The dataset contains the extracted water vapor abundances from the Mars Express instruments PFS and SPICAM.
The dataset is organized in columns and given time, location, dust opacity and water vapor abundances between 0 and 5 km, and over the full atmospheric column.
Contributors:Kevin Cannon, Ralph Fritsche, Daniel Batcheldor, Trent Smith, Daniel Britt
- Particle size distribution for the MGS-1 prototype simulant
- Visible-near infrared spectra of MGS-1 prototype simulant and previous Mars simulants for comparison
- Thermogravimetry analysis data for MGS-1 prototype
- Evolved Gas Analysis for MGS-1 prototype
This dataset contains processed data: in the excel table all the band spectral parameters (position, width, area, depth) retrieved are reported, as a function of temperature and of grain size.
Zipped file geodatabase and "readme" plain text file. The geodatabase includes mapping of recurring slope lineae (RSL) for 10 different HiRISE images, mapping of dust devil tracks and rockfall markings in HiRISE images across four Mars years, and some manual traces of notable RSL growth. All 3D information is derived from a smoothed digital terrain model (except where explicitly noted otherwise, that is, for certain long profiles only), which in turn is derived from stereo HiRISE imagery. See published paper for additional details.
The raw seismic data in seed format and temperature and other data in csv format for an experiment where seismometers were deployed on and below the engineering model of the Mars Science Laboratory Curiosity rover in order to demonstrate feasibility of deck-mounted instruments. Tools for plotting and processing the data consistent with the study are available at https://github.com/mpanning/MSL-experiment
Contributors:Joshua Cahill, Alex Boosalis, Nhan Nguyen, Samuel Lawrence, Brett Denevi, David Blewett
Optical constants for iron and nickel metals from the far-ultraviolet through the near-infrared.
Contributors:Atkinson J., Durham W.B., Seager S.
Stress and displacement (where applicable) data for experiments conducted at MIT concerning the cryogenic deformation of Bishop Tuff and Indiana Limestone. Pictures also included where applicable.
Contributors:Anderson R.B., Rubin D.M., Lewis K.W., Edgar L.A., Newman C.
gale2_1mded.tif = Digital elevation model of the study area.
PSP_001422_1750_RED.jp2 = Full-resolution HiRISE image of the study area.
PSP_001422_1750_REDmos_hijitreged_o1m.j2k = 1m scale ortho image.
*.tfw files are "world files" containing map projection information.
Contributors:Blain D., Li C., Orton G., Fouchet T., Encrenaz T., Drossart P., Greathouse T., Charnay B., Bezard B., Lellouch E., N. Fletcher L.
Contains three spectral cubes of Jupiter at 5 microns obtained on 16 January 2016 (UT) using Texas Echelon X-Echelle Spectrograph (TEXES) mounted on the InfraRed Telescope Facility (IRTF) at Mauna Kea, Hawaii.
The spectral cubes have a size of ~60x95 pixels, depending of the cube. On each spectral cube, nearly all the disk of Jupiter is visible, lacking only a few pixels near the poles.
The three spectral cubes together cover the 90--360 system III degree west longitudinal range.
The spectral range is comprised between ~1930 and ~1945 cm-1 (~5 microns), divided in ~200 samples with a spectral resolution of ~0.15 cm-1.
This spectral range contains essentially a NH3 line located at ~1939 cm-1, and probes the atmosphere of Jupiter in the 1--4 bar region.
More informations can be found in the README file (including a file format description and examples of utilization), and in the related article.