adsabs/AstroCLIMB huggingface dataset:
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: North-to-south Th (top), plagioclase (middle), and crust thickness (bottom) profiles across maria Marginis, Smythii, and Australe. See Figure 4 for the location of the profile.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: A suite of four map tiles (Th content, WAC geomorphology (E. J. Speyerer et al. 2011), crustal thickness, and plagioclase content) for the vicinity of crater Kohlschütter. The white dashed circle in the WAC image delineates the extent of the Kohlschütter-Lenov basin proposed by C. J. Byrne (2016).
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: Southwest-to-northeast Th (top), plagioclase (middle), and crust thickness (bottom) profiles across the Keeler West basin and the Dewar cryptomare. See Figure 2 for the location of the profile.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: West-to-east Th (top), plagioclase (middle), and crust thickness (bottom) profiles across the Kohlschütter-Lenov basin. See the Th map in Figure 12 for the location of the profile.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: West-to-east Th (top), plagioclase (middle), and crust thickness (bottom) profiles across the Korolev and Hertzsprung basins. See Figure 2 for the location of the profile.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: A suite of four map tiles (Th content, FeO, 643 nm WAC, and FeO zoomed in) for the vicinity of the Dewar cryptomare.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: Northwest-to-southeast Th (top), plagioclase (middle), and crust thickness (bottom) profiles across the B-K basin. See the Th map in Figure 15 for the location of the profile.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: North-to-south Th (top), plagioclase (middle), and crust thickness (bottom) profiles across the Orientale and Mendel–Rydberg basins. See Figure 3 for the location of the profile.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: A suite of four map tiles (Th content, FeO, crustal thickness, and plagioclase content) for the vicinity of the B-K basin.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: A suite of four map tiles (Th content, plagioclase content, crustal thickness and impact basins, and 643 nm band of WAC) for the near side. See the map legends for the color-coding of the individual maps. The thick green dashed lines roughly delineate the extent of the PKT. The thick white dashed line represents a circle of 2800 km radius centered at the Imbrium basin.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: Southwest-to-northeast Th (top), plagioclase (middle), and crust thickness (bottom) profiles across the Th anomaly northeast of Moore F. See Figure 2 for the location of the profile.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: CO2 vapor distribution maps 4 hr, 3 hr, 2 hr, 1 hr, and 14 minutes prior to closest approach of Hartley 2. CO2 is ubiquitous in the near-nucleus coma but is enhanced by a factor of ∼2 compared to the mean in the direction extending from the small lobe of the comet (+Z-axis indicated by black arrows). The small insets are images of the nucleus simulated from the Hartley 2 shape model (T. L. Farnham & P. C. Thomas 2013; P. C. Thomas et al. 2013) at the orientation and solar illumination conditions as seen by the spacecraft incorporating the rotation rate of M. J. S. Belton et al. (2013). The nucleus undergoes ∼20% of its primary axis rotation during the 4 hr time span. The location of the unresolved nucleus is marked with a black plus sign. In the E – 14-minute map, the saturated nucleus is overlaid with the shape model simulation. Each image is normalized to the mean of its radiance map. The Sun is to the right in all the images, and Ecliptic North is up.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Spatial distribution maps of volatile species in Hartley 2 derived from an HRI-IR spectral scan 7 minutes after closest approach. While H2O and CO2 are ubiquitous in the scene, enhancements in their abundances are uncorrelated. However, the distribution of H2O ice appears to be correlated with CO2. Figure modified from M. F. A’Hearn et al. (2011) (PDS data set dif-c-hrii-3_4-epoxi-hartley2-v3.0; DOY 308, Exposure ID hi5006000, scan start time 2010-11-04T14:05:49; spatial resolution 52 m pixel−1; Sun to the right; S. A. McLaughlin et al. 2014).
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: H2O vapor distribution maps at E – 4 hr, E – 3 hr, E – 2 hr, E – 1 hr, and E – 14 minutes prior to closest approach. H2O is ubiquitous in the scene but asymmetric and is especially enhanced in the sunward direction and above the smooth waist in these fields of view and spatial resolution. The annotations are similar to those in Figure 3; however, here the red arrows are the projected normal to the illuminated waist area of the nucleus. Each map is normalized to its mean, and the Sun is to the right, with Ecliptic North toward the top.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Representative continuum-removed spectrum for a single pixel in the E + 5 hr scan (dif-c-hrii-3_4-epoxi-hartley2-v3.0; DOY 308, Exposure ID hi4001300, scan start time 2010-11-04T18:58:19; S. A. McLaughlin et al. 2014). Emissions due to H2O, CO2, and a weak organic blend are present in this spectrum. The regions used for final continuum removal flanking each emission are indicated with thick red lines.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Radial profiles and production rates of CO2 (left column) and H2O (right) showing where the data deviate from an r−1 falloff. The top panels are the combined E + 25-minute through E + 52-minute data, and the middle panels are the combined E + 9 hr through E + 9.5 hr data, representative of the period in the comet’s rotation where each of the lobes is pointed either sunward (red) or antisunward (black). The CO2 and H2O profiles are inversely proportional to radial distance beyond 20 km, inside of which the profiles suffer from varying degrees of opacity and accelerating gas flow, for both the small (diamonds) and large (squares) lobes of the comet. The exception is the H2O profile for the antisunward small lobe, where the deviation from r−1 between 10 and 150 km is attributed to sublimation from an icy grain population. Associated production rates are displayed in the bottom panels. The H2O production in the antisunward-facing small-lobe plot stands out because it never levels off to a steady rate. These data integrate a 60° wedge with vertex at the nucleus. The gaps in the small-lobe sunward data from ∼16 to 28 km in CO2 and ∼160–195 km antisunward in the H2O data are due to poorly calibrated data with the HRI-IR ASF.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Near-nucleus distribution of H2O measured from the extracted radiance in azimuthally adjacent 15° sectors at radial distances of 2, 3.8, and 5.2 km from the nucleus and normalized to the peak radiance for each distance (top left). The peak in the distribution is dependent on the distance from the nucleus and the solar illumination. For the closest distance, 2 km, the peak is due to the H2O released directly from the illuminated waist, while by 3.8 km the waist H2O has diffused and the peak shifts to the sunward direction and is due to subsolar nucleus outgassing. The peak remains in the subsolar direction at 5.2 km. The antisunward enhancement cannot be discerned this close to the nucleus. The plots for 2 and 5.2 km are offset for clarity by +0.1 and −0.1, respectively. Bottom left: the azimuthal radiance plots are fit with three parabolic components, accounting for contribution from the waist (orange dotted), the subsolar point (orange dashed), and an ambient sublimation background (orange dashed–dotted) in the example fit offset and plotted for the 5.2 km distance. The corresponding total fit is overplotted as a thick solid line for each radial distance. The minimum occurs in the antisunward direction. Right: the annotated E + 52-minute H2O distribution map is representative of this time period and geometry, with the nucleus at the center of the image, 90° at the top, and the azimuthal angle increasing in the clockwise direction. The brighter pixels correspond to higher abundance, and the scale is ∼8 km across.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: H2O (blue color scale images) and CO2 (green color scale) distribution maps, normalized to their mean, at 3 hr increments post-encounter showing coma enhancements in each species and their time variability. Illuminated shape model images (not to scale) of the simulated orientation and solar illumination conditions of Hartley 2 as seen by the spacecraft are included for each time step. In the H2O maps, a 90° wedge is overplotted in gray, indicating the antisunward quadrant where water concentrates after closest approach. In the CO2 maps, a black arrow is drawn in the projected direction of the small lobe of the nucleus (the +Z-axis). As in the approach data (Figure 3), the CO2 distribution is strongly correlated with the small lobe, rotating with it throughout the 18 hr period. The unresolved nucleus (black plus sign) is located at the center of each of the maps. The Sun is to the right, and Ecliptic North is down.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Azimuthal distribution of H2O measured from extracted radiance in azimuthally adjacent 15° sectors at a radial distance of 60 km from the nucleus and normalized to the peak radiance for each time step representing over half of Hartley 2’s rotation (E + 6 hr through E + 15 hr). The thick black curve is the average of the plotted data. At these larger distances, the relative production of H2O is stable over time, and thus the comet’s rotation, and shows peak production from icy grains in the antisunward direction by a factor of ∼2 over the minimum.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Azimuthal distribution of CO2 around the nucleus measured at E + 6 hr from extracted radiance in adjacent 15° sectors at radial distances of 10, 26, 40, and 60 km from the nucleus and normalized to the peak radiance for each distance. The peak in the distribution of CO2 around the nucleus is clearly not dependent on either radial distance or solar direction, but rather is directly correlated to the direction of the small lobe (+Z pole). As in Figures 6 and 8, this result demonstrates the nonuniform release of CO2 from the nucleus, with a maximum at the small lobe that is a factor of ∼3 larger than its minimum.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Enhanced maps of CO2 vapor in Hartley 2’s coma observed after closest approach, revealing that in all fields of view the enhanced CO2 distribution is correlated with the small lobe and rotates with the nucleus. Simulated nucleus orientations (left column, not to scale) and CO2 distribution maps (middle column) are as in Figure 5. The rightmost column displays normalized distribution maps after an azimuthal average was divided out. The Sun is to the right, and Ecliptic North is down.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: H2O distribution map with contours taken at E + 6.5 hr showing a strong antisunward enhancement, which out to ∼10 km is superimposed on the nucleus contribution in the sunward direction. The pixel containing the nucleus is circled in black, and the Sun is to the right, with Ecliptic North down.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Small-lobe CO2 production decreases, but does not cease, when unilluminated. The peak in CO2 production at ∼ 4 hr and minimum at ∼14 hr are approximately separated in time by half of the primary rotation of the nucleus’s complex rotation period of ∼18 hr, corresponding to when the small lobe is pointed in the antisunward hemisphere. The CO2 production of the small lobe never completely stops and increases when illuminated again with a maximum production that is ∼3 larger than its minimum. The CO2 is measured 20 km off the small lobe of the nucleus in a 30° opening angle.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Enhanced maps of H2O vapor in Hartley 2’s coma (analogous to Figure 6). The resulting distribution maps emphasize that in small fields of view (top) the water vapor is more symmetric about the nucleus, but in the later, larger fields of view an antisunward enhancement of a factor of ∼3 is very pronounced. The antisunward asymmetry persists with time and is independent of how the nucleus is oriented, consistent with a water vapor contribution from icy grains pushed antisunward by solar radiation pressure. The Sun is to the right, and Ecliptic North is down.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Simple icy grain source sublimation model described in Section 4.2 compared to H2O column density distribution maps from Hartley 2: (a) model with implanted r−1 sources; (b) smoothed model; (c) random noise added to the model; (d) observed map of the H2O distribution of Hartley 2 at E + 6.5 hr; (e) azimuthal average divided out of the model to accentuate the antisunward distribution enhancement; (f) azimuthal average divided out of the observations to accentuate the antisunward distribution enhancement in the H2O distribution of Hartley 2 at E + 6.5 hr. This simple model replicates the observations in both morphology and relative scale to within ∼10%, increasing the plausibility that H2O-ice grains are responsible for Hartley 2’s extended H2O and are producing the observed asymmetry in the coma. Model plots are in units of 1016 cm−2, and E + 6.5 hr data are in cm−2. The Sun is to the right, and the nucleus location is indicated by the black circle.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Radial profiles of H2O column density for a representative sample of data covering a full primary rotation of Hartley 2. An r−1 falloff is overplotted (solid black line) for reference. The antisunward coma has more H2O than predicted from a nucleus sublimation source. Both the sunward and antisunward profiles converge to an asymptotic value at 100–200 km. The antisunward value (∼3.2 × 1015 cm−2) is larger than the sunward value (∼1.0 × 1015 cm−2) by a factor of ∼3, indicative of an antisunward extended source of water.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: The average H2O distribution (blue) at 60 km from Figure 12 compared with the CO2 distribution (orange) at the same distance at E + 6 hr. The peaks in the two species differ as expected, with the H2O peak near the anti-Sun direction and the CO2 peak near the projected small-lobe direction.
Paper: Unraveling the Water Sources in Comet 103P/Hartley 2 from Deep Impact Flyby Observations
Authors: L. M. Feaga, J. M. Sunshine
Figure caption: Sunward (+) and antisunward (–) radial profiles from the model (black solid line) described in Section 4.2 compared to radial profiles extracted from H2O distribution maps of Hartley 2 at E + 6.0 hr (blue dashed line) and E + 6.5 hr (red solid line). Quantitatively, the model represents the observations well, agreeing with the r−1 nucleus sublimation radial falloff in the sunward direction and the asymmetric factor of 2 larger column density in the antisunward direction due to a secondary H2O source of ice gains in the coma.
Paper: LiDO: Exploring the Stable Plutino Parameter Space
Authors: Samantha M. Lawler, Mark Comte, Rosemary E. Pike, Mike Alexandersen, Ying-Tung Chen, 英同 陳, Cameron Collyer, Matthew Holman, J. J. Kavelaars, Lowell Peltier, Cameron Semenchuck
Figure caption: Nested contour lines or shades show the relative density of stable plutinos and Kozai plutinos from Figure 3 in a, e, and i: red contour shades show non-Kozai plutinos, and blue contours show Kozai plutinos. Contours enclose 0.1%, 10%, 30%, 50%, 70%, 90%, and 99% of the synthetic distribution points. Overlaid are real TNOs from characterized surveys that are close to a = 39.4 au. Those detected by the LiDO survey are dark green squares (plutinos) or light green squares (nonplutinos), those previously detected by OSSOS++ are black (plutinos) or gray points (nonplutinos), and the orbital uncertainties on OSSOS++ TNOs are smaller than the point size. The LiDO classifications are preliminary but have sufficiently long arcs and use the same methodology as this work. The i range of these plots is trimmed, as while the high-i parameter space is stable, no real TNOs have been discovered in this part of the resonance.
Paper: LiDO: Exploring the Stable Plutino Parameter Space
Authors: Samantha M. Lawler, Mark Comte, Rosemary E. Pike, Mike Alexandersen, Ying-Tung Chen, 英同 陳, Cameron Collyer, Matthew Holman, J. J. Kavelaars, Lowell Peltier, Cameron Semenchuck
Figure caption: Osculating end-state orbital elements for 4 Gyr stable plutinos, with non-Kozai plutinos in red, stable Kozai plutinos in blue, unstable Kozai oscillators in yellow, and Kozai flippers in purple. Histograms along the x- and y-axes of each plot show the relative number densities of each set of objects across each parameter-space cut. Note that at the central a value for the 3:2 resonance, e > 0.24 will result in a pericenter sunward of Neptune’s orbit.
Paper: LiDO: Exploring the Stable Plutino Parameter Space
Authors: Samantha M. Lawler, Mark Comte, Rosemary E. Pike, Mike Alexandersen, Ying-Tung Chen, 英同 陳, Cameron Collyer, Matthew Holman, J. J. Kavelaars, Lowell Peltier, Cameron Semenchuck
Figure caption: On the left is the distribution of ϕ3:2 for all 4 Gyr stable plutinos (Kozai and non-Kozai summed in a stacked histogram) in orange, with the Kozai plutinos only in purple. The difference in peak libration amplitude is likely a result of the a and e dependence of ϕ3:2 (see Figure 6). The black and green dotted lines show the parametric distributions used in models based on debiased CFEPS (B. Gladman et al. 2012) and OSSOS (K. Volk et al. 2016) data, respectively, both of which used the same libration amplitude distributions for Kozai and non-Kozai plutinos. The right panel shows ω-libration amplitudes for Kozai librators only; note that these amplitudes vary quite a bit over the course of the simulation, so large bins are used to show the overall distribution. K90 librators are in blue, K270 librators are in red, and there is no measurable difference between the distributions.
Paper: LiDO: Exploring the Stable Plutino Parameter Space
Authors: Samantha M. Lawler, Mark Comte, Rosemary E. Pike, Mike Alexandersen, Ying-Tung Chen, 英同 陳, Cameron Collyer, Matthew Holman, J. J. Kavelaars, Lowell Peltier, Cameron Semenchuck
Figure caption: The argument of pericenter ω and the resonant angle ϕ3:2 plotted over 4 Gyr simulations (sampled at 10 Myr intervals) for four different test particles showing the range of behaviors identified within the 3:2 resonance. Each test particle is labeled with the classification determined by our classification script.
Paper: LiDO: Exploring the Stable Plutino Parameter Space
Authors: Samantha M. Lawler, Mark Comte, Rosemary E. Pike, Mike Alexandersen, Ying-Tung Chen, 英同 陳, Cameron Collyer, Matthew Holman, J. J. Kavelaars, Lowell Peltier, Cameron Semenchuck
Figure caption: Nested contour lines or shades enclose 0.1%, 10%, 30%, 50%, 70%, 90%, and 99% of the 4 Gyr stable synthetic distribution plutinos in a (top left) and e (top right) vs. ϕ3:2-libration amplitudes of the particles. The distribution for the Kozai plutinos is shown with blue contours, while the non-Kozai plutinos are shown in reddish solid contours. The lower panel shows the ω-libration amplitudes vs. the ϕ3:2-libration amplitudes for 4 Gyr stable Kozai plutinos.
Paper: LiDO: Exploring the Stable Plutino Parameter Space
Authors: Samantha M. Lawler, Mark Comte, Rosemary E. Pike, Mike Alexandersen, Ying-Tung Chen, 英同 陳, Cameron Collyer, Matthew Holman, J. J. Kavelaars, Lowell Peltier, Cameron Semenchuck
Figure caption: A snapshot of the predicted positions of a flux-limited set of simulated plutinos on the sky, generated using a toy model version of the expected LiDO survey sensitivity and an orbital element distribution model based on debiased measurements from S. M. Lawler & B. Gladman (2013) and M. Alexandersen et al. (2016). Kozai plutinos are shown with blue points, and non-Kozai plutinos are in red. The ecliptic and position of Neptune at the midpoint of the survey are also marked. Our CFHT program targeted the highest predicted on-sky density of K90 librators in the A-semester block and K270 librators in the B-semester block.
Paper: LiDO: Exploring the Stable Plutino Parameter Space
Authors: Samantha M. Lawler, Mark Comte, Rosemary E. Pike, Mike Alexandersen, Ying-Tung Chen, 英同 陳, Cameron Collyer, Matthew Holman, J. J. Kavelaars, Lowell Peltier, Cameron Semenchuck
Figure caption: Histogram of ﹩{I}_{{\rm{\max }}}﹩ (see Equation (2)) for all Kozai plutinos in the simulation (﹩\cos {I}_{{\rm{\max }}}﹩ along top axis for reference). Kozai particles with different levels of stability have different ﹩{I}_{{\rm{\max }}}﹩ values: the lowest ﹩{I}_{{\rm{\max }}}﹩ values tend to be unstable Kozai librators (yellow), while the highest ﹩{I}_{{\rm{\max }}}﹩ values tend to be stable Kozai librators (cyan), with Kozai flippers inhabiting midrange ﹩{I}_{{\rm{\max }}}﹩ values (magenta).
Paper: LiDO: Exploring the Stable Plutino Parameter Space
Authors: Samantha M. Lawler, Mark Comte, Rosemary E. Pike, Mike Alexandersen, Ying-Tung Chen, 英同 陳, Cameron Collyer, Matthew Holman, J. J. Kavelaars, Lowell Peltier, Cameron Semenchuck
Figure caption: Selections from the 4 Gyr integration of several test particles are plotted in ﹩e\cos \omega -e\sin \omega ﹩, with example test particles exhibiting K270 libration (red), K90 libration (blue), unstable Kozai libration (yellow), Kozai flipping (magenta), and an example K0 librator in green, discussed in Section 3.4.