adsabs/AstroCLIMB huggingface dataset:
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: The importance of the spectral parameters simulating different available and proposed Mars multispectral camera filters. IMP: Imager for Mars Pathfinder; PAN: Mars Exploration Rover Panoramic Camera (Pancam); MAS: Mars Science Laboratory Curiosity rover Mastcam; MAZ: Mars 2020 Perseverance rover Mastcam-Z; EXO: ExoMars Panoramic Camera; MSC: Multispectral Camera on the Mars Tianwen-1 rover; RED: MicaSense RedEdge-M camera; NEW: proposed wavelength filters. The number after the camera name represents the wavelength. The slope and the band depth are indicated by S and B after the wavelength, respectively.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: Comparison of the different reflectance transformation methods. Radiance-to-reflectance conversion using (a) the one-point ELM, (b) the two-point ELM, (c) the DLS method alone, and (d) a combination of the DLS method and ELM. The X-axis shows the selected images for the calculation. Moinik Formation clays and tuff (MFC); Humbu Formation at Pinini (HFP); and Humbu Formation at Mtowabaga (HFM). Numbers after the three letters indicate the image number.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: MicaSense RedEdge-M camera mounted on a drone (a) and black-and-white reference (b) with their spectra in the field (c). Black points in the plot represent the wavelength positions of the MicaSense RedEdge-M camera filters.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: Image preprocessing steps showing the raw images, vignette factors, raw gradient factors, and resultant radiance images of MicaSense RedEdge-M band 1 and 4 of a selected image.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final, binned SpeX spectra. Note that the portion of each spectrum below 2.7 μm is omitted for clarity. Example SpeX prism spectra for each object are shown in Figure 2. Each panel shows all data for a different apparition of each object. Apparition 1 for both FG3 and QE2 has been further separated for clarity. We note that on 2022 April 28 for FG3 set C was the only viable data set of the evening, due to weather, and that data were not available at wavelengths longer than 4.2 μm. Furthermore, we note that 2015 July 21 for JD6 Apparition 2 was provided to us by V. Reddy (personal communication) and has LXD short (1.67–4.2 μm) data only. The y-axis is normalized flux, normalized to 1.0 at ∼1.6 μm. The x-axis is wavelength in microns. Note that different panels have different axis scales.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Left: example χ 2 fit map for model fits to a single data set (2008 October 1 A) for UO1. Every colored (i.e., nonblack) square represents a different model that can be said to fit the data, with good fitting to poor fitting corresponding to purple to red. Right: example final fit map. Here we show the first SpeX apparition of UO1 with all seven total data sets in 2008 (see Table 1). Every colored square represents a different model, with the color indicating the number of data sets from that apparition that can be fit by the given model. Thus, purple squares represent models that fit more data sets, thus indicating a higher likelihood that the given parameters can describe the object’s overall properties, not just properties associated with a particular viewing geometry. In both plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo. Here thermal inertia was sampled between 0 and 800 TIU in steps of 100 TIU and the visible albedo was sampled between 0 and 0.5 in steps of 0.05.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Final, averaged NEOWISE data sets. Each panel shows different data sets from different mission phases. WA denotes WISE data, PC denotes post-cryo data, and NW denotes NEOWISE data (Section 2.2). Some panels are further separated for clarity. Letters within each panel denote different data sets. Missing letters indicate sets that were rejected after looking at the raw NEOWISE images (Section 2.2). The y-axis is absolute flux density. The x-axis is wavelength in microns. Note that different panels have different axis scales.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: The consistency of NEOWISE model fits relative to fits based on the SpeX data as a function of various orbital parameters. Each point is a different NEOWISE data set. “Consistent” means that models based on the given data set are consistent with results based on SpeX data. “Inconsistent” means that a model was fit to the data set, but the model was inconsistent with the results based on the SpeX data. “No Fit” means that no models could be fit to the data set. The top three panels show the fit consistency as a function of the solar phase angle (units of degrees), Sun–object distance (units of au), and theoretical blackbody temperature of the object at the time of observation (units of K), respectively. The bottom panels show how these quantities are related to each other. Here the fit consistency is given by the color. The bottom left panel shows solar phase angle and Sun–object distance; the bottom right panel shows theoretical blackbody temperature and Sun–object distance.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Examples of how all data sets for a given object do not necessarily overlap. Here we show NEOWISE data for SD220. The bottom left panel shows the overlap of all NEOWISE data sets for SD220. The other panels show individual data sets, where colored squares indicate models that fit the data. The three omitted data sets (B, C, E) have no models that produce spectra consistent with the data. Furthermore, we note that not all data sets are consistent with each other. Thus, there are only six data sets with fitting models, and the maximum number of overlapping data sets (four) is less than the total number of data sets (nine). This can be seen in the bottom left panel. In other words, out of all nine data sets, the model with the most overlap only fits four data sets. In all plots the x-axis is the thermal inertia in TIU and the y-axis is visible albedo. We note that for SD220 we only examine a thermal inertia of 0 TIU, due its extremely slow rotation (Section 4.4); however, for all other objects a range of thermal inertias are investigated.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Various NEATM-like model fits to a sample SpeX data set for QE2. The different colored lines show different models. Here the y-axis is normalized flux, normalized to 1.0 at ∼1.6 μm. The x-axis is wavelength in microns. As the model parameters change monotonically, the models move monotonically across the data set. This property of the model allows us to easily identify a range of model parameters that can be said to fit the data. Top: the beaming parameter is held at 0.86, and the visible albedo and thermal inertia are allowed to vary. Bottom: the albedo is held at 0.06, thermal inertia is held at 100 TIU, and the beaming parameter is allowed to vary.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Example of the acceptable fit range of our NEATM-like model to the data. Any models that fall within the 1σ uncertainties of the data are accepted as fitting the data. Left: a single SpeX data set for UO1. The y-axis is normalized flux, normalized to 1.0 at ∼1.6 μm. The x-axis is wavelength in microns. Right: a single NEOWISE data set for JD6. The y-axis is absolute flux density. The x-axis is wavelength in microns.
Paper: Inconsistencies in Simple Thermal Model Results for Near-Earth Asteroids between Infrared Telescope Facility SpeX and NEOWISE Data
Authors: Samuel A. Myers, Ellen S. Howell, Christopher Magri, Ronald J. Vervack, Yanga R. Fernández, Mary L. Hinkle, Sean E. Marshall
Figure caption: Example SpeX prism spectrum for each object. The y-axis is normalized flux. The x-axis is wavelength in microns. Data were taken on 2008 May 13 (JM8), 2010 July 29 (JD6), 2010 October 3 (UO1), 2018 December 7 (SD220), 2011 November 28 (FG3), and 2013 June 8 (QE2).
Paper: On the Early Thermal Processing of Planetesimals during and after the Giant Planet Instability
Authors: Anastasios Gkotsinas, David Nesvorný, Aurélie Guilbert-Lepoutre, Sean N. Raymond, Nathan Kaib
Figure caption: Cumulative distribution of the CO ice interface depths on planetesimals implanted at distances below the Oort spike (a < 10,000 au) and considered to be DO (orange dotted line) and planetesimals implanted beyond the Oort spike, considered to be DN (blue dashed line).
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: Natural color composite (a) and K-means clustering of the image data (b). The spectra of 12 classes mapped with the most distinguished spectra of selected materials over the imaged area (c). Different beds marked in Figure 9(a) are tuff (1), chert (2), carbonate (3), and green clay beds (4).
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: (a) Mosaic natural color composite image of the selected area of the Moinik Hills. (b) Weighted K-means classification image derived from the combination of reflectance images and DEM. (c) Weighted K-means classification image derived from the index images. (d) Weighted K-means classification images derived from the combination of index images and digital elevation provides the optimal result.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: Fuzzy C-means clustering results of the selected single image area. Natural color composite image (a), four selected fuzzy membership value images ((b)–(e)), classified false-color composite image using three selected fuzzy membership images (f). Lithologies covered in Figure 11(a) are Hajaro basalt (1), Sambu lavas (2), and soils (3). The x- and y-axes show the pixel number in the image.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: Field photograph of the imaged area (a), natural color composite image (b), and K-means clustering results of the image data (c). Shadows on the original image are not affected by the classified image due to the use of band index images for the classification.
Paper: Mapping Paleolacustrine Deposits with a UAV-borne Multispectral Camera: Implications for Future Drone Mapping on Mars
Authors: Gayantha R. Kodikara, Lindsay J. McHenry, Brian M. Hynek, Jackson K. Njau
Figure caption: Density plot showing the elevation distribution of 20 classes mapped over the selected study area.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Comparison of the scaled spectral reflectances of JIX Sinope (2006, blue dots; 2009, tan dots) and JXI Carme (red dots) with the ECAS mean values (large filled red triangles), highest values (green circles), and lowest values (tan squares) for D-class asteroids (Tholen 1984). The scaled reflectance values of Sinope and Carme compare directly with the scaled photometry of 26 D-class asteroids included in the mean value and fall within the extreme end-member values from the ECAS D-class asteroids.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Mixing modeling fits to two members of the retrograde (i = 149°) cluster: JVII Pasiphae, JXII Ananke (in 2006), and JXII Ananke (in 2010). Satellite spectra are plotted in blue. Model fits are plotted in red.
Paper: Clues to the Origin of Jovian Outer Irregular Satellites from Reflectance Spectra
Authors: Faith Vilas, Amanda R. Hendrix
Figure caption: Mixing modeling fits to JXI Carme of the retrograde (i = 165°) cluster and individual satellite JIX Sinope (in 2006) and JIX Sinope (in 2009). Satellite spectra are plotted in blue. Model fits are plotted in red.
Paper: Solar Energetic Particle Track Accumulation in Edgeworth–Kuiper Belt Dust Grains
Authors: M. Lin, A. R. Poppe
Figure caption: The fraction of modeled IDP grains that migrated from their birthplace in the EKB to 1 au as a function of grain radius for each separate EKB subpopulation.
Paper: Solar Energetic Particle Track Accumulation in Edgeworth–Kuiper Belt Dust Grains
Authors: M. Lin, A. R. Poppe
Figure caption: A comparison of the effects of varying the α decay constant on the tracks accumulated for 7 μm size dust grains in the resonant class. The blue vertical dashed line shows the average of the track accumulation distribution, while the orange dashed line shows the expected mean track density from L. P. Keller & G. J. Flynn (2022).
Paper: Solar Energetic Particle Track Accumulation in Edgeworth–Kuiper Belt Dust Grains
Authors: M. Lin, A. R. Poppe
Figure caption: The distributions of dynamically calculated track densities at 1 au for 2, 10, and 30 μm IDPs. Colors denote the contribution from each EKB subpopulation. Note that the distribution of the dust grains is weighted by the relative contribution of each subpopulation (see A. R. Poppe 2016).
Paper: Solar Energetic Particle Track Accumulation in Edgeworth–Kuiper Belt Dust Grains
Authors: M. Lin, A. R. Poppe
Figure caption: A comparison of the dynamically and analytically calculated track densities in grains reaching 1 au for 2, 5, and 10 μm IDPs. The vertical dashed lines denote the mean track densities for each distribution.
Paper: Solar Energetic Particle Track Accumulation in Edgeworth–Kuiper Belt Dust Grains
Authors: M. Lin, A. R. Poppe
Figure caption: A comparison of the average number of tracks accumulated per au for 5 μm grains for (blue) dynamical integration and (red) analytical integration.
Paper: Solar Energetic Particle Track Accumulation in Edgeworth–Kuiper Belt Dust Grains
Authors: M. Lin, A. R. Poppe
Figure caption: The semimajor axis, eccentricity, track accumulation rate, and total accumulated tracks for a typical 20 μm EKB classical grain that successfully drifted from the EKB to 1 au.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. I. The Accuracy and Errors of Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: One can compare actual images to rendered images based upon the same observation geometries to identify and characterize how well SPC constructs boulders. This composite image is constructed by assigning the red channel to the truth image and the cyan channel to a synthetic image generated by the DTM. The terrain that matches is gray, while errors stand out as red or cyan. Here, the missing boulders are noticeable by the red on the asteroid’s limb.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. I. The Accuracy and Errors of Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: Results of the tests for 0° (left) and −70° (right) latitude. One can see in the −70° latitude image that the terrain is much smoother than in the 0° latitude image. These renderings use only topography and lack albedo. The point of view was rotated to make clear the loss of details in the DTM.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. I. The Accuracy and Errors of Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: Vertical profiles of the truth (green) and SPC-generated (purple) DTMs. In the SPC model, the height of the boulder is only about half of the truth height. The example DTM has a GSD of 5 cm pixel–1.
Paper: Sensitivity Testing of Stereophotoclinometry for the OSIRIS-REx Mission. I. The Accuracy and Errors of Digital Terrain Modeling
Authors: Eric E. Palmer, John R. Weirich, Robert W. Gaskell, Diane Lambert, Tanner Campbell, Kris Drozd, Olivier S. Barnouin, Michael G. Daly, Kenneth Getzandanner, John N. Kidd, Coralie D. Adam, Dante S. Lauretta
Figure caption: DTMs that included very high-resolution images and maplets.
Paper: Pre-impact Albedo Map and Photometric Properties of the (65803) Didymos Asteroid Binary System from DART and Ground-based Data
Authors: B. J. Buratti, J. Pittichová, I. Mishra, J. K. Hillier, J. A. Mosher, S. R. Chesley, J. M. Sunshine, O. Barnouin, C. M. Ernst, R. T. Daly, J-Y Li, A. F. Cheng, A. S. Rivkin, J. Rizos
Figure caption: The four panels represent (a) the radiometrically corrected image of the DART target, (b) the same image with a geographical grid of latitude and longitude, and (c, d) the backplanes of geometric information: the emission and incidence angles (panels (c) and (d), respectively) computed with the DART Project’s shape model version 003 (Daly et al. 2023; Barnouin et al. 2024). The image was obtained 8.559 s before closest approach with a spatial resolution of 26 cm pixel−1.
Paper: Pre-impact Albedo Map and Photometric Properties of the (65803) Didymos Asteroid Binary System from DART and Ground-based Data
Authors: B. J. Buratti, J. Pittichová, I. Mishra, J. K. Hillier, J. A. Mosher, S. R. Chesley, J. M. Sunshine, O. Barnouin, C. M. Ernst, R. T. Daly, J-Y Li, A. F. Cheng, A. S. Rivkin, J. Rizos
Figure caption: The reduced data for the TMO (blue squares). For comparison, aggregate curves for C-type and S-type asteroids are shown. The latter phase curves are from Helfenstein & Veverka (1989) and Li et al. (2015). The line is a linear least fit of 0.033 mag deg−1.
Paper: Pre-impact Albedo Map and Photometric Properties of the (65803) Didymos Asteroid Binary System from DART and Ground-based Data
Authors: B. J. Buratti, J. Pittichová, I. Mishra, J. K. Hillier, J. A. Mosher, S. R. Chesley, J. M. Sunshine, O. Barnouin, C. M. Ernst, R. T. Daly, J-Y Li, A. F. Cheng, A. S. Rivkin, J. Rizos
Figure caption: (a) The position of the scan we used for modeling macroscopic roughness based on the crater model of Buratti & Veverka (1983). (b, c) Hand-adjusted fit that looks best and a formal fit to the depth-to-radius ratio, respectively. Panel (d) shows that much better fits can be obtained if the roughness changes with position. The upper 25%–30% of Dimorphos toward the limb is substantially rougher, as shown by the green model. The q-values of 0.25, 0.16, 0.19, and 0.79 correspond to Hapke mean slope angles (Hapke 1984) of about 18°, 12°, 14°, and 53°, respectively.
Paper: Pre-impact Albedo Map and Photometric Properties of the (65803) Didymos Asteroid Binary System from DART and Ground-based Data
Authors: B. J. Buratti, J. Pittichová, I. Mishra, J. K. Hillier, J. A. Mosher, S. R. Chesley, J. M. Sunshine, O. Barnouin, C. M. Ernst, R. T. Daly, J-Y Li, A. F. Cheng, A. S. Rivkin, J. Rizos
Figure caption: Image obtained at Palomar Observatory on the 200-inch telescope on 2022 September 30 (3.5 days after the impact) in the Sloan r filter.
Paper: Pre-impact Albedo Map and Photometric Properties of the (65803) Didymos Asteroid Binary System from DART and Ground-based Data
Authors: B. J. Buratti, J. Pittichová, I. Mishra, J. K. Hillier, J. A. Mosher, S. R. Chesley, J. M. Sunshine, O. Barnouin, C. M. Ernst, R. T. Daly, J-Y Li, A. F. Cheng, A. S. Rivkin, J. Rizos
Figure caption: Planned and actual phase angle coverage at TMO during the 2022 October–2023 February campaign. The planned and actual phase angles and times do not exactly line up because of updates to the ephemeris.
Paper: Pre-impact Albedo Map and Photometric Properties of the (65803) Didymos Asteroid Binary System from DART and Ground-based Data
Authors: B. J. Buratti, J. Pittichová, I. Mishra, J. K. Hillier, J. A. Mosher, S. R. Chesley, J. M. Sunshine, O. Barnouin, C. M. Ernst, R. T. Daly, J-Y Li, A. F. Cheng, A. S. Rivkin, J. Rizos
Figure caption: A typical image of the Didymos–Dimorphos system obtained at TMO on October 21 11:05:37 UT, 25 days after impact. Didymos–Dimorphos is the object with the tail.
Paper: Pre-impact Albedo Map and Photometric Properties of the (65803) Didymos Asteroid Binary System from DART and Ground-based Data
Authors: B. J. Buratti, J. Pittichová, I. Mishra, J. K. Hillier, J. A. Mosher, S. R. Chesley, J. M. Sunshine, O. Barnouin, C. M. Ernst, R. T. Daly, J-Y Li, A. F. Cheng, A. S. Rivkin, J. Rizos
Figure caption: The normal reflectance of Dimorphos computed from the calibrated DRACO image with a corresponding color scale bar. The blue halo surrounding Didymos is a small residual signal in the background of the PDS image.
Paper: Pre-impact Albedo Map and Photometric Properties of the (65803) Didymos Asteroid Binary System from DART and Ground-based Data
Authors: B. J. Buratti, J. Pittichová, I. Mishra, J. K. Hillier, J. A. Mosher, S. R. Chesley, J. M. Sunshine, O. Barnouin, C. M. Ernst, R. T. Daly, J-Y Li, A. F. Cheng, A. S. Rivkin, J. Rizos
Figure caption: The composite data set from TMO and Helfenstein & Veverka (1989) for data at opposition (less than 6.°7) shown with the best-fit photometric model.