adsabs/AstroCLIMB huggingface dataset:
Paper: Mercury’s Hidden Past: Revealing a Volatile-dominated Layer through Glacier-like Features and Chaotic Terrains
Authors: J. Alexis P. Rodriguez, Deborah Domingue, Bryan Travis, Jeffrey S. Kargel, Oleg Abramov, Mario Zarroca, Maria E. Banks, John Weirich, Anthony Lopez, Nicholas Castle, Yan Jianguo, Frank Chuang
Figure caption: iSALE2D hydrocode model incorporating an initial regolith overburden—The model features an overlying stratum of 1.2 km of basaltic regolith placed atop the VRL. Take note of the peak ring, approximately 60 km radially distant from the center, which continues to preserve VRL constituents. (a) Snapshot at 30 s post-impact, illustrating the maximum depth achieved. (b) Frame at 170 s, depicting the ejecta curtain encapsulating the overturned stratigraphy. (c) Image at 300 s showcasing the formation of a transient central peak and ejecta blanket. (d) Final visualization at 700 s (see also Figure 9(A)).
Paper: The Spatial Distribution of the Unidentified 2.07 μm Absorption Feature on Europa and Implications for its Origin
Authors: M. Ryleigh Davis, Michael E. Brown, Samantha K. Trumbo
Figure caption: (a) A map of Europa’s trailing hemisphere, showing a selection of four of the 29 considered “rings of constant radiolysis,” outlined in black, which are used to determine whether the weak 2.07 μm absorption feature is associated with Europa’s large-scale geologic units. The chaos terrains are shown in red and Pwyll crater and its ejecta are orange. For each ring, projected detector pixels are shown and their assigned geologic unit indicated by color, where chaos terrains are dark red, Pwyll crater and its ejecta are orange, and the ridged plains are gray. (Europa map image credit: NASA/JPL/Björn Jónsson). (b) Summed spectra, by geologic unit, for all of the pixels within each example ring. Spectra are normalized to 1.0 at 2.12 μm and offset for clarity. The best-fit polynomial continuum is indicated by a black dashed line. (c) Continuum-removed absorption feature, by geologic unit, for the four selected example constant-radiolysis rings. The depth of the feature decreases noticeably as we move from Ring 1 outwards, however there is no apparent difference in the depth of the 2.07 μm feature between the chaos terrains (red) and ridged plains (gray) for a given ring. This suggests that the absorption feature is unaffected by the compositional difference between the chaos terrains and ridged plains, and it is therefore unlikely to be related to any of the proposed irradiation products of endogenic material. Instead, the 2.07 μm feature appears to arise from the radiolytic processing of water ice with exogenic material, possibly related to the sulfur radiolytic cycle. One notable exception is that the 2.07 μm absorption feature is entirely absent from Pwyll crater and its ejecta blanket.
Paper: The Spatial Distribution of the Unidentified 2.07 μm Absorption Feature on Europa and Implications for its Origin
Authors: M. Ryleigh Davis, Michael E. Brown, Samantha K. Trumbo
Figure caption: (a) Expected trailing hemisphere irradiation patterns as a function of the angular distance from the trailing hemisphere apex for cold sulfur ions (solid; Cassidy et al. 2013), radiolytically produced hydrated sulfuric acid (dashed; Carlson et al. 2002; Ligier et al. 2016), and 0.1–25 MeV electrons (dotted; Paranicas et al. 2009). The estimated energy fluxes are normalized to 1.0 at the trailing hemisphere apex. (b) Calculated band area of the 2.07 μm absorption feature for each of the 29 “rings of constant radiolysis” considered. We find no measurable difference in the absorption depth between the chaos terrains and ridged plains. However, the absorption feature is essentially absent from Pwyll crater and its ejecta blanket. (c) Calculated 2.07 μm band area of the chaos terrains from panel (b), with the chaos terrains further subdivided by type as described in Leonard et al. (2023). There is no measurable difference in the 2.07 μm band area between the different types of chaos terrain.
Paper: The Spatial Distribution of the Unidentified 2.07 μm Absorption Feature on Europa and Implications for its Origin
Authors: M. Ryleigh Davis, Michael E. Brown, Samantha K. Trumbo
Figure caption: Example VLT/SINFONI spectra of Europa’s leading and trailing hemispheres showing the 2.07 μm absorption feature, which is only present on Europa’s more heavily irradiated trailing hemisphere. The data are normalized to 1.0 at 2.2 μm, and the trailing hemisphere spectrum is offset by +0.5 for clarity. The vertical dotted line marks the location of the 2.07 μm band center, and the continuum-removed absorption (multiplied by a factor of 3) is included above each spectrum.
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: examples of Miranda spectra displaying weak absorption features around 2.2 μm. The green spectrum is the (unbinned) spectrum reported in Bauer et al. (2002). The two blue spectra were obtained with SpeX in the PRISM and SXD configuration (unbinned and binned by 10 pixels, respectively). The orange spectra are spectra from individual nights with TripleSpec (binned by 30 pixels). The text next to each spectrum indicates the date of observation in the format UTYYMMDD (e.g., UT200907 = UT 2020-09-07). This UTYYMMDD date format is used throughout this work. Vertical lines are placed at the expected wavelengths for the absorption features studied in this work: brown lines at 1.966, 2.012, and 2.070 μm for the CO2 ice triplet, a black line at 2.134 μm for a feature associated with molecular mixtures including CO2 ice, a blue line at 2.21 μm for NH3 hydrates, and a blue line at 2.24 μm for crystalline NH3 ice. The shaded region indicates the wavelength range measured for the 2.2 μm band in this work. Right panel: the GNIRS spectra and TripleSpec quadrant and hemisphere grand average spectra originally reported in DeColibus et al. (2022). The colored points are binned by 15 pixels, and the gray error bars are presented at the native resolution of the data.
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Left panel: an image mosaic of Miranda’s southern hemisphere from imaging by Voyager 2 in 1986. We use an orthographic projection centered on the south pole, using the Miranda mosaic produced by Schenk & Moore (2020). The “coronae” are regions heavily modified by tectonic activity and possessing intriguing patches of high-albedo material. Only two of the disk-integrated spectra in our data set were observed with subobserver latitudes on the southern hemisphere: UT990607, green (Bauer et al. 2002), and UT000907, blue (Cartwright et al. 2018). The error bars in longitude represent the range of subobserver longitudes covered during the duration of that observation. Right panel: all the other spectra in our data set observed Miranda’s northern hemisphere, which was in darkness at the time of the Voyager flyby and has no imaging data available. The orange spectra were observed with TripleSpec, the blue spectra were observed with SpeX, and the purple spectra were observed with GNIRS. The longitudes appear to increase in opposite directions as seen from the north and south poles, so we chose to orient the 0° meridian at the top of the figure in both panels.
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Band area and depth measurements for each Miranda spectrum in this work, with 1σ error bars. Band area and depth measurements that are not statistically significant (<2σ from zero) are plotted as gray triangles, while those that are ≥2σ are plotted as red triangles. Quadrant-averaged mean band parameters (Table 5) are plotted as purple squares. The gray shaded regions on either side of each plot represent overlapping longitudes. Data points are duplicated in these regions to better visualize possible sinusoidal variations with longitude. The weighted averages and sinusoidal fits to all spectra for each measurement are plotted as golden horizontal lines and gray dotted–dashed lines, respectively. Top left: total band areas for the CO2 ice triplet measurements (sum of the 1.966, 2.012, and 2.070 μm band areas). Center row: band area measurements (left panel) and band depths (right panel) for the 2.13 μm band. Bottom row: the same as the center row, but for the 2.2 μm band.
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: A demonstration of the band area and depth measurement process for the CO2 ice triplet and the 2.13 and 2.2 μm bands, using the GNIRS leading hemisphere spectrum of Miranda from UT201008. The data points over which the band areas are integrated are marked in blue, the points where the band depth is measured in red, continuum fits are cyan lines, and Gaussian band fits are orange lines. A copy of the spectrum plotted with an offset has been binned by five pixels (turquoise points). The vertical lines are the same as in Figure 2.
Paper: Are NH3 and CO2 Ice Present on Miranda?
Authors: Riley A. DeColibus, Nancy J. Chanover, Richard J. Cartwright
Figure caption: Band area and depth measurements for the high-S/N Miranda spectra (GNIRS spectra and the TripleSpec quadrant/hemisphere grand average spectra), along with the same mean measurements (purple squares) plotted in the previous figure. All error bars represent 1σ uncertainties. The weighted average and sinusoidal fits use the mean band measurements.
Paper: Col-OSSOS: The Distribution of Surface Classes in Neptune's Resonances
Authors: Rosemary E. Pike, Wesley C. Fraser, Kathryn Volk, J. J. Kavelaars, Michaël Marsset, Nuno Peixinho, Megan E. Schwamb, Michele T. Bannister, Lowell Peltier, Laura E. Buchanan, Susan Benecchi, Nicole J. Tan
Figure caption: The orbital distribution of Col-OSSOS targets in a, e, and oscillating i as reported by Bannister et al. (2018). The semimajor axis is shown with three different scales, as indicated in the x-axis and separated by axis gaps, in order to show the details in the cold classical region as well as the inner and distant objects in the Col-OSSOS sample. The different dynamical classifications are nonresonant dynamically excited (DE) objects (black circles), cold classical (CC) objects (pink squares), 4:3 resonators (orange triangles), 3:2 resonators (yellow squares), resonant objects within the classical region (green wide ‘x’s, includes all resonant objects within the main classical belt), 2:1 resonators (cyan diamonds), and resonant objects with semimajor axes a > 49 au (blue hexagons). The number of objects in each classification is indicated in parentheses in the legend. All populated resonances are labeled with gray dashed vertical lines. Neptune is indicated with a large blue circle.
Paper: Col-OSSOS: The Distribution of Surface Classes in Neptune's Resonances
Authors: Rosemary E. Pike, Wesley C. Fraser, Kathryn Volk, J. J. Kavelaars, Michaël Marsset, Nuno Peixinho, Megan E. Schwamb, Michele T. Bannister, Lowell Peltier, Laura E. Buchanan, Susan Benecchi, Nicole J. Tan
Figure caption: Left: the r − J versus g − r color distribution of Col-OSSOS TNOs. The black arc is the reddening line, or line of constant spectral slope. The same symbol colors are used here as in Figure 1: nonresonant Dynamically excited objects (black circles), cold classical objects (pink squares), 4:3 resonators (orange triangles), 3:2 resonators (yellow squares), resonant objects within the classical region (green wide ‘x’s), 2:1 resonators (cyan diamonds), and resonant objects with semimajor axes a > 49 au (blue hexagons). The Plutinos are the largest resonant sample, and span the full range of surface colors seen in the sample. The objects below the gap feature (parallel to the reddening line) are primarily cold classical and resonant TNOs. Right: the color–color plot re-projected into the PC1 and PC2 components, the distance along the reddening line and from the reddening line, respectively. In this re-projection, the gap feature is indicated by the dashed line at PC﹩{}_{{grJ}}^{2}=-0.13﹩. The FaintIR surface classification below this line is dominated by cold classical objects and resonant TNOs. It includes one 4:3, one 2:1, and several 3:2 resonators, as well as a few dynamically excited objects and a distant a > 49 au resonator.
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: Ranges of estimated heat fluxes for icy bodies throughout the solar system assuming lithospheres without porosity and that are composed of pure H2O ice. Some references provide additional estimates that account for lithospheric porosity and possible NH3–H2O constituents in the lithospheres, but we do not include them here for a more straightforward comparison. Other than Titania, in the Uranian system, heat flux estimates are provided for two regions on Miranda (Beddingfield et al. 2015a, 2022c) and many regions on Ariel (Peterson et al. 2015; Beddingfield et al. 2022b; Bland et al. 2023). In the Jovian system, heat flux estimates are provided for Europa (Hussmann et al. 2002; Nimmo & Manga 2002; Ruiz 2003, 2005; Tobie et al. 2003; Showman & Han 2004) and Ganymede (Nimmo et al. 2002; Nimmo & Pappalardo 2004; Bland et al. 2017; Singer et al. 2018). For moons in the Saturnian system, heat flux estimates are provided for Enceladus (Bland et al. 2007, 2012, 2015; Barr 2008; Giese et al. 2008; O’Neill & Nimmo 2010; Han et al. 2012; Leonard et al. 2021a), Dione (Hammond et al. 2013; White et al. 2017), Tethys (Giese et al. 2007; White et al. 2017; Beddingfield et al. 2023), Rhea (Nimmo et al. 2010; White et al. 2013), and Iapetus (White et al. 2013). In the Neptunian system, heat fluxes are provided for Triton (Ruiz 2003; Sori 2021). In the Pluto system, heat fluxes are provided for Pluto (Conrad et al. 2019, 2021; McKinnon et al. 2023) and Charon (Conrad et al. 2021).
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: 3D representation of our DEM with vertical exaggeration (Figure 3). Evidence for flexure in the topography is observable bounding both rims of Messina Chasmata (examples shown by white arrows). The ridges and grooves, mapped by Croft & Soderblom (1991; see tectonic symbols in Figure 2), trending approximately perpendicular to Messina, are observable in our DEM. For a scale bar and elevation color bar, see Figure 3. South is to the right, and white squares are removed reseau points. See Figure 2 for the location of our study area on Titania.
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: (a) Estimated elastic thicknesses on Titania. (b) Estimated heat fluxes on Titania assuming a porosity of 0%. (c) Estimated heat fluxes assuming a pure H2O lithospheric composition and porosities ranging from 5% to 25%. (d) Estimated heat fluxes assuming an H2O ice lithosphere with small amounts of NH3 hydrates and porosities ranging from 5% to 25%. See Table 2 in Appendix A.2 for the full set of estimated values. For the location of our study area, see the yellow box in Figure 2.
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: (a) Annotated version of a portion of Voyager 2 ISS image c2684313 (2.88 km pixel−1) showing the locations of the profile lines used for this analysis along the rims of Messina Chasmata. (b) Profile topographic data (black) with superimposed model flexural profiles (cyan) for all study locations (A–J). Gray arrows show locations where flexural curvature is evident. See Figures 6 and 11 for estimated values for T  e  and F. See Table 2 for a full list of estimated values of F for porosities of 0%–25%. In addition to topography associated with flexure, topography associated with impact craters and faults is present. This topography was excluded from our flexural models.
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: Top: processed Voyager 2 ISS image (c2684313) of the Messina Chasmata region. Bottom: structural map of the Messina Chasmata region. Dashed lines indicate where identification of the structure is uncertain. Labels (A, B, and C) indicate specific scarps that are discussed in the text. White arrows indicate areas with important cross-cutting relationships between the scarps.
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: Ranges of estimated heat fluxes for Uranus’s large moons, assuming pure H2O ice lithospheres without porosity. The relative sizes of the moons are shown, and they are ordered with increasing distance from Uranus (from left to right). Our estimates are provided for Titania (D = 1578 km). Other heat flux estimates are provided for Miranda (D = 472 km; Beddingfield et al. 2015a, 2022c) and Ariel (D = 1158 km; Peterson et al. 2015; Beddingfield et al. 2022b; Bland et al. 2023). Heat fluxes have not yet been investigated for Titania’s neighboring moons, Umbriel (D = 1169 km) or Oberon (D = 1523 km).
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: Mapped estimates of heat fluxes that take into account porosity and assuming a lithosphere with the following properties: (a) pure H2O ice with 5% porosity; (b) H2O ice with H2O–NH3 and 5% porosity; (c) pure H2O ice with 15% porosity; (d) H2O ice with H2O–NH3 and 15% porosity; (e) pure H2O ice with 25% porosity; (f) H2O ice with H2O–NH3 and 25% porosity.
Paper: Titania's Heat Fluxes Revealed by Messina Chasmata
Authors: Chloe B. Beddingfield, Erin J. Leonard, Tom A. Nordheim, Richard J. Cartwright, Julie C. Castillo-Rogez
Figure caption: Surface heat flux predicted at the surface of Titania (solid gray line) for the interior evolution model featured in Castillo-Rogez et al. (2023) for a time of formation of 4 Myr after the formation of calcium–aluminum inclusions, no tidal heating, and assuming a maximum porosity of 25%. For comparison, the heat flux corresponding to radioisotope decay heat assuming a perfect conductor is presented (dashed black line). See text for more details.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Example of spectra measured by TGO/NOMAD (black curves) in diffraction order 183 (a), order 184 (b), order 185 (c), and order 186 (d). These spectra are measured around 30 km tangential height on 2022 March 1st (the first orbit shown in Table 1). The red curves show the best-fit synthetic spectra. The continuum transmittance is around 0.97, due to the extinction by the aerosols presented along the line of sight. The top small panels show the line intensities of 12C16O (red with circular symbols), 13C16O (blue with triangle symbols), and 12C18O (green with square symbols) in the main diffraction order obtained from HITRAN2020 database. The small bottom panels illustrate the residuals of the top panel in red and the instrumental noise level in black. The residuals are usually within the instrumental noise level, except for some features that come from nearby diffraction orders (these features are present due to the nature of the AOTF transfer function).
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Synthetic spectra of the NOMAD measurements taken with diffraction order 183 (a), order 184 (b), order 185 (c), and order 186 (b) around 30 km tangent height. The assumed vertical profile of total CO volume mixing ratio is 1000 ppm (uniform) and along the line of sight. The isotopic ratios defined in the HITRAN2020 databases are assumed. The red, blue, and green curves illustrate contributions due to 12C16O, 13C16O, and 12C18O absorption lines. The origin of the Y-axis for the red, blue, and green curves have been offset to improve visibility.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Examples of the NOMAD spectra measured by diffraction order 132 around 30 km tangent height (black) and the best-fit synthetic spectra (red). The bottom small panels show the differences between the observed spectra and the best-fit synthetic spectra in red curves and the instrumental noise level in black.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ 13C values in CO obtained with 12C16O and 13C16O volume mixing ratio retrieved with original temperature profiles and AOTF transfer function shifted by its uncertainty in the positive direction.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ 13C values in CO obtained with 12C16O and 13C16O volume mixing ratio retrieved with original temperature profiles and AOTF transfer function shifted by its uncertainty in the negative direction.
Paper: Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations
Authors: S. Aoki, K. Shiobara, N. Yoshida, L. Trompet, T. Yoshida, N. Terada, H. Nakagawa, G. Liuzzi, A. C. Vandaele, I. R. Thomas, G. L. Villanueva, M. A. Lopez-Valverde, A. Brines, M. R. Patel, S. Faggi, F. Daerden, J. T. Erwin, B. Ristic, G. Bellucci, J. J. Lopez-Moreno, H. Kurokawa, Y. Ueno
Figure caption: Vertical profiles (a) and histogram (b) of δ 13C values in CO obtained with 12C16O and 13C16O volume mixing ratio retrieved with original AOTF transfer function and temperature profiles.