These are the gypsum, carbonate, nontronite, montmorillonite, and kaolinite spectral libraries used in Tarnas et al. (2021) Successes and challenges of factor analysis/target transformation application to visible-to-near-infrared hyperspectral data, Icarus doi.org/10.1016/j.icarus.2021.114402 The spectra in these libraries were all measured in the NASA Reflectance Experiment Laboratory (RELAB; http://www.planetary.brown.edu/relabdocs/relab.htm). They were created by extracting all spectra from the RELAB database that were associated with each specific mineral name. For example, if the word "gypsum" was in the RELAB sample description, the spectrum of that sample would be extracted and placed in the gypsum spectral library. This means that the libraries include many spectral mixtures, as well as pure mineral endmembers. They are not curated by-eye. They were resampled to the spectral sampling interval of the Headwall hyperspectral images used in Tarnas et al. (2021) Successes and challenges of factor analysis/target transformation application to visible-to-near-infrared hyperspectral data, Icarus doi.org/10.1016/j.icarus.2021.114402. They are available as .txt files and .sli files (ENVI spectral libraries with associated .hdr files). Use the spectral ID unique to each spectrum to find information on the samples in the RELAB database hosted on the PDS Geosciences Node (https://pds-speclib.rsl.wustl.edu/search.aspx?catalog=RELAB). RELAB data are archived at the PDS Geosciences Node and can be accessed at: https://pds-geosciences.wustl.edu/spectrallibrary/default.htm. Thanks to Takahiro Hiroi and Ralph Milliken for operating RELAB. Copyright 2014, Brown University, Providence, RI.; All Rights Reserved Permission to use, copy, modify, and distribute any of these data and their documentation for any purpose other than its incorporation into a commercial product is hereby granted without fee, provided that the above copyright notice appear in all copies and that both that copyright notice and this permission notice appear in supporting documentation, and that the name of Brown University not be used in advertising or publicity pertaining to distribution of the data without specific, written prior permission. BROWN UNIVERSITY DISCLAIMS ALL WARRANTIES WITH REGARD TO THESE DATA, INCLUDING ALL IMPLIED WARRANTIES OF MERCHANTABILITY AND FITNESS FOR ANY PARTICULAR PURPOSE. IN NO EVENT SHALL BROWN UNIVERSITY BE LIABLE FOR ANY SPECIAL, INDIRECT OR CONSEQUENTIAL DAMAGES OR ANY DAMAGES WHATSOEVER RESULTING FROM LOSS OF USE, DATA OR PROFITS, WHETHER IN AN ACTION OF CONTRACT, NEGLIGENCE OR OTHER TORTIOUS ACTION, ARISING OUT OF OR IN CONNECTION WITH THE USE OR PERFORMANCE OF THESE DATA.

Venus is home to thousands of volcanic landforms that range in size from less than 5 km in diameter to well over 100 km in diameter, and their extrusive materials comprise ~80% of the surface. With the NASA Magellan SAR (synthetic aperture radar) FMAP (full-resolution radar map) left- and right-look global mosaics at 75 meter-per-pixel (m/px) resolution, we created a global catalog of volcanic edifices on Venus that contains ~85,000 features, ~99% of which are volcanoes.Additionally, we developed an automated approach to grouping volcanoes into volcanic fields, often referred to as "shield fields" on Venus. Volcanic fields are areas with relatively high spatial concentrations of shield- or dome-like volcanic edifices that are ≤20 km in diameter. This global dataset can be used as a tool to investigate the morphological, spatial, and temporal properties of volcanoes on Venus.