{"references": ["Shean, D.E., Alexandrov, O., Moratto, Z.M., Smith, B.E., Joughin, I.R., Porter, C., Morin, P., 2016. An automated, open-source pipeline for mass production of digital elevation models (DEMs) from very-high-resolution commercial stereo satellite imagery. ISPRS J. Photogramm. Remote Sens. 116, 101\u2013117. https://doi.org/10.1016/j.isprsjprs.2016.03.012", "Rodriguez Sanchez-Vahamonde, C., 2019. Quantification of Surface Roughness of Lava Flows on Mars (MSc Thesis), University of Western Ontario,115p", "McEwen, A. S., Eliason, E. M., Bergstrom, J. W., Bridges, N. T., Hansen, C. J., Delamere, W. A., \u2026 Weitz, C. M. (2007). Mars reconnaissance orbiter's high resolution imaging science experiment (HiRISE). Journal of Geophysical Research E: Planets, 112(5), 1\u201340. https://doi.org/10.1029/2005JE002605"]}

In an effort to better understand the surface roughness of Martian lava flows, we generated the 35 HiRISE DTMs using ISIS3 and ASP and extracted their roughness (Rodriguez Sanchez-Vahamonde, 2019). We have posted the DTMs generated for public use here. HiRISE stereo images typically have a spatial sampling of 25 - 50 centimeters, providing us with DTMs of 1 - 2 meters per pixel. We also converted the HiRISE stereo-pair ID for each product into its proper DTM ID using the NASA Planetary Data System product naming convention for HiRISE DTMs (https://www.uahirise.org/dtm/about.php; last accessed 18.09.2019).