Icarus
ISSN: 0019--1035
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Datasets associated with articles published in Icarus
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Database of classified craters including center point latitude and longitude, diameter (km), and degradation class. Craterstats output files used to generate Figure 6.
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Ion mobility mass spectrometry data of tholins
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This file contains supplementary figures as well as a description of datasets and code developed for this project. Section 1 is full elevation, slope, orientation, and thermal inertia histograms for all studied sites. Section 2 is a description of data and Matlab code.
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Six crust velocity models based on geological observations
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These data include the mapped extent of the channelized lava flows and regional fissure network in the Cerberus region, Mars. The locations of crater counts, and the associated crater populations are also included.
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These are the ArcMap files created and reported on in Noviello et al. (submitted here)
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Supplementary materials for Karman et al "Update of the HITRAN collision-induced absorption section" Icarus (2018) 1. This readme file 1. The tar file containing the Main and Aletrnate folders. Only data that is updated or new with respect to original Richard et al (2012) are provided. The most current data of the CIA section in HITRAN can be found at https://hitran.org/cia/ 2. The reference mapping file to be used with the data files. Note that the reference numbering is different from that in the article.
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This file Figures.zip contains the scripts and data used to generate all figures in the manuscript. The file Movies.zip contains animations of the simulations presented in the manuscript. Description of movie files Movie S01 (proximal) is the output of the simulation in which only the degradation arising from the slope-dependent mass redistribution of proximal ejecta of the primary production function is modeled. Movie S1 corresponds to Figure 9 of the main text. Movies S02-S03 (micrometeoroid) are the output of the simulations in which an enhanced micrometeoroid population is added to the production function. Two cases are shown, one in which the resolvable crater production SFD has a slope of η=3.2 (S2) and one in which we modeled a slightly shallower production SFD slope of η=3.0. Movie S2 corresponds to Figure 11 of the main text. Movies S04-S10 (uniform) are the output of the simulations in which with additional extra diffusion added over a uniform region with radius f_e r, with K_(d,1) determined by solving equation (32) of the main text for the equilibrium SFD (n_(eq,1)=0.0084 and β=2) given a value of f_e. Here we have varied f_e from 3 to 50. Movie S4 (f_e=3) corresponds to Figure 14 of the main text, and Movie S8 (f_e=10) corresponds to Figure 15 of the main text.   Movies S11-S12 (ray) are the output of simulations in which additional extra diffusion is added over a spatially heterogeneous region mimicking crater rays. Two ray models are tested (see Figure 16 of the main text for the degradation scale “intensity function” for these two models). Both models use values of K_(d,1) needed to match the observed equilibrium SFD. Movie S12 corresponds to Figure 18 of the main text. Movies S13-S17 (etatest) are the output of simulations testing whether the analytical model given by equation (30) of the main text correctly predicts the dependence on the equilibrium SFD when the production function slope, η, is varied. In these simulations, η is varied between 2.6-3.8. We fix the value of K_(d,1), f_e=3, and ψ=2 for the solution to the observed equilibrium SFD for η=3.2, (see Movie S4). Movies S18-S21 (psitest) are the output of simulations testing whether the analytical model given by equation (30) of the main text correctly predicts the dependence on the equilibrium SFD when the degradation function slope, ψ, is varied. In these simulations, ψ is varied between 1.8-2.4. We fix the value of K_(d,1), f_e=3, and η=3.2 for the solution to the observed equilibrium SFD for ψ=2.0, (see Movie S4).
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MATLAB software used to perform plate tectonics force balance for ocean world ice shells.
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Zipped file geodatabase and "readme" plain text file. The geodatabase includes mapping of recurring slope lineae (RSL) for 10 different HiRISE images, mapping of dust devil tracks and rockfall markings in HiRISE images across four Mars years, and some manual traces of notable RSL growth. All 3D information is derived from a smoothed digital terrain model (except where explicitly noted otherwise, that is, for certain long profiles only), which in turn is derived from stereo HiRISE imagery. See published paper for additional details.
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