adsabs/AstroCLIMB huggingface dataset:
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Diameter vs. pseudo-temperature T 1 for 4685 cases calculated from a two-band (W3–4) and four-band (W1–4) reparameterized NEATM model. Each point represents the median diameter and pseudo-temperature value among all accepted bootstrap trials for an object, while error bars represent the standard deviations of the diameter and pseudo-temperature values among accepted bootstrap trials. The W3–4 data shown in this figure are available as the data behind the figure. The data also includes additional information that will allow the reader to recreate Figures 10–12. (The data used to create this figure are available.)
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Histograms of the relative difference and absolute value of the relative difference. Median values are represented with a vertical black line, while a pink highlighted block is used to represent the 5%–95% quantile range. Top left: relative difference in diameter. Top right: relative difference in pseudo-temperature. Bottom left: absolute value of relative difference in diameter. Bottom right: absolute value of relative difference in pseudo-temperature.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Best-fit pseudo-temperature and diameter for 200 bootstrap trials for example asteroid 10006. The median is shown as a red dot, with corresponding parameter values displayed in the legend. Standard deviations in diameter and pseudo-temperature among the bootstrap trials are displayed below the legend. Left: results from two-band modeling. Right: results from four-band modeling, where we replicate the results from Myhrvold et al. (2022) with the same set of observational clusters but a different set of random bootstrap trials.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Histogram of visible-band geometric albedos (p  v ) as calculated using the median modeled diameter for each cluster and the absolute magnitude for the object, H. The median albedo for the two-band fits is shown as a dark red line, while the median albedo of the four-band fits is shown as a dark blue line.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Histogram of visible-band geometric albedos (p  v ) as calculated using the median modeled diameter for each cluster and the absolute magnitude for the object H. The median albedo for the two-band fits is shown as a dark green line, while the median albedo of the four-band fits is shown as a dark blue line.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Histograms of D and T 1 parameter relative uncertainty, i.e., the standard deviation in accepted bootstrap trials for an object divided by the median value of the bootstrap trials. The median of the relative uncertainties for all objects is shown as a vertical line. Two-band results are shown in red whereas four-band results are shown in blue. Left: relative uncertainty in diameter. Right: relative uncertainty in pseudo-temperature T 1.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Histograms of relative uncertainty, where relative uncertainty represents the standard deviation in accepted bootstrap trials for an object divided by the median value of the bootstrap trials. The median of the relative uncertainty for all objects is shown as a vertical line. Two-band results are shown in green, while four-band results are shown in blue. Left: relative uncertainty in diameter. Right: relative uncertainty in pseudo-temperature.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Left: plot of NEOWISE four-band diameters vs. our corresponding two-band (W2–3) modeled diameters. The orange line represents a perfect one-to-one ratio between diameters. The color bar indicates our pseudo-temperature modeled with W2 and W3. Right: plot of NEOWISE two-band (W2–3) diameters vs. our corresponding two-band (W2–3) modeled diameters.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Plot of occultation diameters vs. our corresponding two-band (W2–3) modeled diameters. The orange line represents a perfect one-to-one ratio between diameters whereas the black dotted lines represent a 10% error in the positive and negative directions.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Histograms of the relative difference and absolute value of the relative difference in D and T 1 parameter estimates. Median values are represented with a vertical black line, while a pink highlighted block is used to represent the 5%–95% quantile range. Top left: relative difference in diameter. Top right: relative difference in pseudo-temperature T 1. Bottom left: absolute value of relative difference in diameter. Bottom right: absolute value of relative difference in pseudo-temperature T 1.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Comparison of results from two-band W2–3 fits to results from four-band fits with ϵ fixed to 0.9. Left: diameter vs. pseudo-temperature T 1 for 4533 clusters. Each point represents the median diameter and pseudo-temperature value among all accepted bootstrap trials for an object, while error bars represent the standard deviations of the diameter and pseudo-temperature values among accepted bootstrap trials. Middle: histogram of the relative difference in diameter. Median values are represented with a vertical black line, while a pink highlighted block is used to represent the 5%–95% quantile range. Right: histogram of relative difference in pseudo-temperature.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Comparison of results from Myhrvold et al. (2022) four-band fits to results from four-band fits with ϵ fixed to 0.9. Left: diameter vs. pseudo-temperature T 1 for 4672 clusters. Each point represents the median diameter and pseudo-temperature value among all accepted bootstrap trials for an object, while error bars represent the standard deviations of the diameter and pseudo-temperature values among accepted bootstrap trials. Middle: histogram of the relative differences in diameter. Median values are represented with a vertical black line and the 5%–95% quantile range is represented with a region highlighted in pink. Right: histogram of relative differences in pseudo-temperature.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Histograms of distance from the Sun (left) and phase angle (right) at the time of observations. The blue bars represent all observational clusters, while the orange bars represent clusters that had a low median pseudo-temperature (T 1 < 273 K) from the two-band bootstrapped fits, before implementation of our low-temperature-solution removal process.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Plot of occultation diameters vs. our corresponding diameters modeled with W3 and W4. Red points represent objects with a higher-quality occultation diameter with a quality code of 3, while green objects have a slightly lower-quality occultation diameter with a quality code of 2. The orange line represents a perfect one-to-one ratio between diameters, while black dotted lines represent a 10% error in the positive and negative directions.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Left: histogram of emissivity values obtained with the floating-emissivity model and W2–3. Right: diameter vs. pseudo-temperature two-band estimates for the constant-emissivity model and the floating-emissivity model.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Left: plot of NEOWISE four-band diameters vs. our corresponding diameters modeled with W3 and W4. The orange line represents a perfect one-to-one ratio between diameters. The color bar indicates our pseudo-temperature modeled with W3 and W4. Right: plot of NEOWISE two-band (W3–4) diameters vs. our corresponding diameters modeled with W3 and W4.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Reduced chi-squared vs. pseudo-temperature. Pseudo-temperatures and reduced chi-squared values are both represented by the median value of 200 bootstrapped trials. Two-band values are shown in red whereas four-band values are shown in blue.
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: Logarithmic plot of light-curve peak-to-peak amplitude vs. reduced chi-squared for all remaining clusters with a corresponding light-curve fit. W2–3 clusters are shown in red whereas W1–4 clusters are shown in blue. Light-curve amplitudes were obtained from Lam et al. (2023).
Paper: Thermal Models of Asteroids with Two-band Combinations of Wide-field Infrared Survey Explorer Cryogenic Data
Authors: Emily A. Whittaker, Jean-Luc Margot, Adrian L. H. Lam, Nathan Myhrvold
Figure caption: W1–4 flux values vs. asteroid–Sun distance for asteroid 1182. Black points and error bars indicate the WISE fluxes and uncertainties whereas blue lines indicate the best four-band fit to the data. Error bars incorporate the correction factors.
Paper: Ice, Ice, Maybe? Investigating 46P/Wirtanen’s Inner Coma for Icy Grains
Authors: Theodore Kareta, John W. Noonan, Walter M. Harris, Alessondra Springmann
Figure caption: Monte Carlo icy grain model for grain sizes randomly sampled from the size–frequency distribution governed by the α = −5.989 power law. All particles are subject to gravitational force from the comet nucleus, pressure from the expanding coma gas (assumed to be H2O), and solar radiation pressure at 1 au. The plot is 15,000 km by 15,000 km and shown in a logarithmic scale to match the top row of images shown in Figure 1. The model results have been rotated to match the Earth viewing geometry at the time of observation, a phase angle of 18°, and an orbital difference angle of −16°. The general morphology of the model is in agreement with observations shown in Figure 1.
Paper: Ice, Ice, Maybe? Investigating 46P/Wirtanen’s Inner Coma for Icy Grains
Authors: Theodore Kareta, John W. Noonan, Walter M. Harris, Alessondra Springmann
Figure caption: Top row: average images of 46P/Wirtanen normalized and shown on a logarithmic scale in the J, H, and K filters. The images are scaled identically in each row. Middle row: the same J, H, and K images shown after subtraction of an azimuthally averaged radial profile shown on a symmetric-logarithm scale. Bottom row: the ratios between the images taken in each filter shown on a logarithmic scale between 0.3 and 3.0 times the median value in each image, as well as masked in the center, to enhance contrast. The variations are indeed subtle and not a feature of the color map or scaling. Of particular note is the antisunward extension of the dust tail. See text for more details and interpretation.
Paper: Ice, Ice, Maybe? Investigating 46P/Wirtanen’s Inner Coma for Icy Grains
Authors: Theodore Kareta, John W. Noonan, Walter M. Harris, Alessondra Springmann
Figure caption: Spatial profiles extracted along the Sun–comet axis for the filter ratios shown in the bottom row of Figure 1. X-axis values increase toward the Sun, and the Y-axis values were scaled by the median of each profile. Each profile is the average of three 1 pixel wide spatial profiles, including one that runs through the pixel corresponding to the brightest pixels in the original image and two profiles directly adjacent to it. Explanation and interpretation of the trends are in the text, but no unambiguous signs for ice are apparent.
Paper: Ice, Ice, Maybe? Investigating 46P/Wirtanen’s Inner Coma for Icy Grains
Authors: Theodore Kareta, John W. Noonan, Walter M. Harris, Alessondra Springmann
Figure caption: The distribution of MCMC walker values for our four parameters is shown as a corner plot, with each of the two-dimensional plots showing the inferred posterior distributions for each of the parameters against each other, and at the top of each column is the histogram of marginalized values for each of our model parameters. As expected, the areal ice fraction is very low, less than 0.6% at the 99.7% confidence interval, and the ice grain size has a rather odd distribution owing to the poor ability of the data to constrain that mode parameter. The dust grain size–frequency exponent and volumetric vacuum fraction were constrained to ﹩\alpha ={5.989}_{-0.069}^{+0.069}﹩ and ﹩{f}_{\mathrm{vac}}={0.096}_{-0.001}^{+0.001}﹩, respectively, also at the 99.7% confidence interval.
Paper: Ice, Ice, Maybe? Investigating 46P/Wirtanen’s Inner Coma for Icy Grains
Authors: Theodore Kareta, John W. Noonan, Walter M. Harris, Alessondra Springmann
Figure caption: Top: the NIR spectrum of 46P/Wirtanen’s innermost coma is shown as black open circles with error bars, with the maximum likelihood spectral model from the MCMC package emcee shown as a solid red curve. Bottom: the residuals (data − model) are shown as a function of wavelength, with zero shown as a straight red line for reference. The fit is shown to coincide with the data quite well, and as a result, both the model and the data were moved out of normalized reflectance space by scaling both by the modeled geometric albedo at λ = 1.0 μm of approximately ∼0.087. The high-quality fit and the dark visible albedo together combine to suggest that our model is physically reasonable given the information we have available.
Paper: Laboratory Studies of Brine Growth Kinetics Relevant to Deliquescence on Mars
Authors: Raina V. Gough, Danielle L. Nuding, Germán M. Martínez, Edgard G. Rivera-Valentín, Katherine M. Primm, Margaret A. Tolbert
Figure caption: Time needed to fully deliquesce a Ca(ClO4)24H2O grain at Gale Crater, Mars, as a function of the salt particle diameter in microns and the temperature of the salt particle. Solid colored lines are above the eutectic temperature of Ca(ClO4)2, and dashed colored lines are below the eutectic temperature (only metastable deliquescence possible). If only temperatures above the eutectic temperature of Ca(ClO4)2 (197 K) are considered, then only particles <1 μm will be able to fully deliquesce in less than 8 hr, which is the overnight duration of the conditions potentially favorable for deliquescence.
Paper: Laboratory Studies of Brine Growth Kinetics Relevant to Deliquescence on Mars
Authors: Raina V. Gough, Danielle L. Nuding, Germán M. Martínez, Edgard G. Rivera-Valentín, Katherine M. Primm, Margaret A. Tolbert
Figure caption: Normalized particle growth rate on color axis plotted in temperature vs. water vapor pressure space. It can be seen that the growth rate increases with water vapor pressure at constant T (see dotted rectangle) and increases with decreasing T at constant water vapor pressure (see dashed rectangle). Additionally, a comparison of our experimental data (colored circles) vs. the temperature and water vapor pressures measured by MSL REMS (gray crosses) and Phoenix TECP (black plus signs) shows that all span a similar temperature range, but the lab experiments were performed at higher water vapor pressure values.
Paper: Laboratory Studies of Brine Growth Kinetics Relevant to Deliquescence on Mars
Authors: Raina V. Gough, Danielle L. Nuding, Germán M. Martínez, Edgard G. Rivera-Valentín, Katherine M. Primm, Margaret A. Tolbert
Figure caption: Time needed to fully deliquesce a Ca(ClO4)2 particle at the Phoenix landing site as a function of the salt particle diameter in microns and also the temperature of the salt particle. Solid colored lines are above the eutectic temperature of Ca(ClO4)2, and dashed colored lines are below the eutectic temperature (only metastable deliquescence possible). The higher water vapor pressures (∼30% higher) present at the Phoenix landing site compared to MSL result in shorter deliquescence timescales. Still, only particles <2 μm will be able to fully deliquesce in less than 8 hr if only temperatures above the eutectic temperature of Ca(ClO4)2 (198 or 199 K) are considered.
Paper: Laboratory Studies of Brine Growth Kinetics Relevant to Deliquescence on Mars
Authors: Raina V. Gough, Danielle L. Nuding, Germán M. Martínez, Edgard G. Rivera-Valentín, Katherine M. Primm, Margaret A. Tolbert
Figure caption: Values of the net uptake coefficient, γ net, as a function of temperature, plotted here as ln(γ net) vs. 1/T. Every individual γ net value is shown as a small gray circle, and the large black circles represent the averaged γ net values.
Paper: Laboratory Studies of Brine Growth Kinetics Relevant to Deliquescence on Mars
Authors: Raina V. Gough, Danielle L. Nuding, Germán M. Martínez, Edgard G. Rivera-Valentín, Katherine M. Primm, Margaret A. Tolbert
Figure caption: Schematic illustrating the difference between deliquescence and subsequent growth as it occurs in our laboratory experiments (orange rectangle) and may occur on Mars due to lower water vapor availability (blue rectangle). In both cases, however, the experimentally determined value of the net uptake coefficient for water molecules onto a brine surface is likely relevant.
Paper: Laboratory Studies of Brine Growth Kinetics Relevant to Deliquescence on Mars
Authors: Raina V. Gough, Danielle L. Nuding, Germán M. Martínez, Edgard G. Rivera-Valentín, Katherine M. Primm, Margaret A. Tolbert
Figure caption: Typical microscope field of view showing Ca(ClO4)2 particles detected and measured by the LabVIEW particle sizing program. A few smaller particles were present, but they were smaller than our 5 μm cutoff and not studied.
Paper: Laboratory Studies of Brine Growth Kinetics Relevant to Deliquescence on Mars
Authors: Raina V. Gough, Danielle L. Nuding, Germán M. Martínez, Edgard G. Rivera-Valentín, Katherine M. Primm, Margaret A. Tolbert
Figure caption: Normalized particle growth rate plotted as a function of temperature for three water vapor pressure bins spanning 3 orders of magnitude.
Paper: Laboratory Studies of Brine Growth Kinetics Relevant to Deliquescence on Mars
Authors: Raina V. Gough, Danielle L. Nuding, Germán M. Martínez, Edgard G. Rivera-Valentín, Katherine M. Primm, Margaret A. Tolbert
Figure caption: Microscope images of a single Ca(ClO4)2 particle collected at 50× magnification. In this experiment, the relative humidity was increased, while the temperature of the salt sample was held constant at 273 K. The deliquescence phase transition from crystalline to aqueous occurred between 0.1% and 4.6% relative humidity. Then, for the remainder of the experiment, particle growth (water uptake) occurred.
Paper: Mercury's Circumsolar Dust Ring as an Imprint of a Recent Impact
Authors: Petr Pokorný, Ariel N. Deutsch, Marc J. Kuchner
Figure caption: Relative brightness increase of the circumsolar dust ring with respect to the brightness of the ZC. The figure shows the radial (elongation) and azimuthal (STEREO longitude λ) distribution of the brightness increase. Mercury’s aphelion and orbit locations are shown with white dashed lines. Note that the STEREO observation does not capture the entire structure and is limited to ∼23° in elongation and >110° in STEREO longitude λ. The color coding and contours show the asymmetric nature of the dust ring, suggesting an eccentric distribution of dust. The data for this plot were adopted from Figure 3 in Stenborg et al. (2018b).
Paper: Mercury's Circumsolar Dust Ring as an Imprint of a Recent Impact
Authors: Petr Pokorný, Ariel N. Deutsch, Marc J. Kuchner
Figure caption: Panel A: the same as Figure 7(A) but now for our model of the 2P/Encke meteoroid stream. The relative brightness increase reaches its maximum at ϵ = 23° and λ = 114°, which is a favorable location for the portion of the observation that our dust ring model does not reproduce. However, the cometary contribution spans a wide range of longitudes and contributes significantly to regions where our ring model fits the data well. Panel B: a wider extent of the relative brightness increase of our 2P/Encke model. The dust stream is aligned with the longitude of periapsis of 2P/Encke, ϖ = 161°.1. Note that the longitude in this figure is comparable to the heliocentric ecliptic longitude, where λ = λ S/C − 70° reflects the 70° shift due to the observational geometry.
Paper: Mercury's Circumsolar Dust Ring as an Imprint of a Recent Impact
Authors: Petr Pokorný, Ariel N. Deutsch, Marc J. Kuchner
Figure caption: The co-orbital residence time T res with respect to the simulated particle diameter D (orange line with circles). Both x- and y-axes are in logarithmic scale. The greyscale boxes delineate different regimes of T res behavior. We fitted the 1 ≤ D < 10 mm range with a power law (dashed black line), f(x) = x  a 10 b , where x = D is the particle diameter, a is the power of the power law, and b provides the offset.
Paper: Mercury's Circumsolar Dust Ring as an Imprint of a Recent Impact
Authors: Petr Pokorný, Ariel N. Deutsch, Marc J. Kuchner
Figure caption: Panel A: relative brightness increase of the best-fit model of dust originating in 1:1 MMR with Mercury. The plot shows the same region as the Stenborg et al. (2018b) observation (Figure 1) where the x-axis is the solar elongation ϵ and the y-axis is the spacecraft longitude shifted by −70° to account for the observing geometry (see the text for an explanation). Panel B: model residuals of our best-fit model. Our model does not reproduce the relative brightness increase in the bottom right corner of the figure, that can be attributed to dust from comet 2P/Encke.