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# Supplementary material for "Mars: Abundant Recurring Slope Lineae (RSL) Following the Planet-Encircling Dust Event (PEDE) of 2018"

Preferred citation (DataCite format):

  McEwen, Alfred; Schaefer, Ethan; Dundas, Colin M.; Sutton, Sarah S; Tamppari, Leslie K; Chojnacki, Matthew (2020).
  Supplementary material for "Mars: Abundant Recurring Slope Lineae (RSL) Following the Planet-Encircling Dust Event (PEDE) of 2018"
  University of Arizona Research Data Repository.
  Dataset. https://doi.org/10.25422/azu.data.13385120


Corresponding Author:   
  Alfred McEwen, University of Arizona, mcewen@lpl.arizona.edu


License:
  CC BY 4.0


DOI:
  https://doi.org/10.25422/azu.data.13385120



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## Summary

Supplementary data and figures provided for "Mars: Abundant Recurring Slope
Lineae (RSL) Following the Planet-Encircling Dust Event (PEDE) of 2018"
submitted to Journal of Geophysical Research - Planets
https://doi.org/10.1029/2020JE006575



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## Files and Folders

- TableS1.xlsx: Supplementary Table S1 - Excel format listing all HiRISE images containing candidate Recurring Slope Lineae following the Mars Year 34 planet-encircling dust event, and other information. Rows containing images that overlap the same target are shaded.

- TableS1.csv: Supplementary Table S1 - CSV format exported from the above Excel file.

- Abbreviations contained in Table S1:
  DDT, Dust Devil Track/s
  MY, Mars Year
  Ls, Solar Longitude
  HiKER, a HiRISE image that closely matches the lighting conditions of a previous image
  bin2, a HiRISE imaging mode, nominally 50 cm/pixel

- FigureS1_animated.gif: Supplementary Figure S1 - Animated GIF image sequence shown in Fig. 3 of the accompanying paper. RSL were active during the decay phase of the PEDE at this location. Here we see a small portion of large image covering a ridge in Coprates Chasma, first before the MY34 PEDE (left), then during the decay phase (middle and right). The middle image was acquired at Ls = 229° (~10° latitude separation from the subsolar latitude), is barely clear enough to see small features (consistent with t ~2 to 3), and shows well-developed RSL that were not present in the prior image from before the PEDE. The right image (Ls = 242.7°) reveals growth at the tips of some of the lineae. Thus RSL were active between Ls = 229° and 242.7° with t > 2 such that less than 10% of the top-of-atmosphere illumination reached the surface. At 10° latitude separation from the subsolar latitude, compared to optical depth (t) = 0.1, t = 2.0 allows ~8.8% of the solar radiation to reach the surface (Levine et al., 1977). Full-resolution and uncropped versions of these and other images shown in this paper are available at https://uahirise.org



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## Additional Notes

Links:
  - https://doi.org/10.1029/2020JE006575