adsabs/AstroCLIMB huggingface dataset:
Paper: LiDO: Discovery of a 10:1 Resonator with a Novel Libration State
Authors: Rosemary E. Pike, Ruth Murray-Clay, Kathryn Volk, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Ying-Tung Chen, 英同 陳, Arcelia Hermosillo Ruiz, Cameron Semenchuck, Cameron Collyer, J. J. Kavelaars, Lowell Peltier
Figure caption: The fraction of time that clones of 2020 VN40 spend in various orbital states. The duration spent in the first period of resonance can include occupancy in multiple resonant islands, as long as the test particle’s ϕ does not circulate between these modes. The first resonant island includes only the first mode. In the first 30 Myr, 50% of the particles are resonant 66% of the time, and in 1 Gyr, 50% of the particles are resonant 32% of the time. The particles begin to scatter at 39 Myr, and 62% have scattered within 1 Gyr, indicating that the object is likely not stable on Gyr timescales. The amount of time clones spend in each of the leading and trailing island are comparable, while more time is spent in the symmetric island. The libration around 0° is detected for 51% of clones, and while it is not as common as the other libration modes, it does represent a significant fraction of the long-term behavior.
Paper: LiDO: Discovery of a 10:1 Resonator with a Novel Libration State
Authors: Rosemary E. Pike, Ruth Murray-Clay, Kathryn Volk, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Ying-Tung Chen, 英同 陳, Arcelia Hermosillo Ruiz, Cameron Semenchuck, Cameron Collyer, J. J. Kavelaars, Lowell Peltier
Figure caption: The evolution of one of the clones of 2020 VN40 that demonstrates the “eyehole” behavior, particularly between 0.46 and 0.64 Gyr. The evolution of this clone is typical for particles showing resonance around ϕ = 0°. This includes transitions between other resonant islands and ϕ = 0°, as well as the evolution to higher i and lower e before this behavior begins. As in Figure 3, the periods of resonance are marked in blue and the resonance center and resonance bounds are marked. Each libration of ϕ is sampled >50 times.
Paper: LiDO: Discovery of a 10:1 Resonator with a Novel Libration State
Authors: Rosemary E. Pike, Ruth Murray-Clay, Kathryn Volk, Mike Alexandersen, Mark Comte, Samantha M. Lawler, Ying-Tung Chen, 英同 陳, Arcelia Hermosillo Ruiz, Cameron Semenchuck, Cameron Collyer, J. J. Kavelaars, Lowell Peltier
Figure caption: Visualizations of two highly inclined 2:1 resonant particles completing one orbit (equal to one resonant pattern) with an initial resonant angle ϕ = 10°. The particle orbit is color coded by its distance from Neptune throughout the resonant pattern and the gray arrow shows the direction of motion. Neptune’s orbit is shown in blue. The left panel shows a particle with ω = 0° and the right panel a particle with ω = 90°. The black dots show the initial location of conjunction with Neptune, and the connected red dots show the closest approach to Neptune for the orbit with that conjunction. The black X's indicate the location of conjunction with Neptune 10 particle orbits (also 10 resonant patterns) later, showing how the perturbations from Neptune move conjunction (and the resonant angle) either farther away from (left panel) or back toward (right panel) ϕ = 0°.
Paper: An Estimate of the Importance of Electron-stimulated Desorption of Sodium at Mercury
Authors: Rosemary M. Killen, Jason L. McLain, Matthew H. Burger, Orenthal J. Tucker, Liam S. Morrissey, Ronald J. Vervack
Figure caption: Weibull fit to the mid-energy electron flux in the northern and southern hemisphere under northward IMF.
Paper: An Estimate of the Importance of Electron-stimulated Desorption of Sodium at Mercury
Authors: Rosemary M. Killen, Jason L. McLain, Matthew H. Burger, Orenthal J. Tucker, Liam S. Morrissey, Ronald J. Vervack
Figure caption: (a) The electron flux-weighted release rate from 0 to 500 eV based on the fit to the Y. X. Wang et al. (1984) data. (b) The electron flux-weighted release rate from 500 to 900 eV based on the fit to the Y. X. Wang et al. data.
Paper: An Estimate of the Importance of Electron-stimulated Desorption of Sodium at Mercury
Authors: Rosemary M. Killen, Jason L. McLain, Matthew H. Burger, Orenthal J. Tucker, Liam S. Morrissey, Ronald J. Vervack
Figure caption: Almost every data set in the published literature stopped at around 150 eV but showed a clear plateau >100 eV. This is probably due to the penetration depth of the electrons increasing as a function of energy. These data were taken at Georgia Tech by Jason McLain. The two points at ~500 and 550 eV are probably spurious due to the beam overfilling the detector.
Paper: An Estimate of the Importance of Electron-stimulated Desorption of Sodium at Mercury
Authors: Rosemary M. Killen, Jason L. McLain, Matthew H. Burger, Orenthal J. Tucker, Liam S. Morrissey, Ronald J. Vervack
Figure caption: Fits to the calibrated yield per electron (Na+ e–1) for the Y. X. Wang et al. (1984) data to 550 eV.
Paper: An Estimate of the Importance of Electron-stimulated Desorption of Sodium at Mercury
Authors: Rosemary M. Killen, Jason L. McLain, Matthew H. Burger, Orenthal J. Tucker, Liam S. Morrissey, Ronald J. Vervack
Figure caption: Fits to the calibrated yield per electron for 532 < E < 1000 eV based on Y. X. Wang et al. (1984) data.
Paper: A Terminology and Quantitative Framework for Assessing the Habitability of Solar System and Extraterrestrial Worlds
Authors: Dániel Apai, Rory Barnes, Matthew M. Murphy, Tim Lichtenberg, Noah Tuchow, Régis Ferrière, Kevin Wagner, Antonin Affholder, Renu Malhotra, Baptiste Journaux, Allona Vazan, Ramses Ramirez, Abel Méndez, Stephen R. Kane, Veronica H. Klawender
Figure caption: Results of the habitat suitability assessment for Europa’s subsurface ocean considering the methanogens module. The ocean is nearly isothermal in our model (S. D. Vance et al. 2018, 2021, 2023), meaning the temperature is quite suitable for methanogens throughout its entirety. However, though not shown in the figure, the pressure increases steadily with depth and ultimately limits the extent of suitability.
Paper: A Terminology and Quantitative Framework for Assessing the Habitability of Solar System and Extraterrestrial Worlds
Authors: Dániel Apai, Rory Barnes, Matthew M. Murphy, Tim Lichtenberg, Noah Tuchow, Régis Ferrière, Kevin Wagner, Antonin Affholder, Renu Malhotra, Baptiste Journaux, Allona Vazan, Ramses Ramirez, Abel Méndez, Stephen R. Kane, Veronica H. Klawender
Figure caption: Results of the habitat suitability assessment for the Martian subsurface with the methanogens module. While temperatures are too low close to the surface, due to the geothermal heat gradient, the deeper subsurface is warmer. It becomes more suitable for methanogens, up to the point where it begins to exceed the upper temperature limit of methanogen viability.
Paper: A Terminology and Quantitative Framework for Assessing the Habitability of Solar System and Extraterrestrial Worlds
Authors: Dániel Apai, Rory Barnes, Matthew M. Murphy, Tim Lichtenberg, Noah Tuchow, Régis Ferrière, Kevin Wagner, Antonin Affholder, Renu Malhotra, Baptiste Journaux, Allona Vazan, Ramses Ramirez, Abel Méndez, Stephen R. Kane, Veronica H. Klawender
Figure caption: Flowchart of the python implementation of the NEXSS Quantitative Framework for Habitability presented in this paper. The biological and physical models are imported as modules, which are then sorted into an acyclical graph and evaluated many times in a Monte Carlo approach. The functionality of the framework is configured through the modules included, providing a flexibility and upgradability to the framework.
Paper: Simulating Science Operations for a Joint Rover-helicopter Mission Architecture in a Mars Analog Setting
Authors: Kathryn M. Stack, Raymond Francis, Fred J. Calef, Samantha J. Gwizd, Jeffrey F. Schroeder, Joana R. C. Voigt, Thorsteinn Kristinsson, Peter Schroedl, Jahnavi Shah, Matthew Varnam, Catherine D. Neish, Reid P. Perkins, Sashank Vanga, Michael S. Bramble, Andrea Donnellan, Jeffrey T. Osterhout, Michael Tuite, Brett B. Carr, Christopher W. Hamilton
Figure caption: Helicopter imaging surveys downlinked during the simulation. (a) Low-altitude (10 m above ground level) survey covering the approach to Godric’s Hollow acquired by the helicopter on Sol 101. (b) Low-altitude survey acquired on Sol 101 covering the candidate proximity science stop at Godric’s Hollow. (c) High-altitude (20 m above ground level) survey acquired on Sol 101 covering the Specialis Revelio workspace and the slope of Grimmauld Place. (d) Low-altitude survey acquired on Sol 103 of Godric’s Hollow. (e) High-altitude survey acquired on Sol 103 covering Hogsmeade to Chizpurfle. Note the color artifact at the northern end of the survey. (f) Sol 104 low-altitude survey from Chizpurfle to “Bubotuber.” Note the color artifact at the eastern end of the survey. (g) Low-altitude survey acquired on Sol 105 from “Owlery” (south) to Azkaban (north). Survey flight swaths have been localized on Figure 3(b).
Paper: Simulating Science Operations for a Joint Rover-helicopter Mission Architecture in a Mars Analog Setting
Authors: Kathryn M. Stack, Raymond Francis, Fred J. Calef, Samantha J. Gwizd, Jeffrey F. Schroeder, Joana R. C. Voigt, Thorsteinn Kristinsson, Peter Schroedl, Jahnavi Shah, Matthew Varnam, Catherine D. Neish, Reid P. Perkins, Sashank Vanga, Michael S. Bramble, Andrea Donnellan, Jeffrey T. Osterhout, Michael Tuite, Brett B. Carr, Christopher W. Hamilton
Figure caption: Comparison between orbiter, helicopter survey and oblique images, and rover view. (a) Specialis Revelio workspace observed, from left to right, at the scale of orbiter HiRISE, high-altitude helicopter survey, and rover Navcam. The yellow dot shows the location of the rover from which the rover Navcam (far-right panel) was taken, and the yellow lines show an approximation of the FOV of the Navcam mosaic. (b) Western slope of Godric’s Hollow observed, from left to right, at the scale of orbiter HiRISE, low-altitude helicopter survey, oblique helicopter image. (c) Eastern slope of Godric’s Hollow observed, from left to right, at the scale of orbiter HiRISE and low-altitude helicopter. (d) Locator map for sites (a) through (c) showing a portion of the rover and helicopter’s traverse and flight paths, respectively. The yellow line represents the rover traverse, the blue dashed line represents high-altitude helicopter survey paths, and the red dashed line represents low-altitude helicopter survey paths.
Paper: Simulating Science Operations for a Joint Rover-helicopter Mission Architecture in a Mars Analog Setting
Authors: Kathryn M. Stack, Raymond Francis, Fred J. Calef, Samantha J. Gwizd, Jeffrey F. Schroeder, Joana R. C. Voigt, Thorsteinn Kristinsson, Peter Schroedl, Jahnavi Shah, Matthew Varnam, Catherine D. Neish, Reid P. Perkins, Sashank Vanga, Michael S. Bramble, Andrea Donnellan, Jeffrey T. Osterhout, Michael Tuite, Brett B. Carr, Christopher W. Hamilton
Figure caption: Low-elevation (5 m above ground level) oblique images acquired by the helicopter. (a) View to the north of the west-facing slope of Godric’s Hollow acquired on Sol 101. (b) View to the south of the west-facing slope of Godric’s Hollow acquired on Sol 101. (c) Slope south of the Chizpurfle landing site acquired on Sol 102. (d) View toward the southeast taken north of Godric’s Hollow on Sol 103. (e) Base of Hogsmeade slope acquired on Sol 103. (f) View of east-facing scarp west of the Bubotuber landing site acquired on Sol 104; the yellow arrow points to a greenish, layered outcrop at the base of the scarp. (g) View to the northwest of Owlery acquired on Sol 105. (h) View to the west of Azkaban sequence acquired on Sol 105.
Paper: Simulating Science Operations for a Joint Rover-helicopter Mission Architecture in a Mars Analog Setting
Authors: Kathryn M. Stack, Raymond Francis, Fred J. Calef, Samantha J. Gwizd, Jeffrey F. Schroeder, Joana R. C. Voigt, Thorsteinn Kristinsson, Peter Schroedl, Jahnavi Shah, Matthew Varnam, Catherine D. Neish, Reid P. Perkins, Sashank Vanga, Michael S. Bramble, Andrea Donnellan, Jeffrey T. Osterhout, Michael Tuite, Brett B. Carr, Christopher W. Hamilton
Figure caption: 2018 Rainbow Basin UAS image acquisition and derived data products for the ROI. (a) Image locations collected from the UAS in flight at Rainbow Basin. (b) Analog HiRISE orthomosaic of the Rainbow Basin field site. (c) DEM of the processed UAS images. (d) 1 m slope map derived from the UAS DEM.
Paper: Simulating Science Operations for a Joint Rover-helicopter Mission Architecture in a Mars Analog Setting
Authors: Kathryn M. Stack, Raymond Francis, Fred J. Calef, Samantha J. Gwizd, Jeffrey F. Schroeder, Joana R. C. Voigt, Thorsteinn Kristinsson, Peter Schroedl, Jahnavi Shah, Matthew Varnam, Catherine D. Neish, Reid P. Perkins, Sashank Vanga, Michael S. Bramble, Andrea Donnellan, Jeffrey T. Osterhout, Michael Tuite, Brett B. Carr, Christopher W. Hamilton
Figure caption: Images of the helicopter’s landing sites acquired by the nadir-pointed camera. (a) Flutteryby Bush landing site imaged on Sol 101. (b) Cleansweep landing site imaged on Sol 102. (c) Chizpurfle landing site imaged on Sol 103. (d) Bubotuber landing site imaged on Sol 104.
Paper: Lucy Mission Search Plans for Activity around Its Jovian Trojan Flyby Targets
Authors: S. Alan Stern, Carly Howett, Neil Dello Russo, Harold A. Weaver, James F. Bell, Dennis Reuter, Amy Simon, Hannah Kaplan, Keith Noll, John Spencer, Simone Marchi, Hal Levison
Figure caption: Testing the size detectability limits for boulders near Dinkinesh. A composite of 8300 ms Dinkinesh flyby images (the frame covers 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩29 × 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩29; Dinkinesh and Selam are the two brightest objects in the field) obtained on UT 2023 November 1, displayed using an inverse hyperbolic sine function stretch from 0 to 100 DN. Synthetic objects are marked with red circles. Here, one L'LORRI pixel subtends 79 m projected distance at Dinkinesh (range to target ∼16,000 km) and has an SPA = 59﹩\mathop{.}\limits^{\unicode{x000b0}}﹩24. Fake objects were inserted at 36 different locations with peak signals 3σ, 5σ, and 10σ above the nominal noise level (1σ ≈ 0.36 DN); it was found that even 3σ objects appear to be detectable over most of the FOV. Fake objects had Vmag = 15.09, 14.54, 13.79 for the 3σ, 5σ, and 10σ cases, respectively, assuming for their phase law that G = 0.378, geometric albedo pv = 0.287, and an S-type asteroid spectral energy distribution. (S-type asteroids have moderately steep slope at wavelengths shorter than 0.7 μm; moderate to weak absorption features around 1 μm and 2 μm, indicating the presence of silicates; and a broad but shallow absorption feature centered near 0.63 μm, sometimes present. They have similar spectral characteristics to certain stony meteorites, suggesting a possible connection. S-types are dominant in the near-Earth population and the inner asteroid belt (<2.2 au from the Sun) and are common in the central belt (∼3 au) but rare farther out. Examples include (3) Juno, (15) Eunomia, (7) Iris, and (433) Eros.) This image is a composite of 10 L’LORRI images with a FOV of ∼0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩29. Dinkinesh is the brightest spot and is about 0.82 × 0.45 × 0.77 km in extent.
Paper: Lucy Mission Search Plans for Activity around Its Jovian Trojan Flyby Targets
Authors: S. Alan Stern, Carly Howett, Neil Dello Russo, Harold A. Weaver, James F. Bell, Dennis Reuter, Amy Simon, Hannah Kaplan, Keith Noll, John Spencer, Simone Marchi, Hal Levison
Figure caption: Subsection of the MVIC FOV showing possible annuli addition configurations. Top: coadding profile for a target centered in the FOV (used for distant observations). A 601 × 601 pixel example is given, which could be the full in-track spatial extent but would only be a small part (601 of 5000 pixels) of the cross-track extent. The white circle shows the extent of the 10 pixel annulus that is summed over. The observation used is a violet MVIC observation of Dinkinesh taken on 2023 November 1 at 16:53:27.778 UTC. Bottom: coadding profile of a target centered outside the FOV (used for close observations). Only a subset of the MVIC FOV is shown (64 × 300 pixels). In this example, the extent of the annuli is from the inner to the outer circle, which have diameters of 270 and 200 pixels (shown at a width of 1 pixel). The target (not shown) is assumed to be at the center of the annuli, outside the FOV. There is no scale shown, because different images have differing scales during approach to and then departure from each flyby target.
Paper: Lucy Mission Search Plans for Activity around Its Jovian Trojan Flyby Targets
Authors: S. Alan Stern, Carly Howett, Neil Dello Russo, Harold A. Weaver, James F. Bell, Dennis Reuter, Amy Simon, Hannah Kaplan, Keith Noll, John Spencer, Simone Marchi, Hal Levison
Figure caption: Dinkinesh radial brightness profile showing counts in pixels with increasing radial distance from the center of brightness (blue circles) obtained on UT 2023 October 26 using a coadd of eight 20 s images. For these data, the range to target was 2.4 × 106 km and the Sun–probe angle (SPA) was 117﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5. Both a PSF brightness profile with no coma (black curve) and a coma brightness profile (red curve), assuming a spherical symmetric coma with a 1/r brightness profile (where r is the projected distance from the peak) are shown. The observed Dinkinesh profile is consistent with no or little coma. A model brightness represented by 90% PSF and 10% coma sets a reasonable upper limit to a dust coma, yielding an upper limit for Afρ < 0.94 cm at SPA = 117﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5, and Afρ < 0.72 cm corrected to SPA = 0° using the D. Schleicher (2010) phase law for ensemble cometary dust.
Paper: A JWST Study of CO2 on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, Matthew Belyakov, M. Ryleigh Davis, Ashma Pandya
Figure caption: JWST spectra of the satellites of Saturn, in order of distance from Saturn. Titan’s location is marked to distinguish the inner and outer satellite systems. For synchronously rotating satellites, the leading hemisphere is shown in black, while the trailing is in red. For Enceladus, only the leading was observed. For the nonsynchronous Hyperion and Phoebe, only a single observation was made. The leading/trailing hemisphere spectra of individual satellites are scaled correctly relative to each other, but the scaling of the spectra of the different satellites is arbitrary. Uncertainties in the spectra can be estimated from the scatter in the data of these generally smoothly varying spectra.
Paper: A JWST Study of CO2 on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, Matthew Belyakov, M. Ryleigh Davis, Ashma Pandya
Figure caption: An average of the continuum-removed spectra of the leading and trailing hemispheres of Mimas and Tethys and the leading hemispheres of Dione and Rhea, in black, and of the trailing hemispheres of Dione and Rhea, in red. The lines at the bottom show measured wavelengths of CO2 in different states, including in pure crystalline form and trapped as clathrate in crystalline water ice (A. Oancea et al. 2012), trapped in amorphous ice (S. A. Sandford & L. J. Allamandola 1990; Ó. Gálvez et al. 2008), and physisorbed onto minerals (C. Hibbitts & J. Szanyi 2007), which can lead to a wide range of wavelengths. The shorter-wavelength 4.2487 μm line associated with the darker hemispheres of Dione and Rhea appears to have no corresponding absorption in the 2.7 μm region.
Paper: A JWST Study of CO2 on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, Matthew Belyakov, M. Ryleigh Davis, Ashma Pandya
Figure caption: The region near the 4.27 μm ν3 band of CO2 for the Saturnian satellites. The top row shows the leading hemispheres, while the bottom shows the trailing. For nonsynchronous Hyperion and Phoebe, only a single spectrum is shown. Each spectrum was divided by a local continuum to examine relative absorption, and the uncertainties can be estimated by examining the scatter of the data about the continuum. All satellites have absorptions near 4.25 and 4.27 μm or both, though the central wavelengths of the absorption on the outer satellites differ slightly from those of the inner satellites. For the inner satellites, dashed lines are shown at 4.249 and 4.272 μm, while for the outer satellites, dashed lines are shown at 4.249 and 4.273 μm.
Paper: A JWST Study of CO2 on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, Matthew Belyakov, M. Ryleigh Davis, Ashma Pandya
Figure caption: A comparison of CO2 detected on the Saturnian satellites with the icy Galilean satellites. Dashed lines are shown at 2.6975 and 2.708 μm and at 4.25 and 4.27 μm for reference. Ganymede and Callisto have no JWST observations at 2.7 μm with which to compare.
Paper: A JWST Study of CO2 on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, Matthew Belyakov, M. Ryleigh Davis, Ashma Pandya
Figure caption: Continuum-removed views of the 2.7 and 4.27 μm regions of the spectra of the outer satellites. The colored lines show the wavelengths of various forms of CO2, as in Figure 4. The black line again shows the wavelength of crystalline CO2, and the green lines show those of CO2 clathrates. The red line (not shown in Figure 4), which is consistent with the wavelength seen in the high signal-to-noise Iapetus data, is the wavelength of CO2 formed in irradiated organic material.
Paper: A JWST Study of CO2 on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, Matthew Belyakov, M. Ryleigh Davis, Ashma Pandya
Figure caption: Continuum-divided region of the spectra containing the expected 13CO2 absorption feature. Each spectrum is offset by 0.07 units for clarity. A single Gaussian fit to the data is used to determine detection limits or the strength of the absorption. The vertical red bar shows the 1σ uncertainty on the line strength.
Paper: A JWST Study of CO2 on the Satellites of Saturn
Authors: Michael E. Brown, Samantha K. Trumbo, Matthew Belyakov, M. Ryleigh Davis, Ashma Pandya
Figure caption: Continuum-divided spectra of the 2.7 μm region near the ν1 + ν3 combination band of CO2. Most satellites have a broad absorption near 2.71 μm, while Hyperion and the bright trailing hemisphere of Iapetus have a narrow absorption near 2.70 μm. Phoebe and the dark leading hemisphere of Iapetus have no discernible absorption. All spectra are shown with dashed lines at 2.6975 and 2.708 μm for clarity.
Paper: A Large Outburst, Coma Asymmetries, and the Color of Comet 243P/NEAT
Authors: Michael S. P. Kelley, Silvia Protopapa, Dennis Bodewits, Aren N. Heinze, Youssef Moulane, Quanzhi Ye, 泉志 叶, Bryce Bolin, Simon Conseil, Tony L. Farnham, Lori Feaga, Xing Gao, 兴 高, Chih-Hao Hsia, 志浩 夏, Emmanuel Jehin, Shrinivas R. Kulkarni, Russ R. Laher, 主嶺亞 良, Tim Lister, Frank J. Masci, Josiah Purdum, Bin Yang, 彬 杨
Figure caption: Light curve of comet 243P/NEAT vs. time from perihelion (T − TP) based on all photometry within a 104 km radius aperture. All data have been offset to the r band using the measured colors of the coma (Section 4.2). Two lines of constant A(0°)fρ are shown to emphasize the change in brightness as the comet moved through opposition at T − TP = 57 days (dotted and dashed lines). Two outbursts are identified and labeled with their estimated dates (UTC), and a third is labeled as a tentative event. A thin vertical line marks the time of our near-infrared spectrum with the SpeX instrument. The best-fit light curve for the larger outburst is also shown (solid line).