Mars Odyssey

NASA’s 2001 Mars Odyssey mission created the first global map of chemical elements and minerals that make up the Martian surface.

active Mission

The 2001 Mars Odyssey mission was the first spacecraft to make a global map of the amount and distribution of chemical elements and minerals that make up the Martian surface. The spacecraft also holds the record for the longest continually active mission in orbit around a planet other than Earth. It successfully completed its primary science mission from February 2002 through August 2004.




April 7, 2001




Mapping the chemical elements and minerals that make up the Martian surface

Key Facts

Launch Date: April 7, 2000, 11:02 am EST

Launch site: Cape Canaveral Air Force Station, Florida

Launch Vehicle: Delta II 7925

Mars Orbit Insertion: Oct. 24, 2001

Mission Status: Currently Operating

A view of the biggest canyon in the solar system, captured by NASA's Mars Odyssey orbiter. This canyon system on Mars, named Valles Marineris, stretches as far as the distance from California to New York. Steep walls nearly as high as Mount Everest give way to numerous side canyons, possibly carved by water. In places, walls have shed massive landslides spilling far out onto the canyon floor.

Meet Mars Odyssey

A 3D model of Mars Odyssey.
NASA Visualization Technology Applications and Development (VTAD)

Tech Specs

7.2 feet (2.2 meters) long
5.6 feet (1.7 meters) tall
8.5 feet (2.6 meters) wide
Total Weight
1,598.4 pounds (725.0 kilograms)
Command and Data Handling Subsystem
The heart of this subsystem is a RAD6000 computer, a radiation-hardened version of the PowerPC chip used on most models of Macintosh computers. With 128 megabytes of random access memory (RAM) and three megabytes of non-volatile memory, which allows the system to maintain data even without power, the subsystem runs Odyssey's flight software and controls the spacecraft through interface electronics.

The entire command and data handling subsystem weighs 24.5 pounds (11.1 kilograms).
Electrical power subsystem weighs 189.6 pounds (86.0 kilograms).
Uses hydrazine propellant with nitrogen tetroxide as an oxidizer, produces a minimum thrust of 144 pounds of force (65.3 kilograms) of force.
Each of the four thrusters used for attitude control produces a thrust of 0.2 pound of force (0.1 kilogram) of force. Four 5.0-pound-force (2.3-kilogram-force) thrusters are used for turning the spacecraft.

The entire propulsion subsystem weighs 109.6 pounds (49.7 kilograms).
Odyssey's telecommunications subsystem is composed of both a radio system operating in the X-band microwave frequency range and a system that operates in the ultra high frequency (UHF) range.
The X-band system is used for communications between Earth and the orbiter, while the UHF system is used for communications between Odyssey and any landers present on the Martian surface at any given time.

The telecommunication subsystem weighs 52.7 pounds (23.9 kilograms).


2001 Mars Odyssey has contributed numerous science results supporting the Mars Exploration Program’s overall strategy of “Following the Water.” It has mapped the amount and distribution of chemical elements and minerals that make up the Martian surface. Maps of hydrogen distribution led scientists to discover vast amounts of water ice in the polar regions buried just beneath the surface. Odyssey has also recorded the radiation environment in low Mars orbit to determine the radiation-related risk to any future human explorers who may one day go to Mars.

Terra Sirenum: This color-enhanced mosaic image combines separate frames taken by the Thermal Emission Imaging System (THEMIS), a special camera on NASA's Mars Odyssey orbiter. On the southwest edge of the immense volcanic region of Tharsis, lava from its giant volcanoes flowed down to meet the old cratered landscape of Terra Sirenum. Scientists cannot say how many years separate the flows from the terrain they engulfed, but the relationship between the two tells a complex tale.
NASA/JPL-Caltech/University of Arizona

Science Objectives

To contribute to the four Mars Exploration Program science goals, Mars Odyssey has the following science objectives:

  • Globally map the elemental composition of the surface.
  • Determine the abundance of hydrogen in the shallow subsurface.
  • Acquire high spatial and spectral resolution images of the surface mineralogy.
  • Provide information on the morphology of the Martian surface.
  • Characterize the Martian near-space radiation environment as related to radiation-induced risk to human explorers.

Science Instruments

  • Thermal Emission Imaging System

    The Thermal Emission Imaging System (THEMIS) views the visible and infrared reflections from the Martian surface to make a map showing the location of different mineral concentrations and their relationship to various landforms.
    By looking at the visible and infrared parts of the spectrum, THEMIS is determining the distribution of minerals on the surface of Mars and helping scientists understand how the mineralogy of the planet relates to the landforms.

Tech Specs

Main Job
To determine the distribution of minerals on the surface of Mars
On the body of the orbiter
24.7 pounds (11.2 kilograms)
14 watts
Data Return
IR Imager: Instantaneous internal rate of 1.17 Mbits/sec. Data rate to spacecraft after real-time compression is 0.6 Mbits/sec.
Visible Imager: Instantaneous internal rate of up to 6.2 Mbits/sec. Data rate to spacecraft is <1.0 Mbits/sec.
Color Quality
5 visual bands: 0.425 microns, 0.540 microns, 0.654 microns, 0.749 microns, 0.860 microns.
10 infrared bands: 6.78 microns (used twice), 7.93 microns, 8.56 microns, 9.35 microns, 10.21 microns, 11.04 microns, 11.79 microns, 12.57 microns, 14.88 microns.
Image Size
Visible camera has a 1024 x 1024 pixel array with 5 filters. IR focal plane has 320 cross-track pixels and 240 down-track pixels covered by 10˜1-μm-bandwidth strip filters in nine different wavelengths.
Image Resolution
Visual images: 59 feet (18 meters) per pixel
Infrared images: 328 feet (100 meters) per pixel
Focal Length
~7.8 inch (20 centimeter) effective focal length
Focal Ratio
Field of View
IR Imager: 4.6 degree (80 mrad) cross-track by 3.5 degree (60 mrad) down-track FOV with a 0.25 mrad (100 m) IFOV at nadir.
Visible Imager: 2.66 degree (46.4 mrad) cross-track by 2.64 degree (46.1 mrad) down-track FOV with 0.045 mrad (18 m) IFOV in 1024 x 1024 pixels at nadir. The two imagers are spatially bore-sighted.


In the infrared spectrum, the instrument uses 9 spectral bands to help detect minerals within the Martian terrain. These spectral bands, similar to ranges of colors, can obtain the signatures (spectral "fingerprints") of particular types of geological materials. Minerals, such as carbonates, silicates, hydroxides, sulfates, hydrothermal silica, oxides and phosphates, all show up as different colors in the infrared spectrum. This multi-spectral method allows researchers to detect in particular the presence of minerals that form in water and to understand those minerals in their proper geological context. THEMIS' infrared capabilities have significantly improved the data from TES, a similar instrument on Mars Global Surveyor.

The instrument's multi-spectral approach also provides data on localized deposits associated with hydrothermal and subsurface water and enables 328-foot (100-meter) images of Martian terrain to be captured in each pixel, or single point, of every image.

During the Martian day, the sun heats the surface. Surface minerals radiate this heat back to space in characteristic ways that can be identified and mapped by the instrument. At night, since it maps heat, the imager searches for active thermal spots.

ASTER, an Earth-orbiting instrument on the Terra spacecraft, has used a similar approach to map the distribution of minerals here on Earth.

Variations in the thermal infrared "color" in the right-hand image are due to differences in the kinds of minerals that make up rocks and soil. In the visible part of the spectrum that our eyes can see (left-hand image), it would not be apparent what minerals are present.

How THEMIS Works in the Visible

The part of the imaging system that takes pictures in visible light is able to show objects about as big as a semi-truck. This resolution helps fill in the gap between large-scale geological images from the Viking orbiters in the 1970s and the very high-resolution images from the currently orbiting Mars Global Surveyor.
For more information, visit the THEMIS instrument site at Arizona State University.

  • A black and silver cone-shaped device, wrapped in gold foil around its center, sits atop a dull gray ring on a table in a workshop or lab. Instead of a point, its top is short, squat, cylinder, and veers off-center, toward the upper left of the image at a 120-degree ange. The cylinder is also gold around its top edge, which is reeded like the edge of a coin, and the entire device has white wires plugged into it at various locations.

    Gamma Ray Spectrometer

    The Gamma Ray Spectrometer (GRS) measures the abundance and distribution of many elements of the periodic table, including hydrogen, silicon, iron, potassium, thorium, and chlorine. Knowing what elements are at or near the surface gives detailed information about how Mars has changed over time. To determine the elemental makeup of the Martian surface, the experiment uses a gamma ray spectrometer and two neutron detectors.

Tech Specs

Main Job
To determine the elemental makeup of the Martian surface
On the body of the orbiter; gamma sensor head on 20-foot (6.2-meter) boom.
67.2 pounds (30.5 kilograms)
32 watts
Gamma Sensor (GS): 18.4 inches (46.8 centimeters) by 21.0 inches (53.4 centimeters) by 23.8 inches (60.4 centimeters)
Neutron Spectrometer (NS): 6.8 inches (17.3 centimeters) by 5.7 inches (14.4 centimeters) by 12.4 inches (31.4 centimeters)
High-Energy Neutron Detector (HEND): 11.9 inches (30.3 centimeters) by 9.8 inches (24.8 centimeters) by 9.5 inches (24.2 centimeters)
Data Return
Collects a new spectrum approximately every 20 seconds, 360 times per orbit.
Gamma Sensor (GS): Strikes from high-energy ionizing photons or charged particles are amplified, measured and digitally converted into one of 16,384 (214) channels, or bins.
Neutron Spectrometer (NS): Detects neutrons in three energy bands: thermal, epithermal, and fast.
High-Energy Neutron Detector (HEND): Neutrons are detected in thermal (0.01 eV - 1 eV), epithermal (1 eV - 1 keV), fast (1 keV - 1 MeV), and high-energy (1 MeV - 10 MeV) energy ranges.
Spatial Resolution
186 miles (300 kilometers)

How GRS Works

When exposed to cosmic rays (charged particles in space that come from the stars, including our Sun), chemical elements in soils and rocks emit uniquely identifiable signatures of energy in the form of gamma rays. The gamma ray spectrometer looks at these signatures, or energies, coming from the elements present in the Martian soil. By measuring gamma rays coming from the Martian surface, it is possible to calculate how abundant various elements are and how they are distributed around the planet's surface.

A global map of Mars, showing a wide band of colors, mostly yellow, orange, and red, along the equator. The areas closest to the north and south poles shades of are deep blue and purple.
This map is based on gamma rays from the element hydrogen on Mars.

Gamma rays, emitted from the nuclei of atoms, show up as sharp emission lines on the instrument's spectrum. While the energy represented in these emissions determines which elements are present, the intensity of the spectrum reveals the element's concentrations. The spectrometer has added significantly to the growing understanding of the origin and evolution of Mars and the processes shaping it today and in the past.

How GRS Helps Detect Water

By measuring neutrons, it is possible to calculate the abundance of hydrogen on Mars, thus inferring the presence of water. The neutron detectors are sensitive to concentrations of hydrogen in the upper meter of the surface. Like a virtual shovel "digging into" the surface, the spectrometer allows scientists to peer into this shallow subsurface of Mars and measures the amount of hydrogen that exists there. Since hydrogen is most likely present in the form of water ice, the spectrometer is able to measure directly the amount of permanent ground ice and how it changes with the seasons.

Nuclear radiation from a planetary surface.
NASA/JPL/University of Arizona

Mars Radiation Environment Experiment

Led by NASA's Johnson Space Center, this science investigation characterized aspects of the radiation environment both on the way to Mars and in the Martian orbit.

Since space radiation presents an extreme hazard to crews of interplanetary missions, the experiment predicted anticipated radiation doses that would be experienced by future astronauts and is helping to determine possible effects of martian radiation on human beings.

Mars exploration space radiation comes from cosmic rays emitted by our local star, the Sun, and from stars beyond our solar system as well. Space radiation can trigger cancer and cause damage to the central nervous system. Similar instruments were flown on the space shuttles and are also flown on the International Space Station (ISS), but before Odyssey none had ever flown outside of Earth's protective magnetosphere, which blocks much of this radiation from reaching the surface of our planet.

The Mars Radiation Environment Experiment (MARIE), an instrument to characterize aspects of the radiation environment both on the way to Mars and in the Martian orbit.

How the Instrument Works

A spectrometer inside the instrument measured the energy from these radiation sources.

The instrument, with a 68-degree field of view, collected data during Odyssey's cruise from Earth to Mars. It stored large amounts of data for downlink whenever possible, and operated in orbit around Mars until a large solar event bombarded the Odyssey spacecraft on October 28, 2003. MARIE has been unable to collect data since that time, and engineers believe the most likely cause is that a computer chip was damaged by a solar particle smashing into the MARIE computer board.

Tech Specs

Main Job
To help provide a context for high-resolution analysis of key spots on Mars provided by HiRISE and CRISM.
On the body of the orbiter
7.3 pounds (3.3 kilograms)
7 watts
11.6 inches (29.4 centimeters) by 9.1 inches (23.2 centimeters) by 4.3 inches (10.8 centimeters)
Data Return
Data is saved on 60 Mb of flash memory and transferred at <8 Mbits per day over an RS-422 low speed data line.
Measures particles in the range of 15 MeV to 500 MeV/nucleon.
Field of View
68 degrees
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