adsabs/AstroCLIMB huggingface dataset:
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Expected number of LSST detections for Jurads smaller than radius r vs. exocomet physical size, expressed as a cumulative value N LSST( < r). For this plot, we choose ﹩{r}_{\min }=60\,{\rm{m}}﹩ in the SFD and display the results for various power-law slopes q.
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Expected total number of LSST detections for Jurads of all sizes, given the ﹩{r}_{\min }﹩ and q of the SFD. In these calculations, we have assumed the fiducial values for exo–Oort Cloud populations from Section 4 and the second LSST detection model from Section 5.
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Ice retention fractions against the AGB wind for small bodies composed of pure substances. The contours (from left to right) represent surviving ice fractions f ∈ [0.0, 0.25, 0.5, 0.75]. Importantly, the exo–Oort Clouds under consideration in this study have an inner edge near 1000 au (the upper limit of this figure).
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Masses of the known extrasolar planets (or minimum mass in the case of nontransiting planets detected by the radial velocity method) vs. orbital period, where the markers have been colored by their Safronov number (Equation (51)). The solar system’s planets are denoted with large diamond markers and their corresponding symbols.
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: Estimated landmark location corrections and uncertainties for the combined solution. East/west (positive eastward) estimated deviations (a) and 1σ uncertainties (b). North/south (positive northward) estimated deviations (c) and 1σ uncertainties (d). Altitude (positive radially) estimated deviations (e) and 1σ uncertainties (f).
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: OLA performance for Orbital A vs. Iota (a) and the off-nadir angles (b). The HELT mean and 1σ standard deviation is given in orange. Histograms of the data per bin are given in blue.
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: Orbital A landmark OpNav residuals in the camera pixel (a) and line (b) directions. The bluish green dots are the residuals, the black line is the mean of the residuals, and the orange lines indicate the 1, 2, and 3σ standard deviations around the mean. The residuals are plotted vs. the emission angle, the illumination angle, and the correlation score of the landmark. A histogram of the data distribution is provided for each plot in blue.
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: Standard deviation of OpNav residuals projected on the surface in centimeters per landmark for Orbital A (a), Orbital B (b), Orbital C (c), Orbital R (d), and Recon B (e). Gray indicates that there were fewer than five images of that landmark and no statistics were calculated. No color indicates that there were no images of that landmark.
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: OLA performance for Orbital B (a, b) vs. Iota (a) and the off-nadir angles (b). The LELT mean and 1σ standard deviation is given in green. Histograms of the data per bin are given in blue.
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: Estimated landmark location S/N for the combined solution. East/west (positive eastward) estimated S/N (a), North/south (positive northward) estimated S/N (b), and altitude (positive radially) estimated S/N (c).
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: Landmark OpNav residual 3σ standard deviations per phase in the camera pixel (a) and line (b) directions. Residual 3σ standard deviations are plotted vs. the emission angle, the illumination angle, and the correlation score of the landmark.
Paper: Post-flight Evaluation of Lidar-based Digital Terrain Models for OSIRIS-REx Navigation at Bennu
Authors: Jason M. Leonard, Jeroen L. Geeraert, Leilah K. McCarthy, Coralie D. Adam, Peter G. Antreasian, Olivier S. Barnouin, Michael G. Daly, Jeffrey A. Seabrook, Dante S. Lauretta
Figure caption: Number of images in this analysis that were correlated per landmark for NavCam 1 (a) and MapCam (b). Landmarks without any color were not correlated in a single image for the duration of data listed in Table 3.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Compilation of the spectral identification color-composite maps and the outlined landing-site reference units used in this work for the determination of crater frequencies. We show the maps for all landing sites for which Luna and Apollo missions sampled the Moon. All the landing-site reference units are outlined in white, all landing sites are localized with a filled red dot, and the astronaut tracks are added in black when the map scale allows for visibility. The color maps are using spectral data collected with the Moon Mineralogical Mapper (M3) on board the Chandrayaan-1 mission. Data overlay the morphology imaged by the terrain camera (TC) on board the Kaguya mission. The mapping method and spectral criteria details are fully described in Bultel & Werner (2023). Detection according to the spectral criteria is displayed using the red (R), green (G), and blue (B) channels; the specific used criteria are given here for each landing site. (a) Apollo 12 landing site with a color-coded map (R, IBD1000; G, IBD2000; B, BD2250). (b) Apollo 15 (R, BD1900; G, BD2300; B, IBD1000). (c) Luna 24 (R, IBD1000; G, BD2250; B, BD2300). (d) Luna 16 (R, IBD1000; G, BD2020; B, BD2250). (e) Apollo 11 (R, IBD1000; G, BD1900; B, BD2250). (f) Apollo 17 (R, IBD1000; G, BD1900; B, BD2300). (g) Apollo 14 (R, BD930; G, BD1250; B, BD1900). (h) Apollo 16 (R, IBD1000; G, BD1900; B, BD2300). (i) Luna 20 (R, BD1900; G, BD2200; B, IBD1000). Note the Chang’E 5 site is not included, because no spectral analysis was performed.
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Summary display of the new calibration pairs and the thereof proposed analytical function for the new (cyan) cratering-chronology model. The respective calibration pairs are shown here with uncertainties in the crater frequency and assigned age. The upper and lower bound envelope is so that the calibration uncertainties are captured. Furthermore, we show the age range of samples in cases, for which we have not assigned an age for the calibration. At the young range (below one billion years), calibration pairs marked in red stem from Hiesinger et al. (2012). The current standard cratering-chronology model by Neukum (1983) is plotted (black) together with other more recent models (gray).
Paper: Review and Revision of the Lunar Cratering Chronology—Lunar Timescale Part 2
Authors: Stephanie C. Werner, Benjamin Bultel, Tobias Rolf
Figure caption: Summary display of the new calibration pairs and the thereof proposed analytical function for the new (cyan) cratering-chronology model together with the standard cratering-chronology calibration (black) by Neukum (1983), and other more recent models (gray).
Paper: Pre-landing Assessment of the Surface and Shallow Subsurface Thermal Setting of Mare Crisium of the Moon for the Heat Flow Measurement Planned on the Blue Ghost 1 Mission
Authors: Seiichi Nagihara
Figure caption: Mosaic of the Lunar Reconnaissance Orbiter Camera (LROC) Wide Angle Camera images that include the landing sites of Apollo 15, Apollo 17, and Blue Ghost 1; https://wms.lroc.asu.edu/lroc/view_rdr_product/WAC_GLOBAL_E300N0450_100M. The areas classified as mare (Nelson et al. 2014) are shaded in pink. A more detailed map of the area around A17 is shown in the lower left corner.
Paper: Pre-landing Assessment of the Surface and Shallow Subsurface Thermal Setting of Mare Crisium of the Moon for the Heat Flow Measurement Planned on the Blue Ghost 1 Mission
Authors: Seiichi Nagihara
Figure caption: Model-estimated temperature vs. depth curves for A17 (colored solid lines) showing the fluctuation of the subsurface temperature distribution in 1 month. The equilibrium temperatures obtained from Apollo 17 Probe 1 are shown as red squares. The red line simply connects the temperature data points.
Paper: Pre-landing Assessment of the Surface and Shallow Subsurface Thermal Setting of Mare Crisium of the Moon for the Heat Flow Measurement Planned on the Blue Ghost 1 Mission
Authors: Seiichi Nagihara
Figure caption: Comparison of the model parameter values by V2012 (blue), H2017 (green), and the present study for A17 (red). From left to right, density (ρ) vs. depth, contact thermal conductivity (K  c ) vs. depth, bulk thermal conductivity (K) at 255 K vs. depth, the radiative heat transfer coefficient (B) vs. depth, and thermal diffusivity vs. depth. The gray rectangles indicate the range of values reported for the Apollo 17 site (Langseth et al. 1976).
Paper: Pre-landing Assessment of the Surface and Shallow Subsurface Thermal Setting of Mare Crisium of the Moon for the Heat Flow Measurement Planned on the Blue Ghost 1 Mission
Authors: Seiichi Nagihara
Figure caption: Diviner channel 7 (red) temperatures plotted against the local time of A17 (A) and BG1 (B). For the former, the surface temperature of the heat flow probe deployment site by Keihm et al. (1973) is also shown in black.
Paper: Pre-landing Assessment of the Surface and Shallow Subsurface Thermal Setting of Mare Crisium of the Moon for the Heat Flow Measurement Planned on the Blue Ghost 1 Mission
Authors: Seiichi Nagihara
Figure caption: Comparison of the model-estimated surface temperatures (blue lines) and Diviner observations (open circles) for the Apollo 17 ALSEP site (Figure 2). The parts indicated by the dashed boxes are shown in Figure 8 in more detail.
Paper: Pre-landing Assessment of the Surface and Shallow Subsurface Thermal Setting of Mare Crisium of the Moon for the Heat Flow Measurement Planned on the Blue Ghost 1 Mission
Authors: Seiichi Nagihara
Figure caption: The ground-projected LRO-Diviner flyover temperature measurement locations (yellow dots) for the Apollo 17 (A) and Blue Ghost 1 (B) landing sites are plotted over the LROC images. On Apollo 17, the heat flow probes were deployed as part of the Apollo Lunar Surface Experiment Package (ALSEP).
Paper: Pre-landing Assessment of the Surface and Shallow Subsurface Thermal Setting of Mare Crisium of the Moon for the Heat Flow Measurement Planned on the Blue Ghost 1 Mission
Authors: Seiichi Nagihara
Figure caption: (Top) History of the solar elevation (blue) and distance (orange) and (bottom) solar irradiance at the proposed Blue Ghost 1 landing site for 1980–2021.
Paper: Pre-landing Assessment of the Surface and Shallow Subsurface Thermal Setting of Mare Crisium of the Moon for the Heat Flow Measurement Planned on the Blue Ghost 1 Mission
Authors: Seiichi Nagihara
Figure caption: Magnified views of the parts of Figure 7 that are indicated by the dashed boxes.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: NS flux ratio spectra (average ratio of I/Fs 30° above and below the NSA boundary latitude) from select flybys over a Titan half year. Note that wavelengths where methane absorbs (e.g., 0.89 μm) tend to show an inverted NS flux ratio relative to methane windows (e.g., 0.93 μm). The Ta and T8 spectra show distinct features, while the T114 and 278TI spectra show those same features with a flipped concavity. Changing illumination and viewing conditions can shift these NS ratio spectra vertically. Changing illumination cannot, however, invert absorption lines as we see happen from northern winter into northern spring at 0.89 μm. Thus much of the variation in spectral shape can be attributed to varying atmospheric structure. The other spectra from T31 to T108 that were recorded closer to the vernal equinox show subdued or nonexistent features, indicating a more uniform meridional haze profile for Titan.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: Titan's NSA is evident in two individual band images from the same VIMS cube in Figure 1 (CM_1634082284_1). In the left cube, the southern hemisphere appears brighter at blue wavelengths. In contrast, the NSA reverses in the right image within a methane absorption band at 0.886 μm. Vertical striping artifacts are present in the images.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: Here we present a flowchart of the image processing procedures to obtain the NSA boundary latitude and the NS flux ratio from an individual VIMS cube image.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: Meridional disk brightness (I/F) profiles across Titan from select Cassini flybys over a Titan half year along with published HST NS ratio spectra in the top panel. The top plot shows the profile at 0.550 μm and the bottom at 1.003 μm. The error bars represent the NS boundary location and its uncertainty for each flyby at that wavelength. The shape and trends of the profile did not exhibit much change between 2004 and 2007 (Ta–T31). With the onset of the vernal equinox in T61, the meridional profile developed dramatic changes resulting from both varying solar illumination and dynamic atmospheric structure, with a near-complete latitudinal reversal by 2017 (278TI). It is important to note that in T85, 278TI, and 283TI, drop-offs are removed as the disks are terminated. Additionally, the coaddition of longitudinal data tends to resolve the NSA boundary poorly, resulting in sometimes indistinct NSA boundary transitions, like in 278TI.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: A T62 image of VIMS cube CM_1634082284_1 taken on 2009 October 12 shows a typical low-phase-angle view of Titan with the NSA at visible wavelengths from the VIMS instrument (VIMS-V). The colors are an approximation of true color using the VIMS-V channels. The overall orange color comes from the spectral and scattering properties of the haze particles as well as atmospheric absorption and Rayleigh scattering, which predominate at bluer wavelengths. North is upwards in the image.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: NS boundary latitudes from select flybys that represent a Titan half year. As expected, the data show no evidence of a relationship between wavelength and NS boundary latitude. Even in wavelengths where the NS flux ratio is 1, gradient-based indicators for the NS boundary remain due to the wide sampling latitudinal range (±30°).
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: The top and bottom panels show T67 VIMS cube images at 0.886 and 1.003 μm, respectively. These maps show a visible tilt in the NSA boundary. Some mapping artifacts and voids have been removed to show only the parts of Titan visible during the flyby. The red line tracks individual measurements of the NSA boundary latitude for image columns where the NSA is evident. The blue line shows a linear regression model fit to those NSA boundary latitudes to determine a tilt angle for the NSA boundary. The linear fit indicates that at 0.886 μm, the NSA boundary is located 12°S ± 3° with an angle of −0.°81 ± 0.°22. At 1.003 μm, the NSA boundary is at 12°S ± 0° with an angle of −0.°55 ± 0.°23. These fits and their errors assume a linear tilt to the NS boundary, as opposed to a spherical offset of the atmospheric pole from the rotational pole. Therefore the reported measurement precision may underrepresent the true accuracy after accounting for systematic errors due to our underlying tilt assumption.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: A sequence of false-color (RGB: 0.725, 0.886, 1.003 μm, respectively), near-infrared VIMS cube images show the fading and flipping of the NSA boundary over a Titan half year. The orbital diagram is adapted from Figure 1 of Seignovert et al. (2021) to provide context with the Titan seasons. The red dashed lines indicate the equator. The Ta image has a sharp brightness contrast between the bright (violet) and dark (indigo) hemispheres. The NSA contrast was reduced, but the NSA boundary line was still visible below the equator by 2012 (T85). The NSA boundary line is lost in the T101 image, but some purple color remains. The lack of the NSA persists in the T114 image with a uniform (white) disk brightness profile. The NSA does not return until the near-end of the Cassini mission in mid-2017 in the 278TI and 283TI images. The bright and dark hemispheres have flipped with the subtle boundary line above the equator.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: The time line of the NSA boundary latitude as measured by instruments aboard Titan flyby missions and space telescopes. Before 2000, there was more uncertainty in the NSA boundary due to the reliance on noisier HST images. The period of rapid change applies to the early HST observations of seasonal NSA changes reported in Lorenz et al. (2001). Nearly half of Titan’s 29.5 yr seasonal cycle is precisely documented with the new VIMS NSA boundary data set. A period of a stable NSA from 2004 to 2014 was halted by an abrupt change in the fading of the NSA boundary from 2014 until its reversal and reappearance in 2017. Note that small systemic variations within the uncertainties exist in the NSA boundary latitude estimations between the Cassini ISS and VIMS images from 2004 to 2007. L  s  refers to solar longitude: 0° at Titan’s northern spring equinox.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: Cylindrical projection maps of the high-contrasting band for every flyby with a faint demarcation of the equator in red. The color bar shows the brightness difference between two vertically shifted images. The dark band is visible in most flybys. We note two distinct bands in the T108 image, which hints at the lack of an NSA boundary.
Paper: Titan’s North–South Haze Asymmetry Ratio and Boundary at Visible Wavelengths over the Cassini Mission
Authors: Aadvik S. Vashist, Michael F. Heslar, Jason W. Barnes, Corbin Hennen, Ralph D. Lorenz
Figure caption: Individual VIMS cube images at 0.886 μm taken within one year of each other at a low (37°) and high (88°) phase angle, respectively. The right plot (C) shows a comparison of the meridional profiles for the two phase angles in several methane windows. At blue and green wavelengths, there is little change between the corresponding low- and high-phase profiles. Differences between the two phases increase at longer wavelengths, while the gradient in I/F vs. latitude becomes more shallow at the longest wavelengths. The red dashed lines in (A) and (B) indicate the longitude of the meridional profiles from each image.
Paper: Orbits and Masses of the Small Satellites of Pluto
Authors: Simon B. Porter, Robin M. Canup
Figure caption: Inferred ice fraction for Nix as a function of porosity, using the density estimate in Figure 1 and Equation (4). The blue line shows this relationship, with the blue shaded area covering ±1σ uncertainty in Nix’s density. The gray shaded areas show the estimated ice mass fractions for Pluto and Charon from McKinnon et al. (2017). From its high albedo and ice-dominated surface spectra, the ice mass fraction of Nix is not expected to be lower than Pluto or Charon, but such values are shown here for completeness.
Paper: Interstellar Comets from Post-main-sequence Systems as Tracers of Extrasolar Oort Clouds
Authors: W. Garrett Levine, Aster G. Taylor, Darryl Z. Seligman, Devin J. Hoover, Robert Jedicke, Jennifer B. Bergner, Gregory P. Laughlin
Figure caption: Object-by-object comparison of final eccentricities e J,f  for test particles in the validation rebound simulations that were run with different mass-loss time steps t  s . The y-axis shows e J,f  for t  s  = {10, 100, 1000, 2500} yr vs. e J,f  for the t  s  = 1 yr simulation on the x-axis. Quadrants are labeled I-IV, with regions II and IV representing parameter space where particles are bound (e < 1) in one simulation and unbound (e > 1) for the other simulation.