adsabs/AstroCLIMB huggingface dataset:
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 distribution of ω-libration amplitudes and ﹩{I}_{{\rm{\max }}}﹩ values resulting from the test particles in the four simulations analyzed from N. A. Kaib & S. S. Sheppard (2016) (see legend) compared with the same distributions for our filled-parameter-space synthetic distribution (gray filled histogram). Despite different Neptune migration timescales and smooth or grainy migration, these four simulations result in similar distribution ranges of ω libration while being very different in ﹩{I}_{{\rm{\max }}}﹩.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Schematic diagram of the transport model of a CO2 molecule on Europa. Given that sublimation releases a CO2 molecule with an initial velocity at an elevation angle of γ, the particle flies within Europa’s atmosphere, following a ballistic trajectory (the dashed line). Subsequently, the molecule is adsorbed on the surface. Here, the transport angle Δψ is defined as the angle among the sublimation point, the center of Europa, and the adsorption point.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Longitudinal distribution of CO2 at low latitudes (<30°). See also Figures 4 and 12. Immediately after a CO2 release (e.g., the 1 day case; orange dots), CO2 is concentrated near the hypothetical source (marked by the vertical dashed line). Over time, CO2 becomes more widely distributed along the longitude (e.g., the 10 days case; blue dots). Under steady-state conditions, the probability of detecting CO2 at low latitudes in the eastern hemisphere is comparable to that in the western hemisphere (black dots). Note that under steady-state conditions, most of the CO2 accumulates at higher latitudes (>60°), and the probability of detecting CO2 at low latitudes in either hemisphere is negligible on a global scale (see Supplementary Figure 12(a)).
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Distribution of CO2 particles on Europa. The left column shows the distribution in the western hemisphere, while the right column shows the distribution in the eastern hemisphere. A hypothetical source of CO2 was set at 10°S, 75°W, which is indicated by white diamonds. The subobserver point was set at 30°S, 90°W for the left column, while it was set at 30°N, 90°E for the right column.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Distribution of CO2 particles on Europa with rapid CO2 loss process. The timescale of CO2 loss (τphoto in Equation (27)) was arbitrarily decreased by factors of (a) 100 and (b) 1000 compared to our results shown in Supplementary Figure 12. See Supplementary Figure 12 for further details.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Distribution of CO2 particles on Europa with delayed sublimation. The residence time of CO2 (τice,co2 in Equation (14)) was arbitrarily increased by factors of (a) 105, (b) 106, and (c) 107 compared to our results shown in Supplementary Figure 12. See Supplementary Figure 12 for further details.
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Cross section for electron impact as a function of impact energy. Modified from K. Anzai et al. (2012). The cross section of CO2 (dashed line) tends to be larger than that of H2O (solid line).
Paper: Equatorial CO2 Distribution Suggests Active CO2 Supply on Europa
Authors: Shintaro Kadoya, Yasuhito Sekine, Takanori Kodama
Figure caption: Transition of a particle within a pit. (a) The solid angle when a CO2 particle is adsorbed on the wall of a cylindrical pit. (b) The solid angle when a CO2 particle is adsorbed on the bottom of a cylindrical pit. (c) Definition of pb,m and pw,n.
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: Optimized model fits for all isotopologues in the left column, panels (a), (c), (e), and (g). The data are in black, and the model is in blue. The molecule is identified in the top left corner of the panel along with the corresponding scaling factor. The respective retrieved vertical profiles (VMRs) are in the right column, panels (b), (d), (f), and (h). In all profiles, the red line is the a priori profile, the blue line is the retrieved VMR profile, and the shaded region is the error on the retrieved VMR profile. For the major isotopologue, the dashed black line in panel (b) is the temperature profile. The error envelope of the minor isotopologues is quite narrow; it is within 6%–8% of the obtained isotope ratio value. The red ticks in (e) and (g) identify the 13CH3CN and CH313CN lines, respectively, in the data. The highest-frequency line in (e) is the J = 30–29, Ka = 3 transition of C2H5CN (propionitrile; ethyl cyanide) at 268.0025 GHz.
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: Derived 14N/15N isotopic ratios for molecules in Titan’s atmosphere, including the value derived in this work in red. The N2 data point is plotted against a gray background to distinguish it as the main atmospheric nitrogen reservoir. The black dashed line is the error-weighted average of previously measured 14N/15N ratios from A. Marten et al. (2002), M. A. Gurwell (2004), S. Vinatier et al. (2007), R. Courtin et al. (2011), E. M. Molter et al. (2016), M. A. Cordiner et al. (2018), and T. Iino et al. (2020).
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: CH3CN/CH3C15N isotopic ratio (red point) derived from our scale-factor retrieval, with the horizontal error bar showing the error on the ratio value and the vertical bar spanning the region of highest sensitivity: 150–300 km. For comparison, the chemical model results of M. Dobrijevic & J. Loison (2018; black, without cosmic rays; gold, with cosmic rays) and V. Vuitton et al. (2019; blue line) are shown.
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: Derived continuous CH3CN/CH3C15N isotopic ratio profile with error envelope (red; shaded red region) plotted with photochemical model profiles from M. Dobrijevic & J. Loison (2018; green and gold) and V. Vuitton et al. (2019; blue). The black point is our measured scaling factor for the CH3CN/CH3C15N isotopic ratio from this work, plotted at the weighted mean emission altitude of 230 km (with its corresponding error bars).
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: Spectral line broadening profile based on the CH3CN wind field observed by M. A. Cordiner et al. (2020; left) and the final line-spread function with wind-induced broadening as well as the Hanning-smoothed sinc response of the ALMA correlator (right).
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: Continuously retrieved CH3C15N model fit (left) and VMR profile (right). As in Figures 1(a) and 1(b), the data are in black, and the model is in blue; in the right panel, the red line is the a priori profile, the blue line is the retrieved VMR profile, and the shaded region is the error on the retrieved VMR profile.
Paper: Improved Carbon and Nitrogen Isotopic Ratios for CH3CN in Titan’s Atmosphere Using ALMA
Authors: Jonathon Nosowitz, Martin A. Cordiner, Conor A. Nixon, Alexander E. Thelen, Zbigniew Kisiel, Nicholas A. Teanby, Patrick G. J. Irwin, Steven B. Charnley, Véronique Vuitton
Figure caption: Contribution functions for the strongest lines (K = 3) of CH3CN and its minor isotopologues.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Results from DSMC models of Callisto’s atmosphere at SZA = 0∘ considering interactions with photons only (“Photo Only”; solid lines) compared to those considering interactions with photons and magnetospheric electrons (“Photo+Electron Impact”) assuming an upstream density, ne, of 1 cm−3 and temperatures, Te, of 40 eV (dashed lines) or 400 eV (dashed–dotted lines). Number densities (bottom x-axis) are listed as a function of radial altitude (y-axis) for H2 (red), O2 (blue), CO2 (green), CO (cyan), H (magenta), and O (orange). The corresponding temperature profiles (top x-axis) are also illustrated in gray.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: A comparison of dissociation and/or ionization rates resulting from interactions with photons and magnetospheric electrons in Callisto’s atmosphere composed of CO2 (purple), CO (blue), O2 (cyan), H2 (light green), O (orange), and H (red). A range of photodissociation and/or ionization rates (solid red lines) are listed according to solar minimum (filled red squares), median (filled red diamonds), and maximum (filled red circles). A range of magnetospheric electron-impact dissociation and/or ionization rates (dashed blue lines) are listed assuming the following electron number densities, ne, and temperature, Te: ne = 0.1 cm−3, Te = 40 eV (open blue circle); ne = 1.0 cm−3, Te = 40 eV (open blue square); ne = 0.1 cm−3, Te = 400 eV (open blue diamond); and ne = 1.0 cm−3, Te = 400 eV (open blue triangle).
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Results from the photochemical model of Callisto’s ionosphere at SZA = 0∘, with inputs taken from DSMC models of Callisto’s neutral atmosphere (Figure 3), which is ionized by interactions with photons only. We also list the expected Juice C/A altitude (200 km) as well as the density and energy thresholds for its PEP/NIM instrument, ∼1 cm−3 and 10 eV, respectively.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: A comparison of timescales, τ, calculated in the photochemical model of Callisto’s ionosphere at SZA = 0∘ for photochemistry (τC), diffusion (τD), and magnetospheric pickup (τPU). Results for τC and τD are given for the three considered models, where only interactions with photons were considered (solid lines); and interactions with photons and magnetospheric electrons were considered, where at the top of the atmosphere the latter was assumed to have a density of ne = 1 cm−3 and temperature of either Te = 40 eV (dashed lines) or Te = 400 eV (dashed–dotted lines). Only one line is shown for τPU because the results were effectively the same across all three cases considered.
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Electron densities from the photochemical model of Callisto’s ionosphere compared to those inferred from Galileo observations by PWS during the C10 flyby (red, white, and blue squares; D. A. Gurnett et al. 2000) and from radio occultations during the C20, C22, and C23 flybys (open black circles with horizontal lines representing error bars; A. J. Kliore et al. 2002). Electron densities in the photochemical model of Callisto’s ionosphere are calculated as the sum of all ion densities. The four considered models shown are for when only interactions with photons were considered (“Photo Only”) at SZA = 90∘ (blue) and 0∘ (orange) and when interactions with photons and magnetospheric electrons were considered (“Photo+Electron Impact”) at SZA = 0∘, where at the top of the atmosphere the latter was assumed to have a density of ne = 1 cm−3 and temperature of either Te = 40 eV (green) or Te = 400 eV (red).
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Comparison of results from photochemical modeling of Callisto’s ionosphere at SZA = 0∘ for O﹩{}_{2}^{+}﹩, CO﹩{}_{2}^{+}﹩, CO+, H﹩{}_{2}^{+}﹩, O2H+, HCO﹩{}_{2}^{+}﹩, HCO+, and H﹩{}_{3}^{+}﹩, where only interactions with photons were considered (red) and interactions with photons and magnetospheric electrons were considered an upstream density of ne = 1 cm−3 and temperature of either Te = 40 eV (blue) or Te = 400 eV (green).
Paper: A Direct Simulation Monte Carlo–Driven Photochemical Model of Callisto’s Ionosphere
Authors: Shane R. Carberry Mogan, Luke E. Moore, Lucas Liuzzo, Andrew R. Poppe
Figure caption: Orbital configuration of Callisto during the various observations described in Section 2.1, shown in units of Jupiter radii, RJ = 71,492 km: Voyager 1, “V1,” during its C/A to the Jovian system (A. L. Broadfoot et al. 1979; red); Galileo C3, C9, C10, C21–23, and C30 flybys (D. A. Gurnett et al. 1997, 2000; R. W. Carlson 1999; A. J. Kliore et al. 2002; blue); HST (D. F. Strobel et al. 2002; N. J. Cunningham et al. 2015; green); Keck (K. de Kleer et al. 2023; orange); and JWST (R. J. Cartwright et al. 2024; purple). The +X-direction points toward the Sun, while the Y-axis lies in the ecliptic plane, aligned with Callisto’s counterclockwise orbital motion around Jupiter. Orbital longitude and local time as well as eastern and western elongations are also listed for reference.
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 far side. See the map legends for the color-coding of the individual maps. The red line corresponds to the −4 km elevation contours that roughly delineate the extent of the SPA 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 eastern hemisphere. See the map legends for the color-coding of the individual maps. 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: A Th content map (left) and a plagioclase content map (right) for the PKT. Note that the color-coding for the Th content map has been altered from that for Figures 1–5 to show the variations among relatively high values. The graticules are drawn at 30° intervals. The distribution of the Fra Mauro and Alpes formations is based on C. M. Fortezzo et al. (2020).
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 western hemisphere. See the map legends for the color-coding of the individual maps. 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: A suite of four map tiles (Th content, plagioclase content, crustal thickness and impact basins, and 643 nm band of WAC) for the south polar region. See the map legends for the color-coding of the individual maps.
Paper: A Global Survey of Lunar Surface Thorium Anomalies Associated with Impact Basins
Authors: S. Nagihara
Figure caption: West-to-east Th (top) and plagioclase (bottom) content profiles across the western margin of the PKT and the exterior swath likely blanketed by Imbrium ejecta. 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: North-to-south Th (top) and plagioclase (bottom) content profiles across the Grimaldi Crüger-Sirsalis 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: Southwest-to-northeast Th (top) and plagioclase (bottom) content profiles across the Serenitatis basin. See Figure 1 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) and plagioclase (bottom) content profiles across the Crisium, Fecunditatis, and Nectaris basins. See Figure 4 for the location of the profile.
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: These figures illustrate the performance predicted by the parametric model for an occultation array targeting MBAs using a configuration of N = 200 telescopes of diameter d = 0.4 m at D = 2 km spacing, near the optimum for a $15,000,000 nominal capital cost. The uncertainty on the rms size of an anomalous gravitational displacement after a 10 yr survey is just σtot = 4.4 cm. At left is the total measurement uncertainty in the occulter position for single-chord observations vs. the occulter diameter and magnitude of the occulted star. Overlaid are several important dividing lines; asteroids below the dt = 2F line have radius below the Fresnel scale, only partially blocking stellar light. Those below the “Unknown” line are too faint to be found in the nominal LSST single-epoch data. Those to the right of the B = 0.5 contour are substantially degraded by “background” light from the night sky and the asteroid's reflected light. Those to the left of the ﹩{\sigma }_{\gamma }={\sigma }_{{\rm{SN}}}﹩ contour are limited by shape noise in determining the CM of the asteroid. Those to the right of the σγ = dT/4 curve have too much photon noise for the occultation to be securely detected. The right-hand plot shows the density of information on gravitational perturbations in the dT–mG plane, which is heavily concentrated in the region with the most numerous occultations—the asteroids near the Fresnel scale, with the faintest stars that produce detectable occultations. The 〈Ne〉 = 4 contour marks the magnitude of the star that will on average be the fourth-brightest occulted by an asteroid of a given size. Occulters with Ne < 4 produce negligible information on gravitational perturbations.
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: Sources of uncertainty in the along-track asteroid position from a single occultation chord plotted vs. magnitude of the occulted star. At left is for an occulter diameter dT = 3 km, at right dT = 0.5 km, both sources at a distance of 2.6 au. Each set of lines shows values of the photon noise σγ for new, quarter, and full Moons, and three different telescope diameters d are plotted in each case. The magenta curve plots the expected final Gaia positional uncertainties σG, and the horizontal line marked “shape noise” marks the floor ﹩{\sigma }_{{\rm{SN}}}﹩ set by the unknown shape and density distribution of the occulter. The “detection threshold” marks the uncertainty σγ = dT/4 that we consider an upper limit for detectable occultations, and the σγ curves terminate at this level. The Fresnel scale is also plotted, and the small triangles mark the G magnitudes at which background counts equal star counts for different moon phases. For the 0.5 km occulter, near the diffraction scale, almost all occultations are limited by photon noise, and the sky brightness is unimportant. For the larger occulter, fainter Gaia stars yield detectable occultations, and the shape noise limits the measurement accuracy for much of the detectable regime.
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: The dashed and dotted lines show the assumed cumulative and differential counts, respectively, for the MBA, Trojan, and TNO populations. The histograms show the differential counts dN/dm of objects currently listed by the Minor Planet Center. Each cumulative curve terminates at a star marking an apparent magnitude mV = 24.4, which is roughly the limit at which objects can be detected in single visits by LSST. The vertical lines mark the Fresnel scale for each population. Note that our models are not intended to match the excesses of larger bodies.
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: Value of σM under which a point source at 400 au would be constrained in 90% of the sky. Black contours are lines of equal cost. The white contour at σM = 0.125M⊕ corresponds to a 5σ detection at 800 au. Top left: results for MBA survey with 2 km distance between telescopes. Top right: Jovian Trojan survey with 5 km distance between telescopes. Bottom: combined MBA and Trojan survey with 5 km distance between telescopes.
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: Summaries of the per-occultation measurement errors (left) and total information (right) for an occultation survey targeting Jovian Trojans. All curves have the same meaning as for the MBA case in Figure 3, except that the color scales are changed. The main configuration change is to move the telescopes further apart from each other to increase the occultation rates for the larger-diameter, sparser Trojan population. Analysis is in Section 3.5.
Paper: An Automated Occultation Network for Gravitational Mapping of the Trans-Neptunian Solar System
Authors: Daniel C. H. Gomes, Gary M. Bernstein
Figure caption: Value of σM for a point source at 400 au that would be achieved or surpassed for 90% of possible directions, for a joint MBA/Trojan survey. Blue line assumes 30 cm telescopes; red line assumes 40 cm. Solid lines include fundamental degeneracy of the tidal signal with the uncertainties of large TNO masses and asymmetries in the Kuiper Belt (KBO floor). Dotted lines show the predicted uncertainty disregarding this limitation.