adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Changes in water-vapor column density as a function of Enceladus’s orbital phase. The top panel shows the column density measurements for 249 spectral cubes with different colors representing the days in which the observations were taken. The bottom panel shows nonweighted average column density estimates for each observation group. Column density measurements of Enceladus's plume occultations observed by UVIS obtained from Hansen et al. (2020) are also shown. There is no evidence for a clear pattern of water-vapor column density variations over Enceladus’s orbit. Note that although a small fraction of column densities in the top panel are negative, this is likely due to random noise because the signal-to-noise for individual measurements are relatively low. The fact that none of the averaged points in the lower panel are significantly negative is consistent with this idea. A full table of the estimated column densities and the observation properties of the individual cubes in the top panel is hosted by this figure and is available for download.(The data used to create this figure are available.)
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Left: map of the plume’s brightness at 2.70 μm derived from an average of five VIMS cubes (V1511798376, V1511800181, V1511800741, V1511801493, and V1511802247). Note that this brightness is mostly due to reflected sunlight from Enceladus’s lit limb and the plume particles. The image is reprojected on a grid with 19 km pixel–1 and oriented so that the plume points downward. Right: map of the water-vapor column density derived from the same averaged image. Column densities were calculated using the average residual values and Equation (1). Note that regions of high column density are visible outside the region where the plume particles are bright, which provides evidence that this signal traces a different plume component. The red circles outline Enceladus, and the red rectangles show the pixels used for the spectral analysis (see Section 2).
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Column density variations plotted over the orbital phase in four different observation groups. 2005 November 27 Group: variations in the subset of observations analyzed in Hedman et al. (2009). With good signal-to-noise ratios, this group consistently shows the water-vapor signal in the middle five observations. 2007 September 30 and 2011 October 1 groups: two examples of column density strengths possibly increasing or decreasing within 1 hr. 2012 March 27 group: represents an interesting pattern of column densities between orbital phases 135° and 145°. This region appears to show the column density may be oscillating between two values, one around 3 × 1020 m−2 and the other being within 1σ of 0.
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Theoretical spectral channel shift of the water-vapor emission feature in Cassini-VIMS observations from 2005 to 2015. Spectral shift values were taken from Clark et al. (2018), and the spectral models were produced using the PSG.
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Modeling Enceladus plume spectra using Mie scattering theory. The processed plume spectra were obtained from Hedman et al. (2009). Upper panel shows the best-fit Mie model for plume spectra observed 35 km above the surface of Enceladus in the 2.5–3.7 μm wavelength range. Lower panel shows the resulting residual intensity after subtracting the Mie model from the spectra. The shaded regions on each plot highlight the wavelength band of interest, a near-infrared region that contains a water-vapor emission peak.
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: The nonweighted average spectral residuals for observation groups with a column density error lower than 1.2 × 1019 m−2. Each residual is colored by the date the observations were taken, corresponding to Figure 3.
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Column density variations for groups 2009 November 1 through 2011 November 5. Variations in groups 2005 November 27, 2007 September 30, and 2011 October 1 can be found in Figure 4.
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Column density variations for groups 2012 April 14 and 2015 October 14. Variations in group 2012 March 27 can be found in Figure 4.
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Residual spectra for groups 2005 November 27 through 2011 January 30.
Paper: Constraining Time Variations in Enceladus’s Water-vapor Plume with Near-infrared Spectra from Cassini’s Visual and Infrared Mapping Spectrometer
Authors: K. E. Denny, M. M. Hedman, D. Bockelée-Morvan, G. Filacchione, F. Capaccioni
Figure caption: Residual Spectra for groups 2011 October 1 through 2015 October 14.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: Geographic setting of the lunar south pole with the 13 Artemis candidate landing sites (red boxes) and our study area (green box), which includes two of the candidate landing sites on the Nobile and Amundsen rims (NASA 2022). The WAC image mosaic highlights the extensive shadows at the lunar south pole due to the high-relief topography and low solar illumination angles at the poles.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: The complex impact history of the Amundsen crater (red) region, including the SPA rim (blue), the Amundsen–Ganswindt basin (green), and three pre-Nectarian craters (yellow). The locations of the craters displayed on an LDEM hillshade base map were extracted from the crater catalog of Head et al. (2010).
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: Geomorphologic map of Amundsen crater produced at a mapping scale of 1:100,000 and digitized at 1:1M scale on an LDEM hillshade base map.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: (a) Oblique view of the study area illustrating the SPA massifs (black arrows; pNSPA, no vertical exaggeration, facing the lunar nearside), with the study area outlined in red. (b) Arcuate-oriented segments (indicated by black arrows) of an ancient putative central peak ring (dashed green circle; pNAG) in the Amundsen–Ganswindt basin (green circle). The Amundsen crater rim is shown in red. (c) Example of pre-Nectarian basin materials (pNbm), consisting of arcuate, subdued, and obliterated segments of ancient impact structures (white line).
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: (a) Count areas for the plains materials (Ilp; blue), mantling deposits (Itm; red), and ejecta blanket (NAe; black) on the LDEM hillshade. CSFD measurements of Ilp1 (outside Amundsen) and Ilp2 (Amundsen crater floor) are shown as (b) cumulative and R-plots to highlight their similar ages of ∼3.8 Ga. Plots for “Itm3” are shown in Figure 10 and “NAe” in Figure 13.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: (a) Topographic map of the study area, shown as a 20 m pixel−1 LRO LDEM (Smith et al. 2010), illustrating a regional elevation range of ∼11.5 km and the two Artemis candidate landing sites (red boxes). (b) A slope map derived from (a). (c) Average solar illumination derived from Mazarico et al. (2011) over a lunar year with permanently shadowed regions indicated in red. (d) Earth visibility from Mazarico et al. (2011).
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: LDEM hillshade comparison of the light plains (Ilp) (a) outside and (b; Kaguya mosaic) inside Amundsen crater with (c; Itm) the less cratered terra-mantling unit, which contains (d) buried craters and rill-like features.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: CSFD measurements of the Itm3 area (Figure 9(a)) of the terra-mantling unit (Itm; Figure 4) shown as cumulative and R-plots. The derived AMAs show the assumed formation age of the light plains (∼3.8 Ga; Figure 9(b)) and a possible resurfacing that would correspond to an event at ∼3.7 Ga.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: (a) Close-up view of Amundsen crater units overlaid on a hillshade base map to emphasize the geomorphological units, e.g., ejecta (NAe), perched rim segments (NAr), the terraced crater wall (NAcw), and the central peak (NAcp). The intersection of the two light gray diagonals (a) marks the center of the crater as measured from the rim to illustrate that the central peak complex is centered. Stars mark the positions of the four main peaks of the arcuate central peak structure (a). (b) Flat terraces on the crater wall show a higher crater density due to better preservation of smaller craters compared to the steeply sloping wall (Kaguya TC). (c) Shows two topographically elevated segments of the uplifted rim (NAr) with a missing rim segment between (LDEM).
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: Examples of crater classes included in our geomorphologic map (Figure 4) shown on an LDEM hillshade base map. (a) Nectarian craters generally lack continuous ejecta, do not have a sharp rim crest, and are no longer clearly circular in shape. (b) Imbrian craters, such as Idel’son L, are still morphologically distinct, moderately degraded craters but show continuous ejecta, typically modified by subsequent primary and secondary impacts. (c) Eratosthenian craters, such as Wapowski crater, exhibit a sharp rim crest, a low degree of degradation, and a well-defined ejecta blanket that retains fine texture and ridges (black arrows). (d) A cluster of secondary craters on the floor of Amundsen crater with irregular shapes and partially overlapping morphology.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: (a) Looking to the south at the landslide in Idel’son L crater (hillshade) with an elevation change of ∼1.5 km. (B) Oblique 3D view of the major landslide on the northwest wall of Amundsen crater (no vertical exaggeration), which exhibits an ∼8 km elevation change near the SPA massif remnants. White arrows in (a) and (b) indicate the downslope direction. Unit abbreviations in (b) are from Figure 4.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: CSFD measurements on the Amundsen crater wall (NAcw) and ejecta (NAe) presented as cumulative and R-plots using a Poisson fit. The NAcw-randomness analysis in the panel above shows some degree of clustering in the craters with diameters of <1 km, so these were excluded from the fit range of 1.5–6 km. The derived ages of the ejecta blanket and crater wall are similar.
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: Variations in (a) slope, (b) Sun visibility (Mazarico et al. 2011), and (c) Earth visibility (Mazarico et al. 2011) on an LDEM hillshade base map, colorized according to their implications for landing safety (green to red with decreasing safety). Dark regions in panel (b) show the locations of PSRs. White boxes indicate potential landing regions, discussed in Table 2 (AOI a: Artemis Nobile Rim 2; AOI b: Artemis Amundsen Rim; AOI c: ILRS Amundsen crater floor; AOI d: plains next to Idel’son L crater; AOI e: northern Amundsen Rim).
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: Distribution of (a) FeO and (b) plagioclase based on 1 km pixel−1 resolution spectral data from Lemelin et al. (2022) on a hillshade base map. Linear features (certain and approximate contacts and crater rim) from the geomorphological map (Figure 4) are included to show the characteristics of the mapped units. Spectral data are unavailable in PSRs (Mazarico et al. 2011; gray areas).
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: Temperature maps (Williams et al. 2019) showing the (a) summer average, (b) maximum, and (c) minimum plus the (d) winter average, (e) maximum, and (f) minimum bolometric temperatures on an LDEM hillshade base map. PSRs (black outlines) from Mazarico et al. (2011).
Paper: Geologic History of the Amundsen Crater Region Near the Lunar South Pole: Basis for Future Exploration
Authors: Lukas Wueller, Wajiha Iqbal, Thomas Frueh, Carolyn H. van der Bogert, Harald Hiesinger
Figure caption: Spatial distribution of distinct geomorphologic units over time. (a) Pre-Nectarian, (b) Nectarian, (c) Imbrian, and (d) Eratosthenian units on an LDEM hillshade base map. Secondary craters (sc) are not included, because their age is not differentiated in our geomorphologic map (Figure 4).
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of the posterior distributions for the Earth-like and abiotic false-positive O3 TRAPPIST-1 e using the evenly mixed forward model (﹩{{ \mathcal M }}_{\mathrm{iso}}﹩). The black lines represent the true profiles used to generate the observed spectrum, and the dotted black lines indicate the corresponding average volume mixing ratios (VMRs) of the true gas abundance profiles. We calculate the change in effective transit height for the spectral features of each gas in the noiseless input spectrum, to indicate the atmospheric layers to which the spectrum is sensitive (gray shading). For both atmospheres there are no O2 absorption features in the 2.8–20.0 μm mid-IR wavelength range we considered, so we are unable to perform this analysis. For the abiotic planet, there is no CH4 in the atmosphere, so we do not have true values to compare to.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of simulated transmission spectra for TRAPPIST-1 e modeled with a self-consistent, Earth-like atmosphere. When self-consistent ice and water clouds are included, no significant spectroscopic changes occur to the spectrum. We see small impacts due to clouds in the relatively transparent portion of the atmosphere between 8 and 13 μm, where the clouds reduce the minimum altitude probed from 10 to 12 km.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of the vertically resolved temperature structure and composition of each atmospheric case addressed in this study. The Earth-like and abiotic, O3 false-positive planets (first and second panels) have similar ozone inventories with visible stratospheric bulges.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of the evenly mixed (﹩{{ \mathcal M }}_{\mathrm{iso}}﹩), vertically resolved with three to five fixed pressure points (﹩{{ \mathcal M }}_{3P}﹩, ﹩{{ \mathcal M }}_{5P}﹩), and vertically resolved with three free pressure points (﹩{{ \mathcal M }}_{3F}﹩) forward models for retrieving O3 from a simulated transmission spectrum of a clear-sky, Earth-like TRAPPIST-1 e. The four top panels in the figure show an example of an O3 profile that the forward model may try to produce to generate a fit to the spectral data. The bottom panel compares the corresponding spectra generated by each forward model to the true simulated spectrum. The assumption of isothermal pressure–temperature profiles in each of the forward models also modifies the continuum and the depth of other spectral features relative to the true spectrum.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of O3 total column abundance distributions calculated for retrieval models with and without vertical resolution for both transmission cases. For both cases and across all models, we find that the total column abundance of O3 is broadly distributed and unconstrained, suggesting that the transmission spectra are relatively insensitive to the column even in the absence of aerosols.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of the vertically resolved O3 profiles retrieved by the ﹩{{ \mathcal M }}_{3F}﹩ forward model for the Earth-like and abiotic TRAPPIST-1 e cases. We note that for both atmospheres the retrieval effectively reproduced an evenly mixed O3 profile despite being allowed to move freely in pressure and abundance space for three points along the profile.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of the median spectral fits with ±1σ, 3σ envelopes for the Earth-like and abiotic false-positive O3 TRAPPIST-1 e. On each plot, we show the fit to the spectrum supplied by each version of the forward model and report its associated χ 2 value. Note that the lines and envelopes overlap significantly and appear gray when they do so. All models provide plausible fits to all spectral features for both transmission cases. We zoom in on the 4–12 μm range of the spectrum, as this is where the S/N is largest.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of the posterior distributions for the clear-sky and cloudy Earth using the evenly mixed forward model (﹩{{ \mathcal M }}_{\mathrm{iso}}﹩). Note that the y-axis on the albedo subplot provides a reference axis for interpreting the pressure-dependent profiles of all other parameters in the plot; we do not retrieve albedo as a function of pressure. The black lines represent the true profiles used to generate the observed spectrum. For the clear-sky case, the gray shaded regions indicate the Jacobian contributions to the true spectrum, where the opacity of these regions scales with their relative weight. Thus, a darker gray region indicates the atmospheric layer(s) to which each spectral feature is most sensitive. For the cloudy case, we show the Jacobian contributions to the true spectrum for an atmosphere with either 100% stratocumulus (yellow) or 100% cirrus clouds (red). The opacity of these regions also scales with their relative weight, and regions with significant overlap between stratocumulus and cirrus clouds Jacobian contributions take on an orange hue.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of the median spectral fits with 1 and 3σ posterior distributions shown as shaded envelopes (dark and pale, respectively) for the clear-sky and cloudy Earth. Note that the lines and envelopes corresponding to the different models overlap significantly and appear gray when they do so. On each plot, we show the fit to the spectrum supplied by each version of the forward model and report its associated χ 2 value. For the clear-sky Earth, the evenly mixed model visibly provides a better fit to the 0.3 μm feature. In the upper panel, note the larger distribution on the CO posteriors, and that vertically resolving the O3 profile results in the most significant changes to the fit to the spectrum in the region of the UV Hartley band. In the lower panel, note the large residuals in the water bands and in the CO/CO2 features ∼1.6 μm when wavelength-dependent clouds are present in the data but not included in the retrieval.