adsabs/AstroCLIMB huggingface dataset:
Paper: Moist Convection Is Most Vigorous at Intermediate Atmospheric Humidity
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: CAPE from the (a) EarthTemp, (b) EarthPressure, and (c) Titan experiments from the convection-resolving simulations (colored markers) and from the analytical predictions for CAPE given by Equation (A1) (gray shaded areas). The analytical predictions are shown for values of the bulk-plume parameter a ranging from 0.2 to 0.8 for the Earth-like experiments, and for a ranging from 0.5 to 1.5 for the Titan-like experiment. The analytical solutions are initialized with the temperature and humidity of the lifted condensation level from the corresponding simulation.
Paper: Moist Convection Is Most Vigorous at Intermediate Atmospheric Humidity
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: Profiles of environmental relative humidity in the (left) EarthTemp, (center) EarthPressure, and (right) Titan experiments. Relative humidity is plotted as a function of mean temperature in the troposphere, as in Romps (2014). The line colors are as in the main text figures, with relative humidity generally increasing as the condensible species become more prevalent.
Paper: Moist Convection Is Most Vigorous at Intermediate Atmospheric Humidity
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: As in Figure 1, but for the EarthPressure experiment. Note that in (b) the horizontal axis is inverted so that specific humidity increases toward the right.
Paper: Moist Convection Is Most Vigorous at Intermediate Atmospheric Humidity
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: As in Figures 1 and 3, but for the Titan experiment.
Paper: Moist Convection Is Most Vigorous at Intermediate Atmospheric Humidity
Authors: Jacob T. Seeley, Robin D. Wordsworth
Figure caption: (a) Normalized CAPE from the EarthTemp, EarthPressure, and Titan experiments, plotted as a function of the saturation-specific humidity at the lifted condensation level ﹩{q}_{v,\mathrm{LCL}}^{* }﹩. (b) As in (a), but for normalized high-percentile updraft speeds (﹩{w}_{\max }^{99.9}﹩).
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Clustering diagrams with griz colors in the 3D space (upper left panel) and the 2D projected planes for seven different taxonomic types of asteroids classified by the semisupervised learning model of Roh et al. (2022). The asteroids with errors smaller than 0.05 mag for g − i and i − z and 0.1 mag for griz color are drawn with the colors of their types. The colors of the dots are red for the S type, blue for the C type, purple for the X type, green for the V type, orange for the D type, yellow for the K type, lime for the L type, and gray for asteroids not assigned any types. The dark error bars in the projected planes are the mean errors of the drawn asteroids.
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Distribution of 306 reference asteroids observed by KMTNet on the gri slope and z − i color plane of DeMeo & Carry (2013). The gri slope is calculated as the percentage value of the difference in reflectance between the i and g bands divided by the difference in wavelength. The reference asteroids are plotted based on the KMTNet observations. The boundaries defined by DeMeo & Carry (2013) are drawn with colors corresponding to each taxonomy. The taxonomy types of the asteroids are from DeMeo et al. (2009), and the subtypes of the C, S, and X types are combined following the method used by DeMeo & Carry (2013). The mean error of the drawn asteroids is shown in the lower right corner.
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Taxonomic classification boundaries in the PC and i − z color plane. The colored points represent 308 reference asteroids previously classified by the Bus–DeMeo system. The gray points are the observed asteroids with errors smaller than 0.05. The crossed error bars in the lower left corner indicate the mean errors of the 308 reference asteroids (black) and gray points (gray).
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Distributions of all observed asteroids on the 2D (g − r) and (r − i) color plane (upper) and PC and (i − z) plane (lower). Black dots represent the reference asteroids (classified in the Bus–DeMeo system) with their photometric errors as error bars. Gray dots depict all other observed asteroids. The median errors are plotted in the lower right as gray dots. The black dashed line in the upper panel represents linear regression in the (g − r) and (r − i) color plane.
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Distributions of the observed asteroids on the PC vs. i − z color plane with taxonomic types classified in the 3D FGMM. Asteroids with photometric errors smaller than 0.05 mag are shown in this plot. Unclassified asteroids are marked with gray dots. The average photometric errors of all drawn asteroids are plotted in the lower right. The color boundaries are the taxonomic classification criteria defined in Section 3.2. The taxonomic type for each boundary is marked at the corner of it.
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Distribution of (a) brightness and (b) its uncertainty for the asteroids measured in the griz bands using the KMTNet-CTIO telescope.
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Transmission curves of the KMTNet SDSS filters with the reflectance spectra of S, X, C, and V Bus–DeMeo types. The averaged spectra are normalized at 550 nm.
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Orbital element distributions of taxonomic types assigned by classification methods on the 2D (a) and 3D (b) color planes. The fractions are calculated from the asteroids classified as any type with photometric errors to the axes of color diagrams smaller than 0.05 mag (smaller than 0.1 mag for the griz color of 3D color space). The sums of all fractions for each 0.05 au bin were 1.
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Histograms of photometric errors in i − z color (top) and PC (bottom) of the observed asteroid. For each panel, the blue line is the best fit of the Gaussian profile to the number distribution of the photometric error, where the mean value and 1σ range of the profile are marked on the upper axis (blue dashed lines). The red histogram indicates a normalized cumulative histogram of the photometric error in which the median and interquartile range values are marked on the lower axis (red dashed lines).
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Distribution of asteroids classified by the FGMM with a probability threshold of 0.1.
Paper: Taxonomic Classification of Asteroids Using the KMTNet Multiband Photometry Data Set
Authors: Sangho Choi, Hong-Kyu Moon, Dong-Goo Roh, Min-Su Shin, Myung-Jin Kim, Young-Jong Sohn
Figure caption: Clustering diagrams for asteroids classified by the FGMM with a probability threshold of 0.7.
Paper: Strong Depletion of 13C in CO Induced by Photolysis of CO2 in the Martian Atmosphere, Calculated by a Photochemical Model 
Authors: Tatsuya Yoshida, Shohei Aoki, Yuichiro Ueno, Naoki Terada, Yuki Nakamura, Kimie Shiobara, Nao Yoshida, Hiromu Nakagawa, Shotaro Sakai, Shungo Koyama
Figure caption: (a) Synthetic spectra of a solar occultation measurement by TGO/NOMAD, taken with diffraction order 186. The calculations are performed using the Asimut radiative transfer and retrieval code (Vandaele et al. 2006). The simulation is made for a measurement at 26 km over the northern polar region (latitude: 82°N) at Ls = 165°. The atmospheric condition is obtained from GEM-Mars (Daerden et al. 2019). The CO volume mixing ratio at 26 km is assumed to be 776 ppm. The differences in color represent the assumed isotopic ratios for the 13CO lines (blue: δ 13C = −400‰; light blue: δ 13C = −200‰; black: δ 13C = 0‰; orange: δ 13C = +200‰; and red: δ 13C = 400‰). The rest of the strong features are due to 12CO. The upper panel shows the whole spectral range of order 186, while the small panel below is for a limited spectral range that contains both 12CO and 13CO lines. The typical S/N of a single NOMAD spectrum is more than 1000, which suggests that the strong depletion of 13C presented by this study may be observed with TGO/NOMAD. (b) Synthetic spectra of a measurement by IRTF/iSHELL, taken with diffraction order 215 in the K3 band. The calculations are performed using the online version of PSG (Villanueva et al. 2018). In the calculation, a typical atmospheric condition at the Mars equatorial regions (the volume mixing ratio of CO is 700 ppm) is assumed. The lower panel shows the features due to CO2 (the black curve), H2O (the dark yellow curve), 12C16O (the dark green curve), 13C16O (the purple curve), and 12C18O (the light green curve). The expected telluric transmittance at the Maunakea observatory (where the IRTF telescope is located) is presented as the dotted dotted curve. The small panel above shows the 13C16O lines at 4 151.97 cm−1 for different isotopic ratios (blue: δ 13C = −400‰; light blue: δ 13C = −200‰; black: δ 13C = 0‰; orange: δ 13C = +200‰; and red: δ 13C = 400‰). The typical S/N of a Mars spectrum taken by IRTF/iSHELL over a few pixels (which corresponds to  0.1″) is more than 100, which suggests that the strong depletion of 13C presented in this study may be also observed by IRTF/iSHELL.
Paper: Strong Depletion of 13C in CO Induced by Photolysis of CO2 in the Martian Atmosphere, Calculated by a Photochemical Model 
Authors: Tatsuya Yoshida, Shohei Aoki, Yuichiro Ueno, Naoki Terada, Yuki Nakamura, Kimie Shiobara, Nao Yoshida, Hiromu Nakagawa, Shotaro Sakai, Shungo Koyama
Figure caption: (a) Profiles of the eddy diffusion coefficient and the molecular diffusion coefficient. The solid blue line represents the profile of the eddy diffusion coefficient under the standard setting (the “Standard case”), while the dashed blue line represents that 10 times as small as the standard setting (the “Low eddy case”). The dotted orange, red, and pink lines represent the profiles of the molecular diffusion coefficients of O, H2, and H, respectively. (b) Profiles of the carbon isotopic ratios in CO and CO2, depending on the magnitude of the eddy diffusion coefficient. The isotopic ratios are expressed by the deviation of the calculated ratio with respect to the standard ratio in units per mil: ﹩{\delta }^{13}{\rm{C}}=\left(\tfrac{R}{{R}_{s}}-1\right)\times 1000﹩, where R is the 13C/12C ratio and R  s  = 1.123 × 10−2. The solid lines and dashed lines show the results under the standard eddy diffusion setting and those under the eddy diffusion coefficient 10 times as small as the standard setting, respectively. The orange lines and red lines represent the carbon isotopic ratios in CO and CO2, respectively. The dotted orange line is the same as that in Figure 2, which represents the isotopic ratio of CO on the assumption of the local photochemical equilibrium.
Paper: Strong Depletion of 13C in CO Induced by Photolysis of CO2 in the Martian Atmosphere, Calculated by a Photochemical Model 
Authors: Tatsuya Yoshida, Shohei Aoki, Yuichiro Ueno, Naoki Terada, Yuki Nakamura, Kimie Shiobara, Nao Yoshida, Hiromu Nakagawa, Shotaro Sakai, Shungo Koyama
Figure caption: Profiles of the carbon isotopic ratios in CO and CO2. The isotopic ratios are expressed by the deviation of the calculated ratio with respect to the standard ratio, in units per mil: ﹩{\delta }^{13}{\rm{C}}=\left(\tfrac{R}{{R}_{s}}-1\right)\times 1000﹩, where R is the 13C/12C ratio and R  s  = 1.123 × 10−2. The solid orange line and the solid red line represent the carbon isotopic ratios in CO and CO2, respectively. The dotted orange line represents the ratio of the photolysis rate of 13CO2 to that of 12CO2, which approximates the isotopic ratio of CO, when assuming the local photochemical equilibrium without vertical transport.
Paper: Strong Depletion of 13C in CO Induced by Photolysis of CO2 in the Martian Atmosphere, Calculated by a Photochemical Model 
Authors: Tatsuya Yoshida, Shohei Aoki, Yuichiro Ueno, Naoki Terada, Yuki Nakamura, Kimie Shiobara, Nao Yoshida, Hiromu Nakagawa, Shotaro Sakai, Shungo Koyama
Figure caption: (a) Profiles of the photon flux with wavelength at each altitude. (b) Absorption cross sections of 12CO2 and 13CO2 with wavelength. The black and red lines represent the absorption cross sections of 12CO2 and 13CO2, respectively. (c) The relative difference of the absorption cross sections between 12CO2 and 13CO2: ﹩({\sigma }_{{}^{13}{\mathrm{CO}}_{2}}﹩/﹩{\sigma }_{{}^{12}{\mathrm{CO}}_{2}}-1)\times 1000﹩, where ﹩{\sigma }_{{}^{12}{\mathrm{CO}}_{2}}﹩ and ﹩{\sigma }_{{}^{13}{\mathrm{CO}}_{2}}﹩ are the absorption cross sections of 12CO2 and 13CO2, respectively. Here, the relative difference is averaged over a Gaussian window with FWHMs of 2.5 nm, as done by Schmidt et al. (2013).
Paper: Strong Depletion of 13C in CO Induced by Photolysis of CO2 in the Martian Atmosphere, Calculated by a Photochemical Model 
Authors: Tatsuya Yoshida, Shohei Aoki, Yuichiro Ueno, Naoki Terada, Yuki Nakamura, Kimie Shiobara, Nao Yoshida, Hiromu Nakagawa, Shotaro Sakai, Shungo Koyama
Figure caption:  13C/12C ratio relative to the initial value in the whole atmosphere as a function of the fraction of gas lost to space for each fractionation factor, for the standard eddy diffusion coefficient setting (the “Standard case”), the eddy diffusion coefficient 10 times as small as the standard setting (the “Low eddy case”), the eddy diffusion coefficient 10 times as large as the standard setting (the “High eddy case”), and the setting of Hu et al. (2015; “Hu et al., 2015”), respectively. The dotted black line represents the 13C/12C ratio of the present Martian atmosphere relative to that of the mantle-degassed CO2 derived from the magmatic component of the SNC meteorites (Hu et al. 2015).
Paper: Strong Depletion of 13C in CO Induced by Photolysis of CO2 in the Martian Atmosphere, Calculated by a Photochemical Model 
Authors: Tatsuya Yoshida, Shohei Aoki, Yuichiro Ueno, Naoki Terada, Yuki Nakamura, Kimie Shiobara, Nao Yoshida, Hiromu Nakagawa, Shotaro Sakai, Shungo Koyama
Figure caption: Number density profiles of each chemical species.
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: (a) DEM of our study area (see red polygon in Figure 2 for specific location on Tethys). The locations of where profiles were extracted are shown in black (lines a–f). Ithaca Chasma exhibits raised rims in this region (high-elevation topography colored red and orange in the DEM), which are indicative of flexure. The associated topography along each line is shown in Figure 5. See Figure 1(c) for the Cassini ISS image that covers this region. (b) Estimated elastic thicknesses in our study area (Table 2). The stars are labeled to show the associated profile line. (c) Estimated heat fluxes across our study area for d: 1 mm for pure H2O ice without porosity. The range of heat flux estimates shown here accounts for the range of elastic thickness estimates shown in panel (b). See Figure A1 for estimates assuming porosity. (d) Estimated heat fluxes for d: 1 mm for pure H2O ice mixed with NH3-hydrates. Because we find little evidence for ammonia hydrates on Tethys in ground-based spectra collected by SpeX (see Section 3), we find that our estimates that assume a pure H2O ice lithosphere (panel (c)) are likely more accurate. See Figure A2 for estimates assuming porosity. Grain size (d) was set to 1 mm in order to compare our results to other heat flux estimates for Ithaca’s north limb that incorporated this grain size in their calculations (Giese et al. 2007). See Tables A2–A5 for heat flux estimates that assume d: 0.1 mm.
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: Annotated version of the geologic map presented in Stephan et al. (2010). The underlying Cassini ISS image mosaic is provided in Roatsch et al. (2009). The locations of the study areas for this work (red polygon) and past work that investigated heat fluxes are shown (Giese et al. 2007; White et al. 2017). See Figure 3 for ground-based spectra collected at locations 4–7 (green stars). Spectra for all 10 locations are available as data behind the figure for Figure 3. See Figure 4(a) for specific profile line locations and the DEM of our study area.
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: Disk-integrated, ground-based SpeX spectra of Tethys (dark blue) and 1σ uncertainties (gray error bars), collected over a range of subobserver longitudes (listed on the right with the same spectrum numbers shown in Figure 2 (central locations marked by green stars) that cover the study area reported here, normalized to unity between 1.74 and 1.77 μm and offset vertically for clarity. These data have been resampled to depict their native spectral resolutions (R ∼ 750 at 2.2 μm), whereas their uncertainties are not resampled. The light-blue zone highlights the wavelength range where the Tethys spectra show subtle features that might result from NH3-bearing species. Binned versions of the spectra, simulating the 0.0166 μm channel spacing of VIMS (black), are shown directly below each spectrum, demonstrating that VIMS could not detect the weak features seen in the SpeX data. The Tethys spectra are compared to an atmospheric transmission model for Maunakea that has been resampled to the spectral resolution of SpeX (orange line), demonstrating that Earth’s atmosphere is relatively transparent across the wavelengths covered by the light-blue zone, except for a weak methane gas feature centered at 2.20 μm. The ground-based spectra for all 10 locations shown in Figure 2 are available as data behind the figure.(The data used to create this figure are available.)
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: Portions of Cassini ISS images showing major geologic features on Tethys (Tethys diameter (D): 1062 km). (a) The southern (left) and equatorial (right) portion of Ithaca Chasma and impact structures including Demodocus (D: 125 km), Aietus (D: 91 km), and Telemus (D: 320 km), located on Tethys’s Saturn-facing hemisphere (Image N1589080846_1, 1098 m pixel−1). (b) The equatorial (bottom left) and northern (top right) regions of Ithaca Chasma (Image N1558912068_3, 775 m pixel−1). (c) The region of Ithaca Chasma covered in our study area (see Figure 4(a) for the DEM of the study area) (Image N1716184384_1, 567 m pixel−1). (d) Odysseus (D: 445 km), the largest impact basin on Tethys, located in the northern leading hemisphere (Image N1644802495_1, 1062 m pixel−1). (e) Tethys’s trailing hemisphere, showing Penelope (D: 207.5 km), Phemius (D: 75.9 km), Polyphemus (D: 73 km), Ajax (D: 88 km), and Antinuous (D: 138 km) impact structures (Image N1634217061_1, 769 m pixel−1).
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: Timeline of Tethys’s possible heat flux history. Ranges of modeled (absolute) ages for Ithaca Chasma and Odysseus, estimated assuming a lunar-like cratering chronology, are reported in Giese et al. (2007) and Kirchoff & Schenk (2010) (see Section 1.2 for details). The bordered boxes (Ithaca and Odysseus) represent the range of possible formation periods on the x-axis. The order of events is based on both absolute (bordered boxes only) and relative (nonbordered boxes) age estimates. Relative impact basin ages based on crater densities on their floors were analyzed by White et al. (2017). However, the relative ages between some basins that were near crater saturation (gray dashed line) are indistinguishable (White et al. 2017). These crater saturated basins include Telemus, Dolius, Anticleia, and Penelope. Therefore, here we utilized crater degradation states and geologic mapping (Stephan et al. 2016) to distinguish between the relative ages of these crater saturated basins. Antinous, Melanthius, and Odysseus are not crater saturated and therefore were relative age dated based on crater counts (White et al. 2017). Although Penelope and Antinous exhibit the same geologic unit (b2), Penelope is crater saturated and therefore is likely older than Antinous, which is not crater saturated (White et al. 2017). The geologic unit descriptions associated with basin (b1 and b2) and crater (c1) degradation states are shown in Figure 2 (see Stephan et al. 2016 for more details).
Paper: Tethys’s Heat Fluxes Varied with Time in the Ithaca Chasma and Telemus Basin Region
Authors: Chloe B. Beddingfield, Richard J. Cartwright, Sierra N. Ferguson, Erin J. Leonard
Figure caption: Ranges of estimated heat fluxes for icy bodies throughout the solar system assuming lithospheres without porosity and composed of pure H2O ice. Estimates are provided for Tethys for the Ithaca Chasma south limb (this work), Ithaca Chasma north limb (Giese et al. 2007), and various impact basins (White et al. 2017). For other 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. 2021), Dione (Hammond et al. 2013; White et al. 2017), Rhea (Nimmo et al. 2010; White et al. 2013), and Iapetus (White et al. 2013). In the Jovian system, heat flux estimates are provided for Europa (Hussmann et al. 2002; Nimmo & Manga 2002; Ruiz & Tejero 2003; Tobie et al. 2003; Showman & Han 2004; Ruiz 2005) and Ganymede (Nimmo et al. 2002; Nimmo & Pappalardo 2004; Bland et al. 2017). In the Uranian system, heat flux estimates are provided for Miranda (Beddingfield et al. 2015a, 2022b) and Ariel (Peterson et al. 2015; Beddingfield et al. 2022a). In the Neptunian system, heat flux estimates are provided for Triton (Ruiz 2003; Sori 2021). In the Pluto system, heat flux estimates are provided for Pluto (Conrad et al. 2019, 2021) and Charon (Conrad et al. 2021).