adsabs/AstroCLIMB huggingface dataset:
Paper: Fitting the Light Curve of 1I/‘Oumuamua with a Nonprincipal Axis Rotational Model and Outgassing Torques
Authors: Aster G. Taylor, Darryl Z. Seligman, Olivier R. Hainaut, Karen J. Meech
Figure caption: An ensemble of torque models, sampled from a multivariate Gaussian distribution centered around the optimal parameter values with means and standard deviations given by Table 1. They are plotted vs. the photometric data (gray points) taken in 2017 October (first and third rows) and 2017 November (second and fourth rows). The curves (in the first two rows) are the optimal fit, and the gray curves are the sampled ensemble. Both the CO84 (red, Equation (18)) and the ML15 (blue, Equation (23)) model light-curves are plotted, in the first two and last two rows, respectively. The x-axis scales for the 2017 October and 2017 November data are different. It should be noted that the “optimal fit” is not optimal for the 2017 November data. The time axis has units of days, with a zero point at 58,000 MJD.
Paper: Fitting the Light Curve of 1I/‘Oumuamua with a Nonprincipal Axis Rotational Model and Outgassing Torques
Authors: Aster G. Taylor, Darryl Z. Seligman, Olivier R. Hainaut, Karen J. Meech
Figure caption: Rotation period for ‘Oumuamua over its trajectory, plotted vs. heliocentric distance. Both optimal parameter sets (Table 1) are shown. Because the timescale of the trajectory (∼5 yr) is significantly longer than the ∼1 hr scale modulation effect of the outgassing torques, we present the daily average of the period rather than its instantaneous value. We show the rotation state over the entire trajectory within 15 au inbound and outbound (top panel) and a zoom-in between perihelia and when the Spitzer observations occurred at ∼2 au (bottom panel). The zoom-in is shown on the top panel by a gray highlight. The first photometric observations were obtained when the object was at ∼1.35 au, denoted with a vertical dashed line in the second panel.
Paper: Fitting the Light Curve of 1I/‘Oumuamua with a Nonprincipal Axis Rotational Model and Outgassing Torques
Authors: Aster G. Taylor, Darryl Z. Seligman, Olivier R. Hainaut, Karen J. Meech
Figure caption: Best-fit synthetic light curves (red line) and photometric data (gray points) for a torque-free model, using the CO84 light-curve model. The data shown are those taken in 2017 October only. The parameters for the model are given in Table 2. The time is given in days, with a zero point at 58,000 MJD.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: The total number of detectable ISOs per year. The top and bottom panels show this number when the effects of trailing loss are included and excluded, respectively. The detectability criterion requires at least three detections in the synthetic LSST frames. The trailing loss depends on the exposure time and FWHM. Here we adopt a 0.″7 for FWHM and 30 s exposure time, as given in Jones et al. (2018). We cut the albedo axis at 0.6 because the number of asteroids expected beyond this value is considered negligible (Mainzer et al. 2012).
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: The apparent rate of sky motion of ISOs as a function of the SFD slope. The three panels correspond to three assumed albedos for each object in the synthetic populations. The rates of motion are orders of magnitude higher than for typical solar system objects.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: Examples of sky paths of synthetic detectable objects (top panel). The individual points show individual detections with the OIF simulation. We show one zoomed-in region (indicated in the top panel in the dashed circular region) including a synthetic ISO path with six detections (bottom panel). These plots are obtained assuming an SFD of −2.5 (an intermediate value), albedo of 0.1 (conservative), and O/B kinematics.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: The perihelion distance (top), eccentricity (middle), and inclination (bottom) of detectable ISOs. The underlying population has an SFD slope of −3, and each object has an albedo of 0.1. We show the distributions for the entire population without the detectability constraints (blue filled) and for cases where the albedo is 0.1 (red open), 0.5 (blue open), and 1.0 (black open).
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: Same as Figure 2, but for the acceleration of the sky motion. We only show the absolute value of the apparent acceleration because the sign does not impact the detectability.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: The distribution of geocentric distance of detectable ISOs when they attain maximum brightness.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: The distribution of arc length during which a synthetic ISO is detectable.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: The amount of time an ISO spends inside of the 5 au sphere for O/B kinematics. This distribution is for the entire population and is not filtered by detectable objects.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: The amount of time a detectable ISO spends inside of the 5 au sphere for a range of albedo and SFD slope.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: The distribution of the diameters of synthetic ISOs detectable with the LSST.
Paper: Synthetic Detections of Interstellar Objects with the Rubin Observatory Legacy Survey of Space and Time
Authors: Dušan Marčeta, Darryl Z. Seligman
Figure caption: Mean and median diameter of detectable objects.
Paper: Investigation of Titan’s South Polar HCN Cloud during Southern Fall Using Microphysical Modeling
Authors: Lavender E. Hanson, Darryn Waugh, Erika Barth, Carrie M. Anderson
Figure caption: Atmosphere and cloud variables from L s = 12.°4 to 92.°5 of the 16th Titan year of the simulation: (a) temperature, (b) HCN vapor mixing ratio, (c) HCN particle number mixing ratio, (d) HCN mass mixing ratio, (e) effective radius of HCN cloud particles, (f) extinction of HCN cloud at 0.889 µm, and (g) HCN supersaturation. The thick black dashed line indicates the descending 110 K isotherm, and the thick black dotted line shows the minimum temperature altitude. Vertical black dotted lines indicate L s = 24°, 30°, 36°, 45°, and 65°. Other contours are indicated in the figure legends.
Paper: Investigation of Titan’s South Polar HCN Cloud during Southern Fall Using Microphysical Modeling
Authors: Lavender E. Hanson, Darryn Waugh, Erika Barth, Carrie M. Anderson
Figure caption: Profile plots of (a) temperature, (b) vapor volume mixing ratio, (c) number mixing ratio, (d) mass mixing ratio, (e) effective radius, (f) extinction at 0.889 µm, and (g) supersaturation from the same simulation as Figure 3 at L s = 24°, 30°, 36°, 45°, 65°, and 90°.
Paper: Investigation of Titan’s South Polar HCN Cloud during Southern Fall Using Microphysical Modeling
Authors: Lavender E. Hanson, Darryn Waugh, Erika Barth, Carrie M. Anderson
Figure caption: Temperature profiles constructed by subtracting a Gaussian function centered at 300 km. The initial interpolated temperature profile (Teanby et al. 2019) is shown in green. The minimum temperatures of the modified profiles are 97 K (ΔT = 50 K), 107 K (ΔT = 40 K), and 115 K (ΔT = 30 K), while the temperatures at 300 km are 99, 108, and 118 K. The dashed–dotted lines in (b) and (c) are the modeled Nmr  and reff  using the initial temperature profile with f = f 0 (blue) and f = 10 × f 0 (green). Ranges of observed values of N mr and r eff are shaded.
Paper: Investigation of Titan’s South Polar HCN Cloud during Southern Fall Using Microphysical Modeling
Authors: Lavender E. Hanson, Darryn Waugh, Erika Barth, Carrie M. Anderson
Figure caption: Polar temperature profiles throughout a Titan year for ΔT = 50 K. The dotted lines represent intermediate temperature profiles constructed as described in the text, and the dashed line represents the unmodified L s = 30° profile (ΔT = 0 K).
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: Images extracted from the LROC quickmap interface for study areas I (left column) and II (right column) display, from top to bottom and left to right, LRO WAC albedo and olivine, clinopyroxene, orthopyroxene, and plagioclase abundances. The mineral abundances are from Lemelin et al. (2018).
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: Simulated maximum dust levitation heights over a range of dust sizes from 0.05 to 100 μm launched off the lunar surface at an angle of 45°. Feldspathic highland crust and high-Ti basalt are considered with densities of 2870 and 3460 kg m−3, respectively.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: Images extracted from the LROC quickmap interface for study areas I (left column) and II (right column) display, from top to bottom, LRO Wide Angle Camera (WAC) albedo, FeO abundance, and OMAT values. The FeO and OMAT values are from Lemelin et al. (2018).
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: Cumulative distributions for each of the minerals and the OMAT parameter in the spectral analyses.
Paper: The Variability of Lunar Mare Basalt Properties from Surface Rock Abundance
Authors: Catherine M. Elder, Rebecca R. Ghent, James Haber, Paul O. Hayne, Gareth Morgan, Mark S. Robinson, Matt Siegler, Jean-Pierre Williams
Figure caption: Example histograms of the rock abundance values in one of the most rocky (top left, median RA = 0.0062) and least rocky (top right, median RA = 0.0028) units (note the different axes). The Hiesinger et al. (2011) unit and the number of Diviner pixels, N, are indicated on the plots. The bottom-left histogram is the same region as the histogram in the top left, truncated to RA < 0.1, where the values in blue include all pixels in the region, and the values in pink are those associated with the ejecta blanket of a young crater (40.79°W, 24.04°S, D = 5.5 km). The rock abundance map on the bottom right shows the region and the crater ejecta blanket outlined in magenta.
Paper: The Variability of Lunar Mare Basalt Properties from Surface Rock Abundance
Authors: Catherine M. Elder, Rebecca R. Ghent, James Haber, Paul O. Hayne, Gareth Morgan, Mark S. Robinson, Matt Siegler, Jean-Pierre Williams
Figure caption: Difference between the median rock abundance of each individual unit defined by Hiesinger et al. (2011) and the overall median rock abundance of all of the maria included in the study by Hiesinger et al. (2011). Negative values indicate units which are less rocky than the median rock abundance of the maria.
Paper: The Variability of Lunar Mare Basalt Properties from Surface Rock Abundance
Authors: Catherine M. Elder, Rebecca R. Ghent, James Haber, Paul O. Hayne, Gareth Morgan, Mark S. Robinson, Matt Siegler, Jean-Pierre Williams
Figure caption: Median rock abundance value in each map unit defined by Morgan et al. (2016) vs. the map unit number, where 1 is the oldest and 4 is the youngest.
Paper: The Variability of Lunar Mare Basalt Properties from Surface Rock Abundance
Authors: Catherine M. Elder, Rebecca R. Ghent, James Haber, Paul O. Hayne, Gareth Morgan, Mark S. Robinson, Matt Siegler, Jean-Pierre Williams
Figure caption: Median (top left), mean (center left), and 95th percentile (bottom left) rock abundance, and median (top right), mean (center right), and 95th percentile (bottom right) H-parameter all vs. unit age for all of the Hiesinger et al. (2011) count areas.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Schematic diagram of the model developed in this work. Arrows pointing in and out of the free reservoir are sources and sinks of atmospheric species. This model tracks the abundance of each species and its isotopic composition in the free reservoir.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Estimated volcanic outgassing rates of H2. The conditions that yield maximum outgassing rates are oxygen fugacity at IW-1, H2O concentration in the magma of 2000 ppm, and an outgassing multiplier of 2. The conditions that yield minimum outgassing rates are oxygen fugacity at IW, H2O concentration in the magma of 100 ppm, and an outgassing multiplier of 0.5. We test the volcanic profile derived for the baseline case (Hartmann 2005) and the variant (Ivanov 2001).
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Posterior distributions for atmospheric composition at 3.8 Ga and model parameters in the baseline MCMC solutions. The posterior distributions are reported for discrete values of the amount of CO2 deposited in carbonate minerals before 3.5 Ga, C-DEP = 300, 900, and 1400 mbar. (a) The distributions of pCO2 at 3.8 Ga have medians (and 95% confidence intervals) of 357 (334–373), 977 (950–1000), and 1486 (1453–1513) mbar, respectively. (b) For p N2 at 3.8 Ga: 299 (182–522), 192 (119–348), and 159 (97–302) mbar. (c) For p Ar at 3.8 Ga: 0.35 (0.23–0.51), 0.35 (0.23–0.50), and 0.34 (0.21–0.48) mbar. (d)–(l) See Table 1 for parameter descriptions.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: 100 randomly sampled solutions for each value of C-DEP from the baseline MCMC. The plotted data are slightly transparent for visibility. The solutions are shown with discrete values of the amount of CO2 deposited in carbonate minerals before 3.5 Ga, C-DEP = 300, 900, and 1400 mbar. Note that panels (a), (b), and (c) have a logarithmic X-axis. In panel (d), f col is the fraction of time the atmosphere is in the collapsed state for a given time step (see Section 2.2).
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Representative model solution from the baseline MCMC. Parameter values for this solution are shown at the top right. (a) Evolution of partial pressures. Modern value ranges are shown by the brackets. At 3.8 Ga, pCO2 = 982 mbar, pN2 = 250 mbar, and pAr = 0.33 mbar. (b) Evolution of the isotopic composition. Modern values with 3σ uncertainty are shown by the brackets. (c)–(e) Evolution of the fluxes from sources and sinks of each species. All fluxes are shown as positive values for clarity. In reality, sputtering, photochemical loss, ion loss, carbonate deposition, and nitrate deposition are negative fluxes. The total mass lost or gained over the entire evolution for a given process is shown next to its name in the legends.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Posterior distributions for atmospheric composition at 3.8 Ga and model parameters in the extended range MCMC solutions. The posterior distributions are reported for discrete values of the amount of CO2 deposited in carbonate minerals before 3.5 Ga, C-DEP = 300, 900, and 1400 mbar. (a) The distributions of pCO2 at 3.8 Ga have medians (and 95% confidence intervals) of 290 (260–334), 900 (861–949), and 1412 (1364–1475) mbar, respectively. (b) For pN2 at 3.8 Ga: 7.33 (3.71–13.02), 7.00 (3.43–13.75), and 5.45 (2.35–10.12) bar. Note the large scale of the x-axis. (c) For pAr at 3.8 Ga: 0.134 (0.028–0.300), 0.094 (0.009–0.264), and 0.149 (0.040–0.311) mbar. (d)–(i) See Table 1 for parameter descriptions.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Representative model solution from the variant case where carbonate deposition occurred in shallow subsurface aquifers (SSAs). This case has 50 mbar of carbonate deposition before 3 Ga. Parameter values for this solution are shown at the top right. (a) Evolution of partial pressures. Modern value ranges are shown by the brackets. At 3.8 Ga, pCO2 = 125 mbar, pN2 = 142 mbar, and pAr = 0.54 mbar. (b) Evolution of the isotopic composition. Modern values with 3σ uncertainty are shown by the brackets. (c)–(e) Evolution of the fluxes from sources and sinks of each species. All fluxes are shown as positive values for clarity. In reality, sputtering, photochemical loss, ion loss, carbonate deposition, and nitrate deposition are negative fluxes. The total mass lost or gained over the entire evolution for a given process is shown next to its name in the legends.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Atmospheric composition at 3.8 Ga as a function of early carbonate deposition (C-DEP) in the baseline MCMC. The circular markers are the median values from the baseline MCMC posterior distributions. The dark shaded regions are 50% confidence intervals, and the light shaded regions are 95% confidence intervals. pTOT is defined as the sum of pCO2, pN2, and pAr in a model run.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Posterior distributions for atmospheric composition at 3.8 Ga and model parameters in the variant MCMC solutions. All posteriors have an amount of carbonate deposition before 3.5 Ga (C-DEP) of 900 mbar. More information on the variant scenarios is shown in Table 2.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Evolution of N2 in 100 randomly sampled solutions from the extended range MCMC. The plotted data are slightly transparent for visibility. The solutions are shown with discrete values for the amount of CO2 deposited in carbonate minerals before 3.5 Ga, C-DEP = 300, 900, and 1400 mbar.
Paper: Constraints on the Size and Composition of the Ancient Martian Atmosphere from Coupled CO2–N2–Ar Isotopic Evolution Models
Authors: Trent B. Thomas, Renyu Hu, Daniel Y. Lo
Figure caption: Energy distribution of carbon atoms produced by the photodissociation of CO2 in Mars’s upper atmosphere. The required energies to escape Mars’s gravity for the carbon isotopes are shown by the dashed lines. The shaded regions represent the portion of carbon isotopes that are ejected from Mars’s atmosphere.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Ordinary Chondrite and HED Meteorites
Authors: Bryn Bowen, Vishnu Reddy, Mario De Florio, Theodore Kareta, Neil Pearson, Roberto Furfaro, Benjamin Sharkey, Allison McGraw, David Cantillo, Juan A. Sanchez, Adam Battle
Figure caption: Near-infrared spectra of different grain sizes of the ordinary chondrites H chondrite El Hammami, L chondrite Viñales, and LL chondrite Chelyabinsk. The left column spectra are plotted in absolute reflectance, and the right column spectra are normalized at 1.4 μm. All three meteorites exhibit a general trend of absolute reflectance decreasing as grain size increases, although there is some overlap between El Hammami’s two largest grain size bins and Viñales’ and Chelyabinsk’s 150–300 and 300–500 μm bins.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Ordinary Chondrite and HED Meteorites
Authors: Bryn Bowen, Vishnu Reddy, Mario De Florio, Theodore Kareta, Neil Pearson, Roberto Furfaro, Benjamin Sharkey, Allison McGraw, David Cantillo, Juan A. Sanchez, Adam Battle
Figure caption: Plots of the Band I and II centers and BAR vs. grain size for the ordinary chondrites H chondrite El Hammami, L chondrite Viñales, and LL chondrite Chelyabinsk. The BAR is the ratio of the Band II area to the Band I area. The errors are smaller than the symbols, but they are reported in the tables.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Ordinary Chondrite and HED Meteorites
Authors: Bryn Bowen, Vishnu Reddy, Mario De Florio, Theodore Kareta, Neil Pearson, Roberto Furfaro, Benjamin Sharkey, Allison McGraw, David Cantillo, Juan A. Sanchez, Adam Battle
Figure caption: Comparison between the reflectance modeled via the Hapke model and the reflectance measured in the lab (top) and the values of their χ 2 error (bottom).
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Ordinary Chondrite and HED Meteorites
Authors: Bryn Bowen, Vishnu Reddy, Mario De Florio, Theodore Kareta, Neil Pearson, Roberto Furfaro, Benjamin Sharkey, Allison McGraw, David Cantillo, Juan A. Sanchez, Adam Battle
Figure caption: Simulated SSA from the Hapke model against the particle sizes with polynomial regression for the Camel Donga meteorite.
Paper: Grain Size Effects on Visible and Near-infrared (0.35–2.5 μm) Laboratory Spectra of Ordinary Chondrite and HED Meteorites
Authors: Bryn Bowen, Vishnu Reddy, Mario De Florio, Theodore Kareta, Neil Pearson, Roberto Furfaro, Benjamin Sharkey, Allison McGraw, David Cantillo, Juan A. Sanchez, Adam Battle
Figure caption: Optimized Hapke model parameters ω, b, and c for the Camel Donga meteorite for all grain sizes.