adsabs/AstroCLIMB huggingface dataset:
Paper: Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles
Authors: Margaret E. Landis, Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, David A. Paige
Figure caption: (a) Region of the north polar nearside that includes Nansen A (∼82° N, 64° E) and De Sitter M (∼81° N, 67° E) craters, where water ice deposits can be seen between 80 and 85° N. (b) Small impact craters on the rim of Newton A provide locations for ≲107 K bolometric temperature measurements from Diviner.
Paper: Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles
Authors: Margaret E. Landis, Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, David A. Paige
Figure caption: Area in square kilometers of water ice thermal stability in 0.25° latitude bins for the north (red) and south (blue) poles of the Moon based on the Diviner data presented here. The total areas and net distribution of the surface water ice thermal stability are different between the poles.
Paper: Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles
Authors: Margaret E. Landis, Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, David A. Paige
Figure caption: Polar stereographic display of the volatile species of interest that have surface thermal stability regions at the south pole from 80° to 90° S (species and stability temperature given in the legend). Background data are the Lunar Orbiter Laser Altimeter (LOLA) 100 m pixel−1 shaded relief map. Each ring is 5° latitude. Black arrows on the CO2 map indicate the small thermal stability regions for CO2 at the south pole.
Paper: Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles
Authors: Margaret E. Landis, Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, David A. Paige
Figure caption: Polar stereographic display of the volatile species of interest that have surface thermal stability regions at the north pole from 60° to 90° N (species and stability temperature given in the legend). Background data are the Lunar Orbiter Laser Altimeter (LOLA) 100 m pixel−1 shaded relief map. Each ring is 5° latitude.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: CA08 flux density observations and model fits. The thick green curve shows the averaged relative flux density measurements from Figure 5. The thin black curve is the flux density S(δ) of a model with a Gaussian of maximum S 0 superposed onto a linear background S  L  according to the equations shown on the left side of the figure. The parameters determined by the fitting procedure are displayed in the upper right corner of the figure. The data are also compared with a simple emission model of the predicted flux density of the KBO (violet dashed curve), with the projected area and brightness temperature indicated in the lower right corner. The mean and standard deviation of the data in the calibration intervals are ΔS = 0.3 Jy and σ  s  = 6.9 Jy, and the peak KBO flux density from the Gaussian fit is S 0 = 62.7 Jy, yielding a detection S/N in this case of S 0/σ  s  ≈ 9. The quantities σ FIT and σ MODEL are the standard deviations of the data from the Gaussian fit and the emission model, respectively, considering only those measurement points outside the calibration intervals.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: Dieletric constant, loss tangent, and electrical skin depth as a function of porosity (p) for some proposed materials on Arrokoth (Table 3). Top: dielectric constant. The curves use formulae for various inclusion shapes as described by Liu et al. (2016). The linear decrease with p from Equation (10) is consistent with laboratory measurements. Middle: loss tangent. This quantity, essentially a measure of radio wave absorption, is assumed to decrease linearly to zero with p according to Equation (11). Bottom: electrical skin depth. Curves for δ el at λ = 4.2 cm (in m) are calculated from Equation (9) for the three tholin entries of Table 3. An increase to infinity occurs as p goes to 1 owing to the vanishing loss tangent. The skin depth for the “tholin powder” curve runs from 2 to 10 m for p from 0% to 80%. For compact tholin, the skin depth cannot fall lower than about 0.5 m even at zero porosity.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: Global sky model @ 7.18 GHz in the J2000 coordinate system. The contour map of brightness temperature has been convolved with a Gaussian beam of width equal to 1.2°, corresponding to the New Horizons HGA. The CMB temperature of 2.725 K has been subtracted, and the maximum temperature has been capped at 0.2 K (color scale at right in mK). The HGA positions for the CA03 (dayside) and CA08 (nightside) REX observations of the KBO Arrokoth are shown in white; REX observations at Pluto are shown for comparison in yellow. Close-ups of the regions important for the REX observations at Arrokoth are shown in Figure A2 (dayside stare) and Figure A3 (nightside scan), respectively.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: Predicted global brightness temperature of KBO Arrokoth during the REX CA08 scan as a function of thermal inertia and electrical skin depth. The four maps correspond to the four values of effective emissivity denoted in the upper left corner of each panel. Contours for T  b  = 29 ± 5 K, the range of brightness temperatures consistent with the REX observation, are drawn explicitly.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: Background sky for the CA08 nightside observation. The map shows a 20° × 20° patch of sky centered at (06 hr, 10°). The red circles show position and 1.2° diameter of the HGA beam for the start and end of the observation, which passed over the position of the KBO Arrokoth defined by the black arrow. The scan also came uncomfortably close to the Rosette Nebula, a strong radio source with an estimated flux density of 330 Jy at X band. The miss distance of 5°, however, was large enough that flux density confusion could be ruled out. The mean brightness temperature of the background over the scan was estimated to be 2.74 K.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: Background sky for the CA03 dayside observation. The map shows a 20° × 20° patch of sky centered at (18 hr, −25°). The red circles indicate the positions and 1.2° diameter of the HGA beam at the start and end of the observation. The KBO Arrokoth remained within the HGA beam throughout the observation. The mean background brightness temperature for this observation, about 50 mK greater than T CMB, was estimated from this map to be 2.78 K.
Paper: Detection of Radio Thermal Emission from the Kuiper Belt Object (486958) Arrokoth during the New Horizons Encounter
Authors: M. K. Bird, I. R. Linscott, G. L. Tyler, O. M. Umurhan, R. A. Beyer, W. M. Grundy, C. M. Lisse, D. P. Hinson, M. Pätzold, S. A. Stern, H. A. Weaver, C. B. Olkin, L. A. Young, J. R. Spencer, K. N. Singer, J. M. Moore, G. R. Gladstone, C. C. DeBoy, M. Vincent, S. B. Porter
Figure caption: Average nightside temperature of KBO Arrokoth as a function of thermal inertia and depth over all facet areas facing the spacecraft during the REX CA08 scan.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: Unenhanced (top row) and enhanced (bottom row) images of C/2021 A1 (Leonard) in various filters on 2021 November 29. All images are centered on the opto-center of the comet and have north up and east to the left. All images in the top row are 325,000 km across, while all images in the bottom row are 100,000 km across and have been enhanced by subtraction of an azimuthal median profile. Light is bright and dark is faint in all panels. The first and second panels in each row are the ﹩g^{\prime} ﹩ and ﹩r^{\prime} ﹩ images, respectively, and the third panel in each row is a synthetic “gas” image created by scaling an ﹩r^{\prime} ﹩ image (median of all images taken that night) by the estimated dust color and subtracting this scaled image from a median ﹩g^{\prime} ﹩ image. As discussed in the text, the morphology of this synthetic gas image closely matches that of the CN gas image (fourth column; acquired by B. Skiff using the Lowell Observatory 42-inch telescope) and is very different from the “dust” (﹩r^{\prime} ﹩-band) image. Two jets can be seen oriented near positional angles 40° and 220° in the enhanced gas images, while the tail is to the northwest in the dust images. A very faint residual dust tail is still seen near the northwest corner in the gas images.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: LOOK Project and TRAPPIST light curve of comet 7P/Pons–Winnecke, measured within 5″-radius apertures. This plot and the subsequent three show the time on the lower x-axis as a function of time from perihelion. The g P1-band photometry has been offset by the measured color of the inner coma, g P1 − r P1 = 0.50 ± 0.01 mag, to produce effective r P1-band data. TRAPPIST-South (TS) and TRAPPIST-North (TN) R  c -band photometry has been offset by the color of the Sun: R  c  − r P1 = −0.21 mag (Willmer 2018). An approximate secular trend line is plotted, based on an Af ρ model: ﹩A(0^\circ )f\rho =148\ {r}_{h}^{-0.4}﹩ cm. Arrows mark outbursts of the comet. An inset shows the light curve of the 2021 July 10 outburst in detail.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: LOOK Project and TRAPPIST light curve (indicated by “TN” for TRAPPIST-North and “TS” for TRAPPIST-South) of comet 156P/Russell-LINEAR, measured within a 5000 km radius aperture at the comet distance. LOOK g P1-band photometry has been offset by the measured color of the inner coma, g P1 − r P1 = 0.50 ± 0.01 mag, to produce effective r P1-band data. Also plotted (right panel) are the Af ρ and A(0°)f ρ values from LOOK. Both panels show time as a function of time from perihelion (T  p  = 2,455,9171.313576862 or 2020 November 17 19:31:33 TDB).
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: Light curve of comet 57P based on 5″-radius r P1-band photometry from the LOOK Project and TRAPPIST-South (TS) R  c -band photometry, which has been offset by the color of the Sun: R  c  − r P1 = −0.21 mag (Willmer 2018). Data from 2021 October 29, which was affected by a bright stellar contaminant, has been removed.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: Absolute magnitude of comet P/2020 X1 (ATLAS) based on ATLAS (o band; Tonry et al. 2018b), Pan-STARRS (PS1, i P1 and w P1 bands; Tonry et al. 2012), and ZTF (r P1 band; Bellm et al. 2019) data reported to the Minor Planet Center and 5″-radius r P1-band photometry from the LOOK Project. No attempt has been made to correct for different aperture sizes and bandpasses. However, the rapid decline in brightness, suggestive of an outburst, is clear.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: Total magnitudes for 156P from the Minor Planet Center database (orange squares) for the 2013–2015 apparition, along with the predicted total magnitude from JPL Horizons (black dashed line). The time of perihelion is indicated by the vertical dotted line, and the time when the solar elongation was <40° is shown by the blue shaded area.
Paper: The LCO Outbursting Objects Key Project: Overview and Year 1 Status
Authors: Tim Lister, Michael S. P. Kelley, Carrie E. Holt, Henry H. Hsieh, Michele T. Bannister, Aayushi A. Verma, Matthew M. Dobson, Matthew M. Knight, Youssef Moulane, Megan E. Schwamb, Dennis Bodewits, James Bauer, Joseph Chatelain, Estela Fernández-Valenzuela, Daniel Gardener, Geza Gyuk, Mark Hammergren, Ky Huynh, Emmanuel Jehin, Rosita Kokotanekova, Eva Lilly, Man-To Hui, Adam McKay, Cyrielle Opitom, Silvia Protopapa, Ryan Ridden-Harper, Charles Schambeau, Colin Snodgrass, Cai Stoddard-Jones, Helen Usher, Kacper Wierzchos, Padma A. Yanamandra-Fisher, Quanzhi Ye, 泉志 叶, Edward Gomez, Sarah Greenstreet
Figure caption: Evolution of 156P coma morphology before and after perihelion in ﹩r^{\prime} ﹩ images from LOOK. The orientation and scale are given at the bottom of the lower panels.
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: Psyche’s observed thermal inertia is significantly lower than meteorite samples and theoretical curves for low-porosity material. From this, we infer that Psyche’s surface likely has a very high porosity regolith. Psyche’s observed Γ is shown as shaded regions, meteorite measurements are diamonds, and theoretical curves are shown as lines. Model curves use base values of k 0 = 2.0 W m−1 K−1, k  r  = 10−3 W m−1 K−1, ρ  g  = 3800 kg m−3, and c  p  = 500 J kg−1. Changing these bulk values would shift the lines vertically by the square root of the change (Equation (2)) but not change the dependence on porosity. This is shown by the two curves for effective medium theory, which use different solid thermal conductivity values. Meteorite thermal inertia values shown are all determined at 200 K.
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: Comparison of numerically integrating the Paris law (Equation (14)) with a diurnal temperature variation history, constant temperature variation, and the constant temperature analytic solution (Equation (16)). The value for N crit is shown by the vertical dashed lines. When the numerical method is given a constant ΔT, it recovers the analytic solution for N crit to within within 0.1%. Integrating with the model diurnal ΔT results is a slightly smaller N crit than using the analytic scaling for the seasonal mean of the diurnal ΔT. This difference is expected, as the crack growth is a power law with ΔT.
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: A deep model domain is important for realistically modeling surface temperatures during polar night. We compare the model used in this work with the standard TPM configuration. This configuration uses a shallow model domain (eight diurnal skin depths), and the object is fixed in its orbit as it rotates. The top row are models with an obliquity of 20°, and the bottom row is for 85°. In each plot, the vertical red line is the subsolar latitude at the time of this snapshot. Regions shaded yellow are in polar day, and regions shaded gray are in polar night. For this example, no shape model is used (assumed perfect sphere).
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: The rms error in the upper five diurnal skin depths (panel (a)) and annual skin depth (panel (b)). In the near surface, the error between three and four diurnal skin depths is larger than that at four to five skin depths (so the latter is not visible). For reference, all results presented in the main text have been initialized for three orbits (∼15 yr).
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: As expected, the diurnal temperature variations are strongest in the equatorial region. Generally, diurnal temperature variations are a factor of 2–5 times weaker than annual temperature variations. (a) Diurnal temperature variations as a function of season and latitude. (b) Maximum, minimum, and mean diurnal temperature variation as a function of latitude.
Paper: The Geologic Impact of 16 Psyche’s Surface Temperatures
Authors: Carver J. Bierson, Linda T. Elkins-Tanton, Joseph G. O'Rourke
Figure caption: Error in the surface flux for the sin test. Results are shown that include both the annual and diurnal periods and those that only include the annual period (similar to the real polar forcing).
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The opposition surge data from VIMS analyzed used in this paper. The data for Mimas, Tethys, and Dione include trailing-side observations, while the data for Rhea include leading-side observations. Data for Enceladus include both hemispheres. These measurements, as well as additional ones at larger solar phase angles (see Figures 8 and 9), are included in a supplementary materials package, along with the relevant pointing information.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The empirical phase curve parameters determined from Equation (1). The leading and trailing only refers to the opposition surge that was used to correct the data. B is β, the phase coefficient (left five panels); C is the half-width at half-max (the middle five panels); and A is the amplitude of the opposition surge (the right five panels).
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The spectra of the main moons of Saturn obtained at the smallest solar phase angles from Figure 1, and normalized to the geometric albedo. The red dots represent the wavelengths of values computed in Table 2. All the spectra were obtained at a solar phase angle of 2°, or in the case of Tethys, 1.7°.
Paper: Observations and Modeling of the Opposition Surges of the Icy Moons of Saturn Based on Cassini Visual Infrared Mapping Spectrometer Data
Authors: B. J. Buratti, J. H. Hillier, P. A. Dalba, M. D. Hicks, J. A. Mosher, A. R. Hendrix, L. Abramson, N. Akhter
Figure caption: The infrared albedos of the moons plotted as a function of distance from Saturn, along with the earlier results in the visible (Verbiscer et al. 2007).