adsabs/AstroCLIMB huggingface dataset:
Paper: The New Horizons Extended Mission Target: Arrokoth Search and Discovery
Authors: Marc W. Buie, John R. Spencer, Simon B. Porter, Susan D. Benecchi, Alex H. Parker, S. Alan Stern, Michael Belton, Richard P. Binzel, David Borncamp, Francesca DeMeo, S. Fabbro, Cesar Fuentes, Hisanori Furusawa, Tetsuharu Fuse, Pamela L. Gay, Stephen Gwyn, Matthew J. Holman, H. Karoji, J. J. Kavelaars, Daisuke Kinoshita, Satoshi Miyazaki, Matt Mountain, Keith S. Noll, David J. Osip, Jean-Marc Petit, Neill I. Reid, Scott S. Sheppard, Mark Showalter, Andrew J. Steffl, Ray E. Sterner, Akito Tajitsu, David J. Tholen, David E. Trilling, Harold A. Weaver, Anne J. Verbiscer, Lawrence H. Wasserman, Takuji Yamashita, Toshifumi Yanagisawa, Fumi Yoshida, Amanda M. Zangari
Figure caption: Map showing the field pointings for the 2004 search plotted on the plane of the sky in equatorial coordinates. The solid blue line is the Galactic equator, and the center of the displayed segment is just 10° from the Galactic center. The solid green line at the bottom is the ecliptic. The green boxes are the size of the SuprimeCam FOV and show the positions from Table 2. The solid ellipse shows the 1σ search area in 2004, and the dashed ellipse shows the search area in 2005.
Paper: Constraints on the Long-term Existence of Dilute Cores in Giant Planets
Authors: A. Tulekeyev, P. Garaud, B. Idini, J. J. Fortney
Figure caption: Same as Figure 1, but for Pr = τ  =  0.1 and ﹩{R}_{0}^{-1}\,=\,1.75﹩. Left: time series of vertical density profiles. Each blue line corresponds to Δt = 2000 time unit increments. The various evolutionary stages are marked with arrows. Right: inverse density ratios vs. time: R −1 (0, t)(green) and R −1( ± 75, t) (orange). The red horizontal dashed line shows ﹩{R}_{L}^{-1}\simeq 1.5﹩, which is the layering threshold for Pr = τ  =  0.1, and the black dashed line corresponds to t = 2000 when the convection is triggered.
Paper: Constraints on the Long-term Existence of Dilute Cores in Giant Planets
Authors: A. Tulekeyev, P. Garaud, B. Idini, J. J. Fortney
Figure caption: Same as Figure 1, but for Pr = τ  =  0.1 and ﹩{R}_{0}^{-1}\,=\,1.25﹩. Left: time series of vertical density profiles. Each blue line corresponds to Δt = 1000 time unit increments. The various evolutionary stages are marked with arrows. Right: inverse density ratios vs. time: R −1(0, t)(green) and R −1( ± 75, t) (orange). The red horizontal dashed line shows ﹩{R}_{L}^{-1}\simeq 1.5﹩, which is the layering threshold for Pr = τ  =  0.1.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with JSC-1af and stirring. JSC-1af_Brined_Stirred_2022-05-13_14-15-15 0:01—valve closed, 0:03—during expansion, 0:15—thin layer of unconsolidated solid floating on top stops flowing, 1:40—overturn just started, 2:53—right before spindle sticks (is the shiny bit on the right liquid?), 4:37—sample has slowly become brighter (note: the cup shifted with respect to the spindle when the spindle stuck).
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with JSC-1a and stirring. JSC-1a_dilute_Brine_Stirred_2022-05-13_16-45-17 (lower power than others like this) 0:01—valve closed, 0:02—during expansion, 0:13—thin layer of unconsolidated solid floating on top stops flowing, 0:54—beginning to consolidate on walls and rod, 1:38—final lid has mostly formed, but overturn and liquid still seen below it, 2:04—final lid fully formed, spindle sticks less than 10 s later.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Eutectic (23%) brine with 44 μm glass beads and stirring. glassBeads44micron_Brine_Stirred_2022-05-13_15-25-30 0:06—valve closed, 0:07—during expansion, 0:14—viscous material stirring and bubbling 0:37—small chunks starting to form within the folds of the stirred material, 1:02—overturn dominates surface morphology, 2:55—sample has slowly become brighter (though less obvious than on JSC-1af).
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Image of a poorly degassed (left) and fully degassed (right) pure water experiment after removal from vacuum.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Image of a representative sample of the glass bead mixture after removal from vacuum. The sample looked the same with both pure water and brine.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Image after removing the stirred brine (no particles) from vacuum. The solid tended to be pushed up by the rotating blades.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Image of brine after removal from vacuum—the brine was the only sample that was mostly liquid upon removal from vacuum.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Image after removing the stirred brine with JSC-1af from vacuum.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Image after removing the stirred brine with JSC-1a from vacuum.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Analysis of the effect of residual atmosphere on the ice morphology and the temperature progression during the experiments. The morphology of 1 was concentric ice, while 2 was fluffy ice. “Warm” and “cold” base are described in the main text, Section 3.5.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Graph of how long (in seconds) after the vacuum shock began before the spindle became stuck in the vacuum-induced solids. Stir rate is motor steps per second, with 3200 steps being one full rotation.
Paper: Experimental Examination of Brine and Water Lifetimes after Impact on Airless Worlds
Authors: Michael J. Poston, Samantha R. Baker, Jennifer E. C. Scully, Elizabeth M. Carey, Lauren E. Mc Keown, Julie C. Castillo-Rogez, Carol A. Raymond
Figure caption: Image of the stirred brine with the 44 μm glass beads after bringing back to atmosphere.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final fit maps for FG3. (For an example of how to read these fit maps, see Figure 7.) The panels show, from left to right and top to bottom, the two SpeX apparitions; the NEOWISE data with both bands W1 and W2, first looking at the lower beaming parameter range and then looking at the upper beaming parameter range; the NEOWISE data with band W2 only, first looking at the lower beaming parameter range and then looking at the upper beaming range; the WISE data with bands W2 and W3, first looking at the lower beaming parameter range and then looking at the upper beaming parameter range; the WISE data with bands W1 and W2, first looking at the lower beaming parameter range and then looking at the upper beaming parameter range; and the WISE data with band W2 only, first looking at the lower beaming parameter range and then looking at the upper beaming parameter range. Note that other combinations of WISE bands did not produce any models that were consistent with the data (Section 4). The lower beaming parameter range goes from 0.70 to 1.20 in increments of 0.01. The upper beaming parameter range goes from 1.21 to 1.70 in increments of 0.01. The SpeX beaming parameter range goes from 0.70 to 1.20 in increments of 0.01. There are 11 total SpeX data sets in the first apparition and seven total in the second apparition, 16 total NEOWISE data sets, and one total WISE data set. In all plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final fit maps for JD6. (For an example of how to read these fit maps, see Figure 7.) The panels show, from left to right and top to bottom, the two SpeX apparitions; the NEOWISE data with the lower beaming parameter range, first looking at both bands W1 and W2 and then looking at band W2 only; the NEOWISE data with the upper beaming parameter range, first looking at both bands W1 and W2 and then looking at band W2 only; and the WISE data with emissivity of 0.9, first looking at both bands W1 and W2 and then looking at band W2 only. The NEOWISE lower beaming range goes from 0.50 to 1.70 in increments of 0.02. The NEOWISE upper beaming parameter range goes from 0.70 to 1.70 in increments of 0.02. The WISE beaming parameter range is 0.50–2.50 in increments of 0.05. The SpeX beaming parameter range goes from 0.70 to 1.70 in increments of 0.02. There are five total SpeX data sets in the first apparition and three total in the second apparition, 10 total NEOWISE data sets, and three total WISE data sets. In all plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final fit maps for SD220. (For an example of how to read these fit maps, see Figure 7.) The panels show, from left to right and top to bottom, the two SpeX apparitions; the NEOWISE data with the nominal diameter, first looking at both bands W1 and W2 and then looking at band W2 only; and the NEOWISE data with the smaller diameter, first looking at both bands W1 and W2 and then looking at band W2 only. We note that it is the H magnitude input to the model that actually changes between these two cases (Section 3). The beaming parameter range goes from 0.50 to 2.00 in increments of 0.05. There are four total SpeX data sets in the first apparition and four total in the second apparition, and there are nine total NEOWISE data sets. In all plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final fit maps for JD6. (For an example of how to read these fit maps, see Figure 7.) Here we show all explored band combinations for the WISE data. The panels show, from left to right and top to bottom, all four WISE bands, first looking at emissivity of 0.7 and then looking at emissivity of 0.9; WISE bands W2, W3, and W4, first looking at emissivity of 0.7 and then looking at emissivity of 0.9; WISE bands W3 and W4, first looking at emissivity of 0.7 and then looking at emissivity of 0.9; and WISE bands W2 and W3, first looking at emissivity of 0.7 and then looking at emissivity of 0.9. (For bands W1 and W2 and band W2 alone, see Figure 10.) In all cases the beaming parameter range is 0.50–2.50 in increments of 0.05. There are three total WISE data sets. In all plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: The consistency of NEOWISE model fits relative to models based on the SpeX data as a function of the NEOWISE magnitude. Each point is a different NEOWISE band observation (i.e., here the W1 and W2 band observations from a single data set are treated separately). “Consistent” means that the model results based on that band are consistent with results based on SpeX data. “Inconsistent” means that a model was fit to the band but the model was inconsistent with the results based on the SpeX data. “No Fit” means that no models could be fit to the band. A band observation is characterized as consistent vs. inconsistent or inconsistent vs. no fit if at least one band combination involving the given band can be fit with a model that meets the given criteria. The different colors represent the different bands. Magnitude uncertainties are the same size as or smaller than the symbols. Bands have been offset for clarity.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final fit maps for JM8. (For an example of how to read these fit maps, see Figure 7.) The panels show, from left to right and top to bottom, the single SpeX apparition; the NEOWISE data with both bands W1 and W2, first looking at the lower beaming parameter range and then looking at the upper beaming parameter range; and the NEOWISE data with band W2 only, first looking at the lower beaming parameter range and then looking at the upper beaming range. The lower beaming parameter range goes from 0.70 to 1.20 in increments of 0.01. The upper beaming range extends to 1.50. The SpeX beaming parameter range goes from 0.70 to 1.20 in increments of 0.01. There are seven total SpeX data sets and 10 total NEOWISE data sets. In all plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final fit maps for UO1. (For an example of how to read these fit maps, see Figure 7.) The panels show, from left to right and top to bottom, the two SpeX apparitions and the NEOWISE data, first looking at both bands W1 and W2 and then looking at band W2 only. The beaming parameter range goes from 0.70 to 1.20 in increments of 0.01. There are seven total SpeX data sets in the first apparition and eight total in the second apparition, and there are three total NEOWISE data sets. In all plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final fit maps for QE2. (For an example of how to read these fit maps, see Figure 7.) The panels show, from left to right and top to bottom, the single SpeX apparition and the NEOWISE data, first looking at both bands W1 and W2 and then looking at band W2 only. The NEOWISE beaming parameter range goes from 0.40 to 0.95 in increments of 0.01. The SpeX beaming parameter range goes from 0.55 to 0.80 in increments of 0.01. There are 20 total SpeX data sets and one total NEOWISE data set. In all plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo. (Note that these results were previously presented in S. A. Myers et al. 2023.)
Paper: On the Early Thermal Processing of Planetesimals during and after the Giant Planet Instability
Authors: Anastasios Gkotsinas, David Nesvorný, Aurélie Guilbert-Lepoutre, Sean N. Raymond, Nathan Kaib
Figure caption: Thermal processing of a planetesimal scattered toward the OC. Upper panel: evolution of the effective thermal radius (r  T ). Lower panel: temperature distribution (denoted by the color code) in the planetesimal’s interior at a subsurface layer of ∼1000 m. The dashed, dotted, and dashed–dotted white lines show the CO, CO2, and crystallization interfaces, respectively.
Paper: On the Early Thermal Processing of Planetesimals during and after the Giant Planet Instability
Authors: Anastasios Gkotsinas, David Nesvorný, Aurélie Guilbert-Lepoutre, Sean N. Raymond, Nathan Kaib
Figure caption: Characteristic timescales of the main physical processes taking place in a comet’s nucleus: crystallization of amorphous H2O ice, denoted by the green dashed–dotted line; sublimation of different volatile species, denoted by the blue dashed lines; gas diffusion within the pores for pore radii between 10−3 and 10−6, denoted by the orange dotted lines and the orange shaded area; and heat diffusion in a nucleus of different compositions: pure dust, pure crystalline H2O ice, and a nucleus with characteristics resembling those of comet 67P/Churyumov–Gerasimenko. The black loosely dotted lines serve as timescale indicators. Figure adapted from D. Prialnik et al. (2004) and W. F. Huebner et al. (2006).
Paper: On the Early Thermal Processing of Planetesimals during and after the Giant Planet Instability
Authors: Anastasios Gkotsinas, David Nesvorný, Aurélie Guilbert-Lepoutre, Sean N. Raymond, Nathan Kaib
Figure caption: Example of the planetesimals’ implantation on the Kuiper Belt (upper panel) and the OC (lower panel) on the semimajor axis vs. eccentricity plane. The color code provides the timescale of the simulation. The orange clusters denote the orbital evolution of Jupiter, Saturn, Uranus, and Neptune.
Paper: On the Early Thermal Processing of Planetesimals during and after the Giant Planet Instability
Authors: Anastasios Gkotsinas, David Nesvorný, Aurélie Guilbert-Lepoutre, Sean N. Raymond, Nathan Kaib
Figure caption: Orbital distribution in the semimajor axis and eccentricity plane of the KB/SD (black dots) and OC (red triangles) planetesimals at the beginning (t = 0 yr; top panel) and the end of the simulation (t = 200 Myr; bottom panel).
Paper: On the Early Thermal Processing of Planetesimals during and after the Giant Planet Instability
Authors: Anastasios Gkotsinas, David Nesvorný, Aurélie Guilbert-Lepoutre, Sean N. Raymond, Nathan Kaib
Figure caption: Cumulative distribution of the CO ice interface depths for the members of the three studied populations, KB/SD (red dashed line), OC (green dashed–dotted line), and ejected (black dotted line) planetesimals, at the end of their reservoir implantation and ejection phases, respectively.
Paper: On the Early Thermal Processing of Planetesimals during and after the Giant Planet Instability
Authors: Anastasios Gkotsinas, David Nesvorný, Aurélie Guilbert-Lepoutre, Sean N. Raymond, Nathan Kaib
Figure caption: Cumulative distribution of the amorphous water-ice crystallization interface depths for the members of the three studied populations, KB/SD (red dashed line), OC (green dashed–dotted line), and ejected (black dotted line) planetesimals, at the end of their reservoir implantation and ejection phases, respectively.
Paper: On the Early Thermal Processing of Planetesimals during and after the Giant Planet Instability
Authors: Anastasios Gkotsinas, David Nesvorný, Aurélie Guilbert-Lepoutre, Sean N. Raymond, Nathan Kaib
Figure caption: Cumulative distribution of the CO2 ice interface depths for the members of the three studied populations, KB/SD (red dashed line), OC (green dashed–dotted line), and ejected (black dotted line) planetesimals, at the end of their reservoir implantation and ejection phases, respectively.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: Effect of the two-point ELM with three panels at the same scene. Triangles facing upward show the radiance values of panel (1) (highest-elevation panel), while triangles facing downward indicate the radiance values of the lowest-elevation panel (panel (3)). The diamond symbols indicate the middle panel (panel (2)). The colors of the symbols indicate the different bands of the MicaSense RedEdge Camera. The radiance values are in W m−2 sr−1 nm−1.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: (a) The west of Lake Natron study area. Three sites discussed in this study are shown with red symbols: (i) Moinik Formation clays and tuff (MFC); (ii) Humbu Formation at Pinini (HFP); and (iii) Humbu Formation, Hajaro basalt, and Sambu lava exposures at Mtowabaga (HHS). (b) A field photo showing badland features. (c) Geology map of the study area (after G.L. Isaac 1967). Sample locations are indicated by yellow stars.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: All spectra collected using the Halo instrument in the study, with all available Mars multispectral cameras and RedEdge-M band locations. Gray vertical lines show the wavelengths selected to calculate band indices. Dashed vertical lines show the proposed band locations for future multispectral cameras based on this study. See Table 3 for wavelength values.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: Optical path affecting the drone observation between at-target, above-surface (canopy), and at-sensor positions. E AC: above-surface (canopy) irradiance; E AS: at-sensor irradiance; E AT: at-target irradiance; L ADT: at-dark-target radiance; L ABT: at-bright-target radiance; L ASD: at-sensor radiance coming from the dark target; L ASB: at-sensor radiance coming from the bright target; L DIF: diffuse radiance; R D: reflectance factor of dark panel; R B: reflectance factor of bright panel; t: atmospheric transmittance.