Icarus

We provide three separate .csv files that contain the supplementary material requested by Reviewer 1. An explanation of the contents of each file is given in the file description.

The file MIRO_Columns.txt contains the column densities and their uncertainties corresponding to the results published previously in the paper by Marshall, D.W., Hartogh, P. Rezac, L. von Allmen, P., Biver, N., Bockelée-Morvan, D., Crovisier, J., Encrenaz, P. Bulkis, S. Hofstadter, M. Ip, W.-H., Jarchow, C. Lee, S., Lellouch, E. 2017. Spatially resolved evolution of the local H2O production rates of coet 67P/Churyumov,Gerasimenko, from the MIRO instrument of Rosetta. Astronomy & Astrophysics 603, A87. The format containes space delimited columns corresponding to Date, UT time, Heliocentric Distance (AU), column density (cm^-2), column density error (cm^-2).

see readme.docx

Surface deposition profiles for the Enceladus plume.

Labeled figures derived from original HiRISE images, as described in the text

All CRISM spectra from plots are stored in an Excel worksheet. Includes ratio spectra as shown in figures as well as original reflectance spectra and alternative ratio spectra. Mosaics of Jezero CRISM RGB combinations over CTX basemaps are included at various zooms and resolutions, as used in figures.

XRD data for the spectra seen in Figure 1a-c

HITRAN2016 line file with hydrogen as the broadening gas. The line file uses the new temperature dependence of the half-width and line shift by Gamache and Vispoel. Please see the read_me.txt file for details.

The formation of impact craters in unconsolidated granular materials is a topic of enduring interest in solid-earth geophysics, planetary science, and several branches of engineering science. In particular, a general relationship between crater size, impact parameters, and target material properties is often sought. This paper presents a new empirical relationship, based on dimensional analysis and inspired by gas-dynamic shock physics, for the diameters of low- and high-speed impact craters in dry granular materials based on the hypothesis that surface-gravity- and shock-wave phenomena primarily set crater size. The final relationship involves the impacting object’s kinetic energy and speed; the target material’s density, angle of repose, and sound speed; and the gravitational acceleration at the impact location. It is formulated in terms of a dimensionless crater diameter, an algebraic combination of Froude number, Mach number, and the tangent of the target material’s angle of repose, using an analogy to gas dynamics and an empirical power law for the dependence of granular-material sound speed on gravitational acceleration. The coefficient of determination for the final fit is 0.969 based on experimental impact data from 325 individual impacts spanning parametric ranges of more than 400 in crater diameter, 10^10 in impact energy, 500 in gravitational acceleration, and 40 in target material density for two different angles of repose. The final formula provides insight into how impact energy conversion depends on Mach number and may be useful for predictive and forensic analysis of planetary impact craters and for granular-flow code validation.

These files list the neutral and ion reactions used for the calculations. They have the form: X: R1 + R2 -> P1 + P2 rate (as a Fortran statement) ; source where X = P, C or 0,I,F for photodissociation, chemical reaction or 3-body reaction