Method: Search limited to latitudes south of 75◦S. All MOC NA images in the PDS archive that cover regions inside this area were checked visually for the presence of spider patterns. Images that contain single spiders, spider arrays, or spider ravines were selected for further analysis. Each of such images was counted as one entry. The archive covers the period from September 1997 to March 2004. We found 326 images that contain spider patterns.
Feature: The name ”martian spiders” was introduced by the MOC team to describe structures that show several branches diverging from one common center. Soon after the first detection they were discovered to be negative topographical features (depressions) – i.e. radial troughs or channels.
Methods Using the Mars version of Google Earth (earth.google.com/mars/), we surveyed Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) and Mars Express High Resolution Stereo Camera (HRSC) images near previously documented ridge occurrences. We then reviewed the 887 MRO High Resolution Imaging Science Experiment (HiRISE) images in the HiRISE catalog that were tagged with the keyword “ridges” by the HiRISE team (www.uahirise.org; as of 5/30/16). Where polygonal ridge networks were present, we mapped their regional extents using the broader spatial coverage of CTX data within the geographic information system software ArcGIS. The entire area of the Medusae Fossae Formation and the Hellas Basin floor deposits were separately surveyed at CTX scale to find additional ridge networks where HiRISE data were sparse.
Significance The diversity of the ridge networks implies a variety of formational mechanisms.
Citation: Milliken, R. E., J. F. Mustard, and D. L. Goldsby, Viscous flow features on the surface of Mars: Observations from highresolution
Mars Orbiter Camera (MOC) images, J. Geophys. Res., 108(E6), 5057, doi:10.1029/2002JE002005, 2003
All data were re-drawn as ellipses that best fit the feature in THEMIS Day imagery and/or MOLA relief. All values were calculated from the re-drawn ellipses.
Lat/Lon are calculated as the centers of ellipses, not Lat/Lon values in the source papers
Diameter, area, perimeter are calculated from the ellipses, and are not taken from the source papers. Diameter is an average, calculated from perimeter.
Height (Max. elev, range of elevation) data are calculated from within the ellipses, and are not taken from the source papers. Heigh data is from MOLA gridded data. MAX=max elevation point within the ellipse, MIN: min. elevation value point within the ellipse
Type/interpretations are taken from the source papers. For small cones and mounds, interpretations vary (pingo/volcano/mud volcano). All features that have at least one volcanic interpretation in a recent (ca. last two decades) paper are included. Features previously (Viking) identified as volcanic but recently reclassified are not included.
Confidence. Major and minor shields, calderas, fissure/small/low shields and lava domes can be considered as confirmed, while all others are candidate volcanic features.
Group: a single ellipse is one example showing actual size, which is part of a group of similar sized features. These are typically interpreted as pseudocraters (rootless cones) or pingos or mud volcanoes.
Type: Caldera: size/range values represent caldera, not volcanic construct (if any). These are caldera volcanoes without substantial construct. (negative relief forms)
Henrik Hargitai, with the help of P. Broz
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