Introduction to JMARS2035
Below is an image that shows the main JMARS2035 user interface. It consists of two main sections: the Layer Manager and the
Pre-loaded Layer Explanations:
Exploration Zone: The Exploration Zone layer marks the extent of where the crew of a 2035 human mission could explore.
To draw this 100km radius circle, the layer must be active. To do so, click the layer in the layer manager and make sure it is
outlined in blue. This indicates the layer is active. To change the color of the Exploration Zone, hold Ctrl while using the scroll wheel.
The mouse mode can be changed to selection from addition mode by right clicking and selecting the desired mode in the menu. Notes can be
added and properties can be changed by double clicking on the layer, and the entire site table can be exported into a csv.
October 2015 Proposed EZs: Locations of all Exploration Zones presented at the First Landing Site / Exploration Zone Workshop
for Human Missions to the Surface of Mars (Houston, TX).
Science ROIs: This marks scientific Regions of Interest within the Exploration Zone. The crew must be able to safely traverse
from the central Landing Zone and Habitation Site to all ROIs. The user can assign names, labels, colors, and notes to each ROI, as well as choose the science categories most closely addressed.
Water Ice Resources:
A sustained human presence would require mining a large quantity of water for human consumption and for fuel.
One source of water is the subsurface ice identified in several locations on Mars. This layer is a work in progress that uses Mars Odyssey Neutron
Spectrometer data to show equivalent weight % water.
This layer marks areas where building resources are present. These include easily accessible metals, silicon, sand,
cobbles (64-256 mm or 2.5-10 in), and bulk regolith.
Solar Flux: This layer shows the calculated average solar flux (W/m2) at the surface. This is useful for considering solar panel efficiency at various latitudes.
Surface Temperature Variations: Thermal insulation requires power and is necessary for crew safety as well as instrument and infrastructure functionality.
Warmer regions or more thermally stable regions are likely desireable.
HiRISE Outlines: The High Resolution Imaging Science Experiment (HiRISE) camera offers unprecedented image quality, giving us a view of the Red Planet in a way never
before seen. It's the most powerful camera ever to leave Earth's orbit. HiRISE offers three data sets, the Experiment Data Record (EDR) data set, the Reduce Data Record (RDR),
and the Digital Terrain Model (DTM) data set. Full resolution HiRISE stamps are accurately projected data for use with other datasets such as CTX data.
CRISM FRT Outlines: The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) is a visible-infrared imaging spectrometer with a scannable field of view.
CRISM can cover wavelengths from 0.362 to 3.92 microns (362 to 3920 nanometers) at 6.55 nanometers/channel, enabling the CRISM team to identify a broad range of minerals on the Martian surface.
Mars 2035 Northern Latitude Mask: This mask was generated for use with the Mars 2035 landing site/exploration zone selection process. This layer masks out latitudes above
50 Degrees N of the equator in accordance with engineering constraints for the landing site.
Mars 2035 Southern Latitude Mask: This mask was generated for use with the Mars 2035 landing site/exploration zone selection process. This layer masks out latitudes below
50 Degrees S of the equator in accordance with engineering constraints for the landing site.
Mars 2035 Thermal Inertia Mask: This mask was generated for use with the Mars 2035 landing site/exploration zone selection process. This layer uses the TES Thermal Inertia
map produced by Phil Christensen to mask out areas with thermal inertia of less than 100 in accordance with engineering requirements to avoid surfaces dominated by dust. The user can
adjust masks as necessary, and can view the calculated thermal inertia and dust statistics for the shapes placed in the Landing Zone, Habitation Zone, Exploration Zone, Food Production
Zone, and ISRU Processing Plant Layers.
Mars 2035 Elevation Mask: This mask was generated for use with the Mars 2035 landing site/exploration zone selection process. This dataset uses MOLA 128ppd elevation with
the threshold to mask out all elevations higher than 2.0 km.
THEMIS Day IR 100m Global Mosaic v11.5: THEMIS Day IR 100 meter/pixel Global Mosaic. The THEMIS 100m/px relative temperature daytime global mosaics were created at the Mars
Space Flight Facility, at Arizona State University, Tempe, Arizona, USA. THEMIS daytime data were selected with the following parameters: shutter closing time less than 150 seconds,
incidence angle less than 85, minimum surface temperature greater than or equal to 160K, 0% saturated pixels from 90S to 90N with unsummed data.
MOLA Shaded Relief/Colorized Elevation: This Mars Orbiter Laser Altimeter (MOLA) instrument colorized shaded relief data layer is derived from Planetary Data
System source images at http://pds-geosciences.wustl.edu/missions/mgs/mola.html. This data product is a shape map of Mars at a resolution of 0.00781 (1/128) by 0.00781
degrees, based on altimetry data acquired by the Mars Global Surveyor MOLA instrument and accumulated over the course of the primary and extended mission. The MOLA Precision
Experiment Data Records (PEDRs) are the source for this data set. The map is in the form of a binary table with one row for each 0.00781-degree latitude. Map coordinates use the
IAU2000 reference system. The binned data include all MOLA nadir observations from the Mapping Phase through the Primary and Extended missions, from the end of aerobraking in
February 1999 through June 2001. Additionally, off-nadir observations of the North pole are included from 87 N latitude and northward, taken during the spring of 1998, and of
both poles taken during Mapping from 87 N and S to the poles. Data are adjusted using a first-order crossover solution for radial, along-track, and across-track position. Parts
of orbits are excluded where solutions for these orbits are deemed to be poor. (Note: subtract 10000 from a MOLA mapping phase orbit number to determine the equivalent MGS Project
orbit number.) Also excluded are shots more than 1.2 degree off-nadir (except as noted above), channel 4 returns, and any returns not classified as ground returns, e.g. clouds or noise,
according to the SHOT_CLASSIFICATION_CODE. A total of nearly 600,000,000 observations are represented.