NASA Payloads for (Task Order) TO20A (VIPER) – Astrobotic Technology Griffin Lander

A graphic illustration of the rover known as VIPER. It is mostly grey with blue siding and the central structure is box-like. Four wheels are underneath the rover, which will help it traverse the lunar south pole. Mounted on top of the rover are a couple of additional small structures as well as lights that will shine the way in permanently shadowed regions (PSRS). In the background is a simulation of the Moon’s surface surrounded by black space.

Artist's concept of NASA’s VIPER, which will gather information on the location and concentration of volatiles (e.g. water ice) and other resources at the Moon's South Pole, bringing us closer to agency goals of a greater presence on the Moon as well as exploring Mars and beyond.

NASA / Daniel Rutter

An engineering model of the Volatiles Investigating Polar Exploration Rover, or VIPER, is tested in the Simulated Lunar Operations Laboratory at NASA’s Glenn Research Center in Cleveland, Ohio. The test helped evaluate qualities like the traction of the wheels on the Moon's surface and, here, shows a swimming-like motion capable of pulling the rover out of very soft soils.

NASA / Alcyon Technical Services/ James Zunt

Summary: The Volatiles Investigation Polar Exploration Rover (VIPER) is a lunar polar volatiles prospecting mission developed through NASA’s Science Mission Directorate (SMD) Planetary Science Division with launch in late 2024. The mission includes a rover-borne payload that (1) can locate surface and near-subsurface volatiles, (2) excavate and analyze samples of the volatile-bearing regolith, and (3) demonstrate the form, extractability, and usefulness of the materials. VIPER’s primary mission goal is to characterize the distribution of water and volatiles across a range of thermal environments. This characterization will assist in understanding the origin of lunar polar volatiles and help evaluate the In-Situ Resource Utilization (ISRU) potential of the lunar poles. VIPER will be optimized for lunar regions that receive prolonged periods of sunlight (short lunar nights); prospectively, the mission duration will be more than 100 Earth days, and result in a traverse distance of 20 or more km. For more information on this mission, visit the NASA’s dedicated VIPER site.
- It has headlights, so it can offer us insight into dark places and dark craters that are permanently shadowed. It is the first NASA rover with headlights. This little rover can move sideways, in circles, and basically any direction for maximum mobility. VIPER's camera system will allow operators on Earth to visualize the terrain the rover needs to navigate and send commands in near-real time based on what they see – where and how fast to move, and where to stop and search for water ice. Typically, the operators will tell the rover to move between 12 and 25 feet (4 to 8 meters), before downlinking data and reassessing. VIPER will send its science and prospecting data back using an X-band communications system that connects directly with Earth over the Deep Space Network
Instruments Included: Neutron Spectrometer System (NSS), Near InfraRed Volatiles Spectrometer System (NIRVSS), Mass Spectrometer. Observing Lunar Operations (MSolo), The Regolith and Ice Drill for Exploring New Terrains (TRIDENT) Drill
Type of Instrument: Rover
Key Measurements: Surface and subsurface volatiles (i.e., things that evaporate or sublimate easily)
Task Order: CLPS TO 20A (VIPER)
Lead Development Organization: ARC
Payload PI: Dr. Anthony Colaprete

Neutron Spectrometer System (NSS)

NMLS engineering model without the top plate, showing twin scintillator detectors, electronics, and harnesses enclosed in an Alodine aluminum casing.

The Neutron Measurements at the Lunar Surface (NLMS) will consist of a neutron spectrometer [JC[1] that will measure thermal and epithermal neutron [JC[2] count rates. This instrument is a redesign of the Fast Neutron Spectrometer that has been on the International Space Station. NLMS is being developed at the Marshall Space Flight Center in Huntsville, Alabama.

NASA / MSFC

Summary: Prospects for hydrogen-rich materials while roving, mapping for the distributions. This instrument will determine the abundance of hydrogen-bearing materials along the rover traverse. NSS can measure the total volume of hydrogen up to three feet below the surface. This is better than just detecting the amount of hydrogen from orbit because this gives us a more accurate reading on the presence of subsurface at very small spatial scales. NSS uses radiation to make its measurements. NSS measures the number and energy of neutrons present as radiation on the Moon, which can be used to infer the amount of hydrogen present in the soil. This detection is possible because when neutrons strike a hydrogen atom, they lose a lot of energy.
Type of Instrument: Two Channel Neutron Spectrometer
Key Measurement: NSS Assesses Hydrogen and bulk composition in the top meter of the regolith, measuring down to 0.5% (wt) WEH while roving
Task Order: CLPS TO 20A (VIPER)
Lead Development Organization: (NASA ARC, Lockheed Martin ATC)
Payload PI: Dr. Rick Elphic (NASA ARC)

Note: See also TO2-AB

Near InfraRed Volatiles Spectrometer System (NIRVSS)

A golden device, known as LETS, sits on a white desk. The IR lamp shines a dark purple while the SCI is a dark black. Most of the devices attached to LETS have a circular shape including: the IR lamp, SCI, Spec. Fiber Aperture, LCS, and the LEDs.

NIRVSS will measure surface and subsurface hydration on the Moon. These measurements can be taken while the instrument is moving.

NASA / JSC

Summary: Prospects for surface water “frosts” and evaluates excavated materials. The payload includes a spectrometer, context imager and a thermal radiometer. It measures surface and subsurface hydration (H₂O and OH) and other volatiles, including, for example, CO₂ and CH₄, while simultaneously mapping surface morphology and surface temperature. The plan is for the measurements to take place during rover traverse, throughout areas of targeted volatile investigation (called science stations), and during drilling activities. This instrument was created at NASA Ames Research Center. In total, it has three specific instruments: the near-infrared spectrometer, Ames imaging module, and a thermal radiometer, known as the longwave calibration sensor. To work in shadowed regions NIRVSS carries with it a lamp and seven different colored LEDs which will be used to illuminate the surface when in the dark.
Type of Instrument: NIR Point Spectrometer, 4 Mpxl Panchromatic Imager with 7 LEDs, 4-ch thermal radiometer
Key Measurement: Volatiles including H₂O, OH, and CO₂ and mineralogy, surface morphology/temps
Task Order: CLPS TO20A (VIPER)
Lead Development Organization: NASA ARC / Brimrose Corporation
Payload PI: Dr. Anthony Colaprete

Note: See also TO2-AB

Mass Spectrometer Observing Lunar Operations (MSolo)

A silver instrument in the shape of a cube has an extending cylindrical rod coming out of the front of it. There are two wires coming out of the back part of the top and they run out of the frame. The instrument is sitting on a white table.

This instrument will allow identification of low-molecular-weight volatiles, it’s named the Mass Spectrometer observing lunar operations (MSolo). Some things that MSolo aims to study is classifying different molecules in the exosphere and collect information on possible formation of those volatiles. It is under construction at the Kennedy Space Center, located in Florida.

NASA

Summary: Prospects for surface volatiles while traversing and during drilling. MSolo will identify low-molecular-weight volatiles with unit mass resolution to measure isotopes including D/H and O¹⁸/O¹⁶. In other words, it will identify molecules coming off the surface or out of subsurface samples, including possible water. MSolo will be making these measurements while the rover is driving, sensing gasses that might be released from the lunar soil by the rover wheels, and while the mission is drilling, measuring gasses come out of subsurface samples.
Type of Instrument: Quadrupole mass spectrometer
Key Measurement: Identifying low-molecular weight volatiles between 1-100 amu, unit mass resolution to measure isotopes including D/H and O¹⁸/O¹⁶
Task Order: CLPS TO 20A (VIPER)
Lead Development Organization: (KSC, INFICON)
Payload PI: Dr. Janine Captain, Dr. Jackie Quinn

Note: See also TO2-AB and PRIME-1

The Regolith and Ice Drill for Exploring New Terrains (TRIDENT )

The tall, slender drilling instrument stands upright with silver rods arranged at the base to create stability. The instrument is primarily orange and grey with occasional black components. The thin drill itself looks like an elongated screw, runs vertically along the front, and is stabilized at the top and bottom by larger pieces. The drill bit at the tip of the long drill string has carbide cutting teeth. Along the length of the drill string are spiraling features, similar to a power drill, called flutes.

This 1-meter hammer drill is named The Regolith and Ice Drill for Exploring New Terrains (TRIDENT). It will provide researchers the opportunity to collect lunar surface samples that are about 10 cm in length to then be analyzed by other VIPER instruments.

NASA / KSC

Summary: Excavates lunar regolith and subsurface material to 1-meter deep (3.3 feet) and measures forces, displacements, and temperatures for regolith bulk properties. This brings samples to the surface where other VIPER instruments (NIRVSS and MSolo) can inspect them for the presence of water and other volatiles. Most samples will be about 10 cm in length giving ten samples across the entire 1-meter drill hole. We were able to use a drill like this on Apollo 15, and this will help us maintain longer missions in the future. TRIDENT is a rotary percussive drill, but unlike its ancestor, it does not require human operation. It weighs 16 kg (35 pounds) and should be capable of digging a hole 1-meter deep (3.3 feet) in 10 cm (4 inch) bites. This approach allows for a more accurate determination of how deep substances of interest can be found in the soil. The drill bit at the tip has carbide cutting teeth. These are harder than steel to maintain their sharpness, and strong enough to drill into basalt if needed.
Type of Instrument: 1-meter Hammer drill
Key Measurement: Excavation of sub-surface material; measuring forces, displacements, and temperatures for regolith bulk properties (e.g., subsurface temperature vs. depth; strength of regolith vs. depth)
Task Order: CLPS TO20A (VIPER)
Lead Development Organization: Honeybee Robotics
Payload PI: Dr. Kris Zacny (Honeybee)

Note: See also CLPS TO PRIME-1

Laser Retroreflector (LRA)

The device is a gold-colored ball with a large square flat plate running through the middle and out the sides of the sphere. The gold-colored sphere is hollow with many holes going through it. These holes have a black edge as well as are equidistant from one another.

This generated image shows how the LRA will be located on the surface of the Moon so orbiting spacecraft can retroreflect to find a precise distance.

NASA / GSFC

The Moon’s surface is presented in grey hues with black space in the background. An orbiter is hovering above the surface with graphic images to represent the laser for measurements. There are three orbiters to represent the different positions possible in orbit. In the center of the crater, on the surface of the moon, sits a yellow star to represent the lander’s position.

This diagram shows the concept of the lunar navigation satellite will work. The MAPS algorithms are shown in the black and white lined arrows while GPS signaling is shown in the squiggly red and black arrows.

NASA / MSFC

Summary: A retroreflector bounces any light that shines on it directly backward (180 degrees from the incoming light). The LRA is a collection of eight of these, each a 1.25-cm diameter glass corner cube prism, all embedded in an aluminum hemisphere (painted gold as shown here) and is mounted to the lander deck. This design ensures that the LRA can retroreflect (i.e., bounce) laser light from other orbiting and landing spacecraft over a wide range of incoming directions and efficiently retroreflect the laser signal directly back at the originating spacecraft. This enables precision laser ranging, which is a measurement of the distance between the orbiting or landing spacecraft to the LRA on the lander. The LRA is a passive optical instrument and will function as a permanent fiducial (i.e., location) marker on the Moon for decades to come. (Note: this LRA design is too small for laser ranging from Earth).
Type of Instrument: Passive optical device that reflects laser light directly backward (for laser ranging)
Key Measurement: Precise distances
Task Order: CLPS TO20A (VIPER)
Lead Development Organization: NASA GSFC
Payload PI: Dr. Xiaoli Sun

Note: See also TO2-AB, TO2-IM, and PRIME-1

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