in Table 2.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: HLS endmember spectrum from 0.88 to 2.6 μm computed from the VIMS cube CM_1481624349_1. In the methane bands (black dots), I/F values come from the pixel including the HLS (pixel [9,3]). In the atmospheric windows (red dots), I/F values are reconstructed by recombining neighboring pixels in order to best represent the spectrum of the HLS spectral/photometric unit. 2σ radiometric error bars are shown in black and 2σ propagated radiometric error bars are shown in red.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Fits between our model and the HLS endmember spectrum in atmospheric bands. Simulated and observed spectra are shown with their 2σ error bars. Best-fitting ﹩{\chi }_{\mathrm{red}}^{2}﹩ is given and associated F  h  and F  m  values with 2σ uncertainties are given in Table 2.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: (a) I/F spectra simulated by the RT-IPGP-2016 (red line) and RT-IPGP-2022 (black line) models under the same configuration (i.e., incidence, emission, phase angles set to 0°, surface albedo set to 0, and haze and mist scaling factors set to 1 with respect to the aerosol opacity observed by Huygens (Doose et al. 2016)). Bottom panels: residuals between RT-IPGP-2016 and RT-IPGP-2022 simulations due to (b) all atmospheric inputs, (c) gas VMR only, (d) gas line lists only, and (e) aerosols only.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: ULIS radiance at 1.278 μm as a function of the altitude for spectra that meet the selection criteria (red dots). The black line corresponds to the best linear fit.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Comparison between ULIS (dotted black) and simulated I/F (RT-IPGP-2016 in red and RT-IPGP-2022 in blue) within the ULIS wavelength range for 21 different altitudes. Simulated spectra are coming from forward RT calculations using the haze and mist opacities estimated from the HLS endmember spectrum (see Section 3.2) and the surface albedo measured by Huygens/DISR (Karkoschka et al. 2012). The simulations are plotted along with their 2σ uncertainties envelope. Atmospheric windows are highlighted in gray.
Paper: The Optical Aurorae of Europa, Ganymede, and Callisto
Authors: Katherine de Kleer, Zachariah Milby, Carl Schmidt, Maria Camarca, Michael E. Brown
Figure caption: Average spectra centered on each emission line discussed in this paper on each night of observation. All spectra are reported in R Å−1 divided by the angular size of the target. Green spectra are detections with calibrated line strengths; red spectra indicate cloudy nights in which a detection is made, but no quantitative measurement is reported; blue spectra indicate that upper limits are reported; and black spectra are nondetections without reported upper limits due to nonphotometric conditions. Ticks along the horizontal axis shows the location of the center of the emission line(s), and the numbers on the bottom row indicate the wavelength boundaries of each plot in that column. For single emission lines, the boundaries are ±1 Å from the line center. For triplet lines, the boundaries are −1 Å from the shortest wavelength and +1 Å from the longest wavelength. All emission lines arise from atomic oxygen, except for hydrogen at 6563 Å (which is not detected).
Paper: The Optical Aurorae of Europa, Ganymede, and Callisto
Authors: Katherine de Kleer, Zachariah Milby, Carl Schmidt, Maria Camarca, Michael E. Brown
Figure caption: Detections of 6300 and 6364 Å O I emission at Callisto. For each emission, the lower panel shows a calibrated background-subtracted image of the spectrum that shows that the emission is localized along the slit (vertical axis), while the upper panel shows the spectrum summed across spatial bins containing the localized emission. The vertical ticks between the panels indicate the locations of the Doppler-shifted emission wavelengths for each transition. Each spectrum has been smoothed with a Gaussian kernel to enhance the features relative to the background. In the 6300 Å case, the bright points near the top and bottom of the slit just to the right of Callisto are residual from the subtraction of Earth’s 6300 Å, which is Doppler-shifted relative to the target.
Paper: The Optical Aurorae of Europa, Ganymede, and Callisto
Authors: Katherine de Kleer, Zachariah Milby, Carl Schmidt, Maria Camarca, Michael E. Brown
Figure caption: Detections of 7774 and 8446 Å O I emission at Ganymede. For each emission, the lower panel shows a calibrated background-subtracted image of the spectrum that shows that the emission is localized along the slit (vertical axis), while the upper panel shows the spectrum summed across spatial bins containing the localized emission. The vertical ticks between the panels indicate the locations of the Doppler-shifted emission wavelengths for each transition. Each spectrum has been smoothed with a Gaussian kernel to enhance the features relative to the background.
Paper: The Optical Aurorae of Europa, Ganymede, and Callisto
Authors: Katherine de Kleer, Zachariah Milby, Carl Schmidt, Maria Camarca, Michael E. Brown
Figure caption: Brightness of Europa’s aurora as a function of plasma sheet distance during each observation. Each observation has been normalized to its average. The dashed curve corresponds to a scale height of 1.67 R J.
Paper: The Optical Aurorae of Europa, Ganymede, and Callisto
Authors: Katherine de Kleer, Zachariah Milby, Carl Schmidt, Maria Camarca, Michael E. Brown
Figure caption: Measured auroral emissions along with the best-fit atmospheric model for Ganymede for each date of observation and for the average auroral emissions including previous UV measurements (Roth et al. 2021).
Paper: The Optical Aurorae of Europa, Ganymede, and Callisto
Authors: Katherine de Kleer, Zachariah Milby, Carl Schmidt, Maria Camarca, Michael E. Brown
Figure caption: Measured auroral emissions along with the best-fit atmospheric model for Europa for each date of observation and for the average auroral emissions including previous UV measurements (Roth et al. 2016).
Paper: The Optical Aurorae of Europa, Ganymede, and Callisto
Authors: Katherine de Kleer, Zachariah Milby, Carl Schmidt, Maria Camarca, Michael E. Brown
Figure caption: Spectrum covering the 7774 and 8446 Å emissions from Earth’s atmosphere, obtained with Keck/HIRES. Figure adapted from Slanger et al. (2004).
Paper: The Optical Aurorae of Europa, Ganymede, and Callisto
Authors: Katherine de Kleer, Zachariah Milby, Carl Schmidt, Maria Camarca, Michael E. Brown
Figure caption: Example MCMC output showing the individual and joint posterior distributions for the column densities of the three atmospheric species, based on the measurements and upper limits for the Ganymede average case. In the fits, the electron energies and densities are fixed at the values described in the text, and the column densities of the three species are the free parameters in the fit.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Two-way vertical transmission as a function of the wavelength as calculated by the RT-IPGP-2022 model. (a) Gas contributions only. (b) Total, all gases, and aerosol contributions.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Longitudinal transects at four different latitudes (5°N, 7°N, 10°N, and 12°N) extracted from the VIMS mosaic of the Selk crater region (see Figures 13 and 14 and 15): (first row) incidence, emission, and phase angles, in red, green and blue, respectively, (second row) I/F in an atmospheric band, at 0.88 μm here, (third row) haze (F  h , red curve) and mist (F  m , orange curve) opacity factors, along with their 2σ uncertainty envelops, (fourth row) I/F in an atmospheric window, here at 1.07 μm, and (fifth row) surface albedos at 1.07 μm, uncorrected (in blue) and corrected (in red) for surface photometry (see text for detailed explanations of the surface photometry correction), along with their 2σ uncertainty envelop. Zooms on a few transitions between VIMS data cubes are also provided. Gray dotted vertical lines correspond to cube transitions.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Mosaics of the four selected (and co-registered) VIMS cubes over the Selk crater area in the four first atmospheric windows: (top row) I/F, (middle row) direct output of our RT model, i.e., Lambertian surface albedo, and (bottom row) Lambertian surface albedo corrected for surface photometry. The mapping projection is rectangular with grid marks every 5° of longitude and latitude. Longitude is in degrees east. We extract I/F, uncorrected, and corrected surface albedo transects along the four horizontal red lines indicated on the 1.07 μm I/F mosaics (see Figure 16).
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: (a) RGB mosaic of the Selk crater region, with the 1.57/1.28 μm albedo ratio as the red channel, the 2.02/1.28 μm albedo ratio as the green channel, and the 1.28/1.07 μm albedo ratio as the blue channel. (b) Same mosaic for the “water ice enrichment” index. (c) and (d) Zooms on (a) and (b). (e) Classification map of the Selk crater region (Lorenz et al. 2021). The color legends are given in the frame above. White arrows designate the areas with the highest “water ice enrichment” index, corresponding to the dark-blue units on the RGB mosaic. The initial landing ellipse of Dragonfly is indicated by the solid oval on each map (Barnes et al. 2021).
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Mosaics of the four selected (and co-registered) VIMS cubes over the Selk crater area in the four last atmospheric windows: (top row) I/F, (middle row) direct output of our RT model, i.e., Lambertian surface albedo, and (bottom row) Lambertian surface albedo corrected for surface photometry. The mapping projection is rectangular with grid marks every 5° of longitude and latitude. Longitude is in degrees east. The 5 μm window mosaics result from averaging over 15 VIMS spectels from 4.89 to 5.13 μm to increase the S/N.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Mosaics of the four selected (and co-registered) VIMS cubes over the Selk crater area: (a) I/F at 0.89 μm, (b) I/F at 0.94 μm, (c) spatial sampling in km pixel−1, (d) RGB color composite with R = 〈5 μm〉, G = 2.02 μm, and B = 1.28 μm (Barnes et al. 2007), (e) RGB color composite with R = 2.02 μm, G = 1.57 μm, and B = 1.28 μm (Soderblom et al. 2010), (f) RGB color composite with R = 1.57/1.28 μm, G = 2.02/1.28 μm, and B = 1.28/1.07 μm (Le Mouélic et al. 2019), (g) incidence angle, (h) emission angle, and (i) phase angle. The mapping projection is rectangular with grid marks every 5° of longitude and latitude. Longitude is in degrees east.
Paper: Updated Radiative Transfer Model for Titan in the Near-infrared Wavelength Range: Validation against Huygens Atmospheric and Surface Measurements and Application to the Cassini/VIMS Observations of the Dragonfly Landing Area
Authors: M. Es-sayeh, S. Rodriguez, M. Coutelier, P. Rannou, B. Bézard, L. Maltagliati, T. Cornet, B. Grieger, E. Karkoschka, S. Le Mouélic, A. Le Gall, C. Neish, S. MacKenzie, A. Solomonidou, C. Sotin, A. Coustenis
Figure caption: Mosaics of the four selected (and co-registered) VIMS cubes over the Selk crater area: (a) I/F at 0.88 μm, (b) retrieved haze scaling factor F  h , and (c) retrieved mist scaling factor F  m . For comparison, the same 33% relative dynamics range values are applied for the three mosaics. The mapping projection is rectangular with grid marks every 5° of longitude and latitude. Longitude is in degrees east. We extract I/F, F  h , and F  m  transects along the four horizontal red lines indicated on the 0.88 μm I/F, F  h , and F  m  mosaics (see Figure 16).