adsabs/AstroCLIMB huggingface dataset:
Paper: Global Hall MHD Simulations of the Solar Wind Implantation Flux on the Lunar Surface
Authors: Lianghai Xie, Lei Li, Huizi Wang, Binbin Tang, Jindong Wang, Yiteng Zhang, Quanqi Shi, Bin Zhou, Yongyong Feng
Figure caption: (a) The map of the magnetic field strength on the lunar surface, obtained from the 450° spherical harmonic model (Tsunakawa et al. 2015). (b) The map of the average number flux (J avg) over one lunation. (c) The map of the average energy flux (E f,avg) over one lunation. The rectangles indicate the locations of the lunar swirls examined by Blewett et al. (2011) and the circles indicate the locations of the other lunar swirls found by Denevi et al. (2016), accompanied by the names of nearby magnetic anomalies.
Paper: Global Hall MHD Simulations of the Solar Wind Implantation Flux on the Lunar Surface
Authors: Lianghai Xie, Lei Li, Huizi Wang, Binbin Tang, Jindong Wang, Yiteng Zhang, Quanqi Shi, Bin Zhou, Yongyong Feng
Figure caption: (a)–(d) The simulation results of the magnetic field (B), the normalized number flux (J/J sw), the penetrating efficiency (η sw), and the normalized kinetic energy (E  k /E k,sw) of the solar wind on the lunar surface, respectively. The white dotted lines indicate the terminators during this period, and the solid dot marks out the location of CE-4.
Paper: Global Hall MHD Simulations of the Solar Wind Implantation Flux on the Lunar Surface
Authors: Lianghai Xie, Lei Li, Huizi Wang, Binbin Tang, Jindong Wang, Yiteng Zhang, Quanqi Shi, Bin Zhou, Yongyong Feng
Figure caption: Comparisons of the implantation fluxes in the southern hemisphere and the northern hemisphere. (a) and (b) Comparisons of the average number flux and the average energy flux, respectively. The magenta, yellow, and gray dots indicate the average fluxes in the northern hemisphere, with latitude ranges of 0°–30°, 30°–60°, and 60°–90°, respectively. The blue, green, and red dots indicate the average fluxes in the southern hemisphere, with latitude ranges of 0°–30°, 30°–60°, and 60°–90°, respectively.
Paper: Global Hall MHD Simulations of the Solar Wind Implantation Flux on the Lunar Surface
Authors: Lianghai Xie, Lei Li, Huizi Wang, Binbin Tang, Jindong Wang, Yiteng Zhang, Quanqi Shi, Bin Zhou, Yongyong Feng
Figure caption: (a) The maps of implanted number flux at different phase angles, in which the number fluxes are normalized by the solar wind number flux. (b) The maps of implanted energy flux at different phase angles, in which the energy fluxes are normalized by the solar wind energy flux.
Paper: Global Hall MHD Simulations of the Solar Wind Implantation Flux on the Lunar Surface
Authors: Lianghai Xie, Lei Li, Huizi Wang, Binbin Tang, Jindong Wang, Yiteng Zhang, Quanqi Shi, Bin Zhou, Yongyong Feng
Figure caption: Different locations of the Moon during its orbit around the Earth. The color contours show the number densities of the Earth's magnetosphere obtained from the global PPMLR-MHD simulation. The black dots show the different lunar locations in the GSE XY-plane with intervals of 5°. The circled dots indicate the locations with intervals of 45°, whose implantation flux maps are shown in this work.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: These images of the Mare Ingenii swirl region (top) show the two swirl areas (I and II) examined in more detail in this study. Both regions are 10 km across. The images were extracted from the LROC quickmap (http://quickmap.lroc.asu.edu) provided by Arizona State University. The crater at the center of the top image is located at 162° longitude, −35° latitude.
Paper: Spectrophotometric and Topographic Correlations within the Mare Ingenii Swirl Region: Evidence for a Highly Mobile Lunar Regolith
Authors: Deborah Domingue, John Weirich, Frank Chuang, Amanda Sickafoose, Li Hsia Yeo, Samuel Courville, Eric Palmer, Robert Gaskell
Figure caption: Images used to study swirl area I shown in Figure 1. The phase angle range for all images in this study area is <71°. The black box denotes the total area examined, where black space indicates no coverage by the image in that portion of the study area. The range in reflectance for the region imaged is shown under the image ID. Photometric angle values across each image are listed in Table 2.
Paper: Dust Properties of Comets Observed by Spitzer
Authors: David E. Harker, Diane H. Wooden, Michael S. P. Kelley, Charles E. Woodward
Figure caption: Two models of the spectrum of comet C2006P1-20070906 (C/2006 P1 (McNaught)) at r  h  = 4.0 au (two models), in flux density (W m2 μm−1) vs. wavelength (μm), showing how models can exhibit degeneracies for comets at r  h  ≥ 3.5 au. Degeneracies in the parameters for the models may occur between amorphous carbon and amorphous silicates at these r  h . Each panel consists of three plots, showing the best-fit model's amorphous carbon (orange solid line), amorphous olivine (cyan sold line), amorphous pyroxene (blue solid line), crystalline olivine (green solid line), and crystalline pyroxene (pink solid line). The top plots contain the observed spectrum (black symbols) and the total thermal model (red solid line). In the middle plots the amorphous carbon component has been subtracted from the total and observed spectra, resulting in the residual silicate component. Similarly in the bottom plots, all amorphous species have been removed resulting in the residual cyrtsalline silicate component. (a) Model fitted to SLLL, dominated by amorphous carbon with some contribution from amorphous silicates. (b) Model fitted to SLLL–SL, fitted solely by amorphous olivine. The vertical lines designate the wavelength positions of features from various refractory species (from left to right) at 9.30 (pink; crystalline pyroxene), 8.20 and 8.47 (orange dotted; PAH features), 10.05 (green; crystalline olivine), 10.50 (pink; crystalline pyroxene), 11.15 (green; crystalline olivine), and 19.50 μm (green; crystalline olivine). The latter feature is also near the order splicing of the IRS. (The data used to create these figures are available.)(The data used to create this figure are available.)
Paper: Dust Properties of Comets Observed by Spitzer
Authors: David E. Harker, Diane H. Wooden, Michael S. P. Kelley, Charles E. Woodward
Figure caption: Projection into 3D and 2D ternary diagram of five model parameters for six comets showing changes in fitted parameters from SLLL to SLLL–SL (Figure 7). From SLLL to SLLL–SL (shown by arrows), CS increases and amorphous carbon (AC) decreases, where (a) and (b) respectively show the changes in amorphous silicates and CS by rods perpendicular to the {AC, AS, CS} plane in 3D. (c) and (d) Ternary diagrams showing changes from SLLL → SLLL–SL, with the mean model parameters as open squares and open circles. The extent of a 1000 (1K) subset of 10,000 Monte Carlo (MC) trials as dots. The SLLL parameter space is more tightly constrained compared to SLLL–SL (see Section 4.5).
Paper: Dust Properties of Comets Observed by Spitzer
Authors: David E. Harker, Diane H. Wooden, Michael S. P. Kelley, Charles E. Woodward
Figure caption: Spearman rank tests (for correlations). (a) The Spearman rank test correlation matrix for each SLLL, with check marks where the p-value (permutation test) is <0.003 (3σ). (b) The KDE plots for the mean parameters for those parameter pairs where the plus signs indicate those with a permutation test p-value of <0.003 (3σ). (c) The KDE for 1000 Monte Carlo trials.
Paper: Dust Properties of Comets Observed by Spitzer
Authors: David E. Harker, Diane H. Wooden, Michael S. P. Kelley, Charles E. Woodward
Figure caption: Unidentified 14 μm feature. Seven spectra have been normalized by their best-fit thermal models to emphasize deviations from the model. Five of the spectra (C/2006 P1, C/2003 T4, C/2003 K4, 88P, and 78P) were identified with our AIC tests, which compared model fits with and without the spectral data from 13.5 to 15.7 μm (marked with a thick horizontal bar). A vertical dashed line marks a proposed feature peak at 14.45 μm. Two additional high-quality spectra (67P and 37P) are shown for comparison. These additional comets may also have evidence for a weak feature.
Paper: Dust Properties of Comets Observed by Spitzer
Authors: David E. Harker, Diane H. Wooden, Michael S. P. Kelley, Charles E. Woodward
Figure caption: Grain size distribution slope (N) vs. peak grain size, a  p (μm), colored by the porosity parameter D that characterizes the amorphous materials. (a) SLLL models. (b) SL models.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Light curves of Chang’e 5-T1 R/B from before each of two sequential close Earth flybys taken from the same observatory. The light curves have been period wrapped by fitting a four-parameter Fourier series to the data via least squares minimization. As can be seen by the fitted period in each plot, the observed rotation rate of Chang’e 5-T1 changed substantially between the two flybys.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Normalized reflectance spectra from RAPTORS I showing a comparison between a Falcon 9 R/B (squares), a Long March 3C R/B (triangles), and the lunar impactor (dots). A third-order polynomial fit to the WE0913A data is provided as a reference. It is clear from the figure that the lunar impactor is a much closer spectral match to the Long March 3C R/B than the Falcon 9 R/B.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Zoomed-in view of the WE0913A calculated perigee (red dot) with the context of the coast and final burn stages of launch (large blue dots). The Chang’e 5-T1 R/B translunar trajectory should have a perigee between these two points, and we see that this is the case. The time window between the two launch phases is T + 22.053 minutes and T + 24.915 minutes and our calculated perigee is at T + 24.572 minutes. The Xichang Satellite Launch Center is again shown as a red star.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Example of the WE0913A orbit (black curve) from 2015 March 15 propagated backward until it hits its perigee on 2014 October 23. Orbits are shown in the geocentric MEME J2000 equatorial reference frame. The Moon’s orbit (gray curve) and Earth’s location (black dot) are included for reference. The rocket body had close encounters with the moon on both 2015 February 13 and 2014 October 28.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Ground track of WE0913A (red curve) showing the orbit propagated backward to perigee (red dot) on 2014 October 23 at 18:24:34.3 UTC (24 minutes after Chang’e 5-T1 launch). Only a short time near perigee is shown for simplicity. The Xichang Satellite Launch Center, from which the Chang’e 5-T1 mission was launched, is shown as a red star.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Example of the Chang’e 5-T1 R/B orbit (black curve) showing close approaches to the Earth between 2022 January until 2022 March, when it collided with the Moon, shown in the geocentric MEME J2000 equatorial reference frame. The Moon’s orbit (gray curve) and Earth’s location (black dot) are included for reference.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: These are approximately 500 m sections of the lunar terrain captured by LRO showing the Chang’e 5-T1 R/B impact site and double crater that was formed. Before is from LRO image M1400727806L and after is from M1407760984R (NASA/GSFC/Arizona State University). Other visual differences in the terrain are caused primarily by the difference in the angle of solar incidence, which was approximately 28° during the before image and 59° in the after image. This section of terrain is near the Hertzsprung crater on the lunar far side.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Illustration of the reference basis and relevant observation vectors on a shape model body facet.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: The 97.5% HPD region (light gray) in light curve phase space as estimated by 1500 random samples from the posterior estimates generated with data taken from the Leo-20 telescope on 2022 January 20. The observed light curve of the Chang’e 5-T1 R/B has been overlaid in black. The diagonal portion of the light curve from approximately 17–21 minutes post-epoch is a period with no data.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Zoomed-in view of the double crater formed by the Chang’e 5-T1 R/B impact with the Moon. Context images in Figures 13(a) and (b). Data from LRO image M1407760984R (NASA/GSFC/Arizona State University).
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Images of craters formed by the intentional impacts of the Apollo Saturn IV stages with the lunar surface. Note the round or elongated shapes, but all being explicitly one crater. (NASA/GSFC/Arizona State University).
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Impact prediction for several trajectory solutions as described in the text. The final delivered prediction was for solution “S23.”
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Time history of parameter sampling from the Bayesian inversion where the first 55,000 samples have been removed to avoid burn-in.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Final estimates of the posterior distributions of each parameter.
Paper: Physical Characterization of Moon Impactor WE0913A
Authors: Tanner Campbell, Adam Battle, Bill Gray, Steven R. Chesley, Davide Farnocchia, Neil Pearson, Grace Halferty, Vishnu Reddy, Roberto Furfaro
Figure caption: Brief overview of the MH algorithm for MCMC sampling.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: Median-averaged slice through the MIRI MRS IFU showing Didymos. It should be noted that Dimorphos was being occulted by Didymos during the entire period of MIRI observations. The measured median PSF FWHM is 0.″332 in sub-band 2B, consistent with the predicted FWHM of 0.″294. The measured FWHM across other sub-bands were found to be 0.9–1.2 times the predicted FWHM, broadly consistent with expectations for a point source. The yellow box marks the 7 × 7 pixel aperture used in our MIRI spectral extraction; the red box denotes the inner edge of the region used for background estimation.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: Ratio of the extracted MIRI MRS spectrum of the A-type standard star HD 163466 from a fixed 7 × 7 pixel square aperture to the CALSPEC spectrum. The individual sub-bands are labeled, and the black curves show low-order polynomial fits to the ratio curves, which were used as a benchmark for correcting Didymos’ extracted spectrum for flux losses outside of the aperture.
Paper: Near to Mid-infrared Spectroscopy of (65803) Didymos as Observed by JWST: Characterization Observations Supporting the Double Asteroid Redirection Test
Authors: Andrew S. Rivkin, Cristina A. Thomas, Ian Wong, Benjamin Rozitis, Julia de León, Bryan Holler, Stefanie N. Milam, Ellen S. Howell, Heidi B. Hammel, Anicia Arredondo, John R. Brucato, Elena M. Epifani, Simone Ieva, Fiorangela La Forgia, Michael P. Lucas, Alice Lucchetti, Maurizio Pajola, Giovanni Poggiali, Jessica N. Sunshine, Josep M. Trigo-Rodríguez
Figure caption: Maps of the surface coverage of Didymos from the NIRSpec and MIRI-Medium observations. Dotted lines separate the hemisphere visible from JWST from the side not visible from JWST, and the solid line separates the lit hemisphere from the unlit hemisphere. Shaded regions show areas that were lit and in the line of sight from JWST. It should be noted that these maps and the values in Table 1 do not take Didymos’ shape into account, though Didymos is spheroidal and shape effects are small. The coordinate system used in this figure is defined by IAU standards (Archinal et al. 2018), with the prime meridian set to be the the zero longitude on 2000 January 1 at 12:00 UT.
Paper: Detectability of the Yarkovsky Effect in the Main Belt
Authors: Denise Hung, David J. Tholen, Davide Farnocchia, Federica Spoto
Figure caption: Equation (7) is represented here as a three-dimensional plot, with the A 2 uncertainty as a function of the semimajor axis a and observational arc length L. Overplotted are contour lines for the minimum arc length for the Yarkovsky effect to become detectable as a function of a for MBAs of 0.1, 0.5, 1, and 5 km in diameter, where their A 2 values are estimated from the diameter scaling relation described in Figure 5.
Paper: Spectroscopic Links among Giant Planet Irregular Satellites and Trojans
Authors: Benjamin N. L. Sharkey, Vishnu Reddy, Olga Kuhn, Juan A. Sanchez, William F. Bottke
Figure caption: Top: spectrum of Uranian satellite Sycorax with a linear continuum fit as shown. A shallow dip is noted relative to this continuum from ∼0.65 to 0.75 μm. This feature is not dominated by a single wavelength bin (which can be indicative of a noise spike or incomplete sky subtraction) and persists far from the edge of the effective wavelength range of the red instrument. Further assessment of this spectral region would be aided by higher-S/N observations to constrain the continuum. Bottom: continuum-removed reflectance spectrum for Uranian satellite Sycorax. Here, values of unity indicate perfect agreement with extrapolation from the linear continuum. Variations below the continuum are small but statistically significant, consistent with the presence of an absorption feature. The depth of this feature is highly dependent on the choice of anchor points used in drawing the continuum, particularly along the short-wavelength edge. Depths vary from 3.0% ± 0.9% (using the continuum shown here) to 1.6% ± 0.9% if all points between 0.55 and 0.65 μm are included as anchors.
Paper: Spectroscopic Links among Giant Planet Irregular Satellites and Trojans
Authors: Benjamin N. L. Sharkey, Vishnu Reddy, Olga Kuhn, Juan A. Sanchez, William F. Bottke
Figure caption: Composite of collected spectra (channels: MODS1 red and MODS2 blue) of Uranian irregular satellites (Sycorax, Caliban) and Neptune Trojans (remaining panels) shown with comparison to photometric colors measured in the literature. Observations of 2010 TT191 and 2010 TS191 were not fully executed due to time constraints and did not produce recoverable traces in the blue channel. Except for the case of 2006 RJ103, the relative fluxes from the red and blue instruments are in good agreement, and no arbitrary scaling is required.(The data used to create this figure are available.)
Paper: Spectroscopic Links among Giant Planet Irregular Satellites and Trojans
Authors: Benjamin N. L. Sharkey, Vishnu Reddy, Olga Kuhn, Juan A. Sanchez, William F. Bottke
Figure caption: Top: spectra of Jovian irregular satellites Ananke and Lysithea. Bottom: comparison to the Jovian Trojan and Lucy spacecraft mission target (617) Patroclus collected in Sharkey et al. (2019). Lysithea is in the prograde Himalia family, while Ananke and its associated family is in a retrograde configuration. Both objects compare closely to the linearly red-sloped P-type spectrum of Patroclus. The gray bars represent wavelength regions with significant telluric absorption features that cause increased scatter and sometimes introduce spectral artifacts in observations of faint objects.(The data used to create this figure are available.)
Paper: Spectroscopic Links among Giant Planet Irregular Satellites and Trojans
Authors: Benjamin N. L. Sharkey, Vishnu Reddy, Olga Kuhn, Juan A. Sanchez, William F. Bottke
Figure caption: Top: comparison of Jovian irregular satellites Sinope and Pasiphae, which are both members of the retrograde Pasiphae family. Bottom: Sinope and Pasiphae present spectral differences that compare very similarly to the differences between Jovian Trojans (3548) Eurybates and (11351) Leucus collected in Sharkey et al. (2019), which will be studied in detail by the Lucy spacecraft mission. The gray bars represent wavelength regions with significant telluric absorption features that cause increased scatter and sometimes introduce spectral artifacts into observations of faint objects.(The data used to create this figure are available.)
Paper: Spectroscopic Links among Giant Planet Irregular Satellites and Trojans
Authors: Benjamin N. L. Sharkey, Vishnu Reddy, Olga Kuhn, Juan A. Sanchez, William F. Bottke
Figure caption: Jovian moon spectra from this work plotted with photometric BVR colors from the literature, normalized to unity at the central wavelength of the R filter. We note strong agreement between the red and blue channels on both MODS instruments for Themisto. Leda was observed with the MODS1 red and MODS2 blue channels.(The data used to create this figure are available.)