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ODE - About Missions, Instruments, and Products
Tell me more about the Mars Reconnaissance Orbiter (Mars ODE)
   Tell me more about CRISM (Mars ODE)
   Tell me more about CTX (Mars ODE)
   Tell me more about MRO Gravity/Radio Science (Mars ODE)
   WTell me more about HiRISE (Mars ODE)
   Tell me more about SHARAD (Mars ODE)
   Tell me more about MCS (Mars ODE)
Tell me more about the Mars Express (Mars ODE)
   Tell me more about HRSC (Mars ODE)
   Tell me more about MARSIS (Mars ODE)
   Tell me more about OMEGA (Mars ODE)
   Tell me more about PFS (Mars ODE)
Tell me more about the Mars Global Surveyor (Mars ODE)
   Tell me more about MOC (Mars ODE)
   Tell me more about MOLA (Mars ODE)
Tell me more about MESSENGER (Mercury ODE)
   Tell me more about MESSENGER's Gamma Ray Spectrometer Instrument (Mercury ODE)
   Tell me more about MESSENGER's Neutron Spectrometer Instrument (Mercury ODE)
   Tell me more about MESSENGER's X-Ray Spectrometer Instrument (Mercury ODE)
   Tell me more about MESSENGER's MASCS Instrument (Mercury ODE)
   Tell me more about MESSENGER's MDIS Instrument (Mercury ODE)
   Tell me more about MESSENGER's MLA (Mercury ODE)
   Tell me more about MESSENGER's Radio Science Experiment (Mercury ODE)
Tell me more about Clementine Mission (Lunar ODE)
   Tell me more about Clementine's UVVIS Camera (Lunar ODE)
   Tell me more about Clementine's NIR Camera (Lunar ODE)
   Tell me more about Clementine's LWIR Camera (Lunar ODE)
   Tell me more about Clementine's HiRes Camera (Lunar ODE)
   Tell me more about Clementine's Star Tracking Cameras (Lunar ODE)
   Tell me more about Clementine's LIDAR Instrument (Lunar ODE)
   Tell me more about Clementine's Radio Science Experiments (Lunar ODE)
Tell me more about Lunar Prospector Mission (Lunar ODE)
   Tell me more about Lunar Prospector's Gamma Ray Spectrometer Instrument (Lunar ODE)
   Tell me more about Lunar Prospector's Nuetron Spectrometer Instrument (Lunar ODE)
   Tell me more about Lunar Prospector's Alpha Particle Spectometer Instrument (Lunar ODE)
   Tell me more about Lunar Prospector's Magnetometer Instrument (Lunar ODE)
   Tell me more about Lunar Prospector's Electron Reflector Instrument (Lunar ODE)
   Tell me more about Lunar Prospector's Doppler Gravity Experiment Instrument (Lunar ODE)
 
Tell me more about the Mars Reconnaissance Orbiter (ODE Mars)
The Mars Reconnaissance Orbiter (MRO) is NASA's latest mission to Mars. MRO carries several instruments including CRISM, CTX, HiRISE, SHARAD, MCS, and a Gravity/Radio Science experiments.
  • Zurek, R. W., and S. E. Smrekar (2007), An overview of the Mars Reconnaissance Orbiter (MRO) science mission, J. Geophys. Res., 112, E05S01, doi:10.1029/2006JE002701.
Tell me more about CRISM (ODE Mars)
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. CRISM produces a wide range of products. More information can be found in:
CRISM is one of the instruments that participate in MRO coordinated observations and can be correlated with HiRISE and CTX images though the MRO Coordinated Obs tab.

Suggestions on finding CRISM products through ODE (particularly TRDRS and DDRs)
How does ODE relate to the CRISM Instrument Team Science Web Site?
The CRISM instrument team maintains an web site for searching and reviewing CRISM products here
Tell me more about CTX (ODE Mars)
The Mars Reconnaissance Orbiter (MRO)'s Context Camera (CTX) is designed to obtain grayscale (black & white) images of Mars at 6 meters per pixel scale over a swath 30 kilometers wide. CTX provides context images for the MRO HiRISE and CRISM. Information about CTX products can be found in: Note, CTX products are stored at the PDS Imaging Node. Please read more about the use of products stored at other PDS nodes in the "Why are there differences between HiRISE, CTX, and the other ODE products" section.

CTX is one of the instruments that participate in MRO coordinated observations and can be correlated with HiRISE and CRISM images though the MRO Coordinated Obs tab.

You may also search CTX images through the PDS Imaging Node 's MRO-specific image search capability. The ODE website complements the PDS Imaging Node's Atlas website by providing cross mission and instrument searches for imaging and non-imaging data products.

Tell me more about MRO Gravity/Radio Science (ODE Mars)
MRO's Gravity Experiment uses Radio Science data from the spacecraft to explore Mars gravity. The radio science Experiment Data Records (EDR) archive is available through ODE. More information about these products can be found in:
Several Reduced Data Record products are also available. More information about these products can be found in:
Tell me more about HiRISE (ODE Mars)
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 two data sets, the Experiment Data Record (EDR) data set and the Reduce Data Record (RDR) data set. EDRs are raw images from the spacecraft. RDRs are combined and processed images based on several EDRs. Most users will want to use the RDRs. Note: HiRISE changed the RDR format in mid-2008 to include embedded map projection information within the JPEG 2000 files. This allows the files to be easily projected in GIS tools such as ESRI's ArcGIS. The change is ignored by tools that do not use embedded map projections. These changes are described in version 1.1 of the HIRISE RDR Product Software Interface Specification (SIS) (PDF). Products without the embedded map projection information are in the data set MRO-M-HIRISE-3-RDR-V1.0 and projects with the embedded map projection information are in the data set MRO-M-HIRISE-3-RDR-V1.1. Overtime, HiRISE expects to replace all older V1.0 products with newer V1.1 versions. In the mean time, ODE offers both. Versions 1.0 products can be search with the RDR product type and Version 1.1 products can be search with the RDRV11 product type. Search on both to find products of either type. Information about HiRISE products can be found in: Note: ODE also presents the HiRISE RDR Anaglyphs as a separate product type. These are files stored in the EXTRAS directory of the HiRISE archive. ODE presents them as separate product types to make it easier to search, view, download, and add them to the cart.

Note, HiRISE products are stored at the PDS HiRISE Data Node. Please read more about the use of products stored at other PDS nodes in the "Why are there differences between HiRISE, CTX, and the other ODE products" section.

HiRISE is one of the instruments that participate in MRO coordinated observations and can be correlated with CTX and CRISM images though the MRO Coordinated Obs tab.

You may also search HiRISE images through the PDS Imaging Node 's MRO-specific image search capability. The ODE website complements the PDS Imaging Node's Atlas website by providing cross mission and instrument searches for imaging and non-imaging data products.

Tell me more about SHARAD (ODE Mars)
The Shallow Subsurface Radar (SHARAD) instrument probes the subsurface using radar waves using a 15-25 MHz frequency band in order to get the desired high depth resolution. The instrument has a horizontal resolution of between 0.3 and 3 kilometers (between 2/10 of a mile and almost 2 miles) horizontally and 15 meters (about 50 feet) vertically in free space (better than 10 m in Mars subsurface). Subsurface features will have to be of the order of these dimensions for them to be observable.
SHARAD offers two data sets, the Experiment Data Record (EDR) data set and the Reduce Data Record (RDR) data set. EDRs are raw radar data from the spacecraft. EDRs are processed into RDRs. Most users will want to use the RDRs. Information about SHARAD products can be found in:
Tell me more about MCS (ODE Mars)
The Mars Climate Sounder is a follow-on experiment to PMIRR, the Pressure Modulator Infrared Radiometer lost with the Mars Observer spacecraft, and to PMIRR2, lost with the Mars Climate Orbiter. MCS observes radiation with 21 detectors in each of nine spectral bands; eight thermal infrared channels are used to characterize atmospheric temperature, pressure, water vapor, and condensates, while the remaining spectral channel (operating in the visible and near infrared, 0.3-3.0 microns) is used primarily to understand the effects of solar radiation on the Martian energy budget.
MCS looks near the horizon of Mars at the atmospheric limb to observe the atmosphere in 21 vertical samples simultaneously, with measurements centered approximately 5 kilometers (3 miles) through the atmosphere at the limb. From these observations vertical distributions ("profiles") of temperature, pressure, water vapor, dust, and condensates are determined. . These profiles are combined into daily, three-dimensional global maps for both daytime and nighttime. Analyzing these profiles and maps should lead to a better understanding of Martian weather and, eventually, of Martian climate.
MCS offers two data sets, the Experiment Data Record (EDR) data set and the Reduce Data Record (RDR) data set. EDRs are raw radar data from the spacecraft. EDRs are processed into RDRs. Most users will want to use the RDRs. Information about MCS products can be found in: You may also search MCS images through the PDS Atmospheres Node.
Tell me more about the Mars Express (ODE Mars)
The European Space Agency (ESA)'s Mars Express mission or MEX carries four instruments whose data is currently supported by ODE, HRSC, MARSIS, PFS, and OMEGA.

Tell me more about HRSC (ODE Mars)
The Mars Express High Resolution Stereo Camera (HRSC) will image the entire planet in full color, 3D and with a resolution of about 10 meters. Selected areas will be imaged at 2-metre resolution. One of the camera's greatest strengths will be the unprecedented pointing accuracy achieved by combining images at the two different resolutions. The HRSC RDR data set contains radiometrically calibrated images.

ODE supports the search, retrieval, and ordering of HRSC RDR products. More information about HRSC RDR products can be found the in: The HRSC REFDR data sets consists of radiometrically calibrated and map projectyed images. A sinusoidal equal area map projection is used for images located between -85 and 85 degrees latitude. Images at the poles are projected in a polar stereographc projection.. See the DSMAP.CAT file for more information on the projections.

ODE supports the search, retrieval, and ordering of HRSC REFDR products. More information about HRSC REFDR products can be found in: The HRSC DTM data sets consist of ortho image versions of the nadir channel and the four color channel data. The data set also contains versions of stereo-derived topographical data referenced to a sphere and to the aeroid. A polar stereographic projection is used for the data from the polar regions and a sinusoidal projection is used for non-polar images.

The HRSC filenaming scheme will help you determine which products are which in the data set:
  • H0010_0009_BL4.IMG BL = blue
  • H0010_0009_DA4.IMG DA = DEM aeroid
  • H0010_0009_DT4.IMG DT = DEM sphere
  • H0010_0009_GR4.IMG GR = green
  • H0010_0009_IR4.IMG IR = near IR
  • H0010_0009_ND4.IMG ND = nadir
  • H0010_0009_RE4.IMG RE = red
ODE supports the search, retrieval, and ordering of HRSC DTM products. More information about HRSC DTM products can be found the in: You may also search HRSC images through the PDS Imaging Node's Atlas website. The ODE website complements the PDS Imaging Node's Atlas website by providing cross mission and instrument searches for imaging and non-imaging data products.

Tell me more about MARSIS (ODE Mars)
The Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) instrument was developed by a team of Italian and United States researchers and is flying on the ESA Mars Express spacecraft. The MARSIS Subsurface Sounding Radar/Altimeter primary objective is to map the distribution of water and ice in the upper portions of the Martian crust. The instrument analyzes reflections of radio waves in the upper 2-3 km of Martian crust to reveal the subsurface structure. MARSIS also studies the ionosphere by characterizing the interaction of the solar wind with the ionosphere and upper atmosphere of Mars. The MARSIS Principal Investigator is Prof. Giovanni Picardi, Universita di Roma 'La Sapienza', Rome, Italy.

ODE supports the search, retrieval, and ordering of MARSIS EDR, Active Ionosphere Sounding RDR, and Subsurface RDR products. More information about MARSIS EDR products can be found in:
Tell me more about OMEGA (ODE Mars)
The Mars Express Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité (OMEGA) visible and infrared mineralogical mapping spectrometer will map the Martian surface with an IFOV of 1.2 mrad (4.1 arc minutes), and acquire for each resolved pixel the spectrum from 0.36 to 5.2 µm in 352 contiguous spectral channels (spectels) in the nominal mode.

ODE supports the search, retrieval, and ordering of OMEGA EDR products. More information about OMEGA products can be found the in:
A note on OMEGA products. OMEGA data products have a Product ID of the form ORBXXXX_Y_DATA where XXXX is the orbit number and Y is an increment per orbit. Each OMEGA data product has a corresponding geometry product with a Product ID of ORBXXXX_Y_GEOM. OMEGA data products are stored in directories under DATA as ORBZZ where ZZ is the first two digits of the orbit number. The corresponding geometry files are stored in directories under DATA as GEMZZ where ZZ is the first two digits of the orbit number. An example is:
  • mex-m-omega-2-edr-flight-v1\mexomg-0001\data\orb18\orb1801_0.qub
  • mex-m-omega-2-edr-flight-v1\mexomg-0001\data\gem18\gem1801_0.nav
With this product ID scheme, any search made with ODE will return a list of products generated during orbit that alternate between data products and geometry products making finding a data product's corresponding geometry product very easy. You can also look at the "Related Products" tab of the products detail page. For the data products, the drop down "Related & Source Products" will show the related geometry product. For the geometry products, the drop down "Related & Derived Products" will show the related data product.

Tell me more about PFS (ODE Mars)
The Mars Express Planetary Fourier Spectrometer (PFS) instrument - The PFS is determining the composition of the Martian atmosphere from the wavelengths of sunlight (in the range 1.2-45 microns) absorbed by molecules in the atmosphere and from the infrared radiation they emit. In particular, it will measure the vertical pressure and temperature profile of carbon dioxide which makes up 95% of the martian atmosphere, and look for minor constituents including water, carbon monoxide, methane and formaldehyde.

ODE supports the search, retrieval, and ordering of PFS EDR products. More information about PFS products can be found the in:
Tell me more about the Mars Global Surveyor (ODE Mars)
NASA's Mars Global Surveyor mission or MGS carries one instruments whose data is currently supported by ODE, MOC.

Tell me more about MOC
The The Mars Global Surveyor's Mars Orbital Camera (MOC) instrument - The MOC science investigation used 3 instruments: a narrow angle camera that obtained grayscale (black-and-white) high resolution images (typically 1.5 to 12 m per pixel) and red and blue wide angle cameras for context (240 m per pixel) and daily global imaging (7.5 km per pixel). MOC operated in Mars orbit between September 1997 and November 2006. It returned more than 240,000 images spanning portions of 4.8 Martian years.
ODE supports the search, retrieval, and ordering of MOC EDR products. More information about MOC products can be found in: You may also search MOC images through the PDS Imaging Node's various search tools. The ODE website complements the PDS Imaging Node's Atlas website by providing cross mission and instrument searches for imaging and non-imaging data products.

Note: MOC location data is taken from USGS's Unified Planetary Coordinate (UPC) database.

Tell me more about MOLA
The The Mars Global Surveyor's Mars Orbital Laser Altimeter (MOLA) instrument - The principal components of MOLA are a diode-pumped, Nd:YAG laser transmitter that emits 1.064 micrometer wavelength laser pulses, a 0.5 m diameter telescope, a silicon avalanche photodiode detector, and a time interval unit with 10 nsec resolution. Additional delay fibers increase the effective resolution to 2.5 ns. When in the Mapping Phase of the mission, MOLA provided measurements of the topography of Mars within approximately 160 m footprints and a center-to-center along-track footprint spacing of 300 m along the MGS nadir ground-track. Range measurements, with an effective resolution of 37 cm, were converted to profiles of planetary radius and topographic height after correction for orbit and pointing errors. Radial accuracy of individual profiles was approximately 1 m RMS, as determined by altimetric crossovers, and shot locations are determined to within 100 m in the along-track and across-track directions. MOLA profiles have been assembled into global grids referenced to Mars' center-of-mass, with resolutions of up to 1/128 degree per pixel, although at this density some interpolation is required across-track. Other standard data products include near-global grids of footprint-scale roughness and 1.064 micrometer surface reflectivity. The background solar illumination noise level provides seasonal maps of narrow-band Lambert albedo.
The MOLA standard science data products are the Aggregated Experiment Data Record (AEDR) - all MOLA raw data aggregated by orbit; Precision Experiment Data Record (PEDR) - MOLA science data processed into profiles with precision orbit locations added; Precision Radiometry Data Records (PRDR); and the Experiment Gridded Data Record (MEGDR) - MOLA gridded data in various densities.
ODE supports the search, retrieval, and ordering of MOLA PEDR, PRDR, SHADR, and MEGDR products. More information about MOC products can be found in:
In addition to access to the MOLA archive, ODE offers both individual derived products and the MOLA PEDR Query tool found under the Tabs tool. PEDR and MEGDR products offer several image versions of the products. More information about the MOLA PEDR Query tool can be found here

Tell me more about MESSENGER (ODE Mercury)
NASA's Mercury Surface, Space Environment, Geochemistry, and Ranging (MESSENGER) mission was launched in August 2004 on a long journey to Mercury. The spacecraft will complete one flyby of Earth, two of Venus, and three of Mercury before entering Mercury's orbit in March 2011 for an orbital phase of one Earth year. The data provided by MESSENGER's multiple instruments will answer questions about Mercury's crust and polar deposits, atmospheric and magnetospheric structure, and tectonic history. MESSENGER carries seven instruments and experiments whose data is currently supported by ODE: GRS, NS, XRS, MASCS, MDIS, MLA, and the Radio Science experiment.

Tell me more about MESSENGER's Gamma Ray Spectrometer Instrument (ODE Mercury)
The MESSENGER Gamma Ray Spectrometer (GRS) instrument measures gamma rays emitted from Mercury's surface in the energy range 0.1 to 10 MeV. This allows identification of elements, such as O, Si, S, Fe, H, K, Th, and U, and their abundances.
ODE supports the search, exploration, and download of GRS EDR (uncalibrated) data products, which include raw spectral, shield spectral, anti-coincident spectral, microphonics, software event counter, and instrument state/status data.
More information about the GRS can be found in:

Tell me more about MESSENGER's Neutron Spectrometer Instrument (ODE Mercury)
The MESSENGER Neutron Spectrometer (NS) instrument measures the flux of ejected neutrons in three energy ranges [thermal neutrons (0.025 to 1 eV), epithermal neutrons (1 eV to 500 keV), and fast neutrons (500 keV to 7 MeV]. This allows identification of elements, such as Fe, Ti, Gd, Sm, Cl, C, H, and their abundances. The NS will map H abundance over Mercury's northern hemisphere.
ODE supports the search, exploration, and download of NS EDR (uncalibrated) data products, which include raw spectral, event, galactic cosmic ray, gamma burst, short science, time-correlated count, instrument state/status, and calibration/diagnostic data.
More information about the NS can be found in:

Tell me more about MESSENGER's X-Ray Spectrometer Instrument (ODE Mercury)
The MESSENGER X-Ray Spectrometer (XRS) instrument measures X-rays emitted from Mercury's surface in the energy range ~1 to 10 keV. This allows measurement of the surface abundances of Mg, Al, Si, Ca, Ti, and Fe.
ODE supports the search, exploration, and download of XRS EDR (uncalibrated) data products, which include raw spectral data and associated instrument parameters.
More information about the XRS can be found in:

Tell me more about MESSENGER's MASCS Instrument (ODE Mercury)
The MESSENGER Mercury Atmospheric and Surface Composition Spectrometer (MASCS) instrument consists of an Ultraviolet-Visible Spectrometer (UVVS) and a Visible-Infrared Spectrograph (VIRS). UVVS covers the wavelength ranges of the far ultraviolet (115-180 nm), middle ultraviolet (160-320 nm), and visible (250-600 nm), with an average spectral resolution of 0.6 nm. VIRS covers the wavelength ranges of the visible (300-1050 nm) and near infrared (850-1450 nm), with an average spectral resolution of 5 nm. MASCS will investigate the composition and structure of Mercury's exosphere and map surface reflectance over Mercury's surface on spatial scales of 5 km.
ODE supports the search, exploration, and download of MASCS EDR (uncalibrated) data products, which include raw UVVS and VIRS spectral and instrument engineering data.
More information about MASCS can be found in:

Tell me more about MESSENGER's MDIS Instrument (ODE Mercury)
The MESSENGER Mercury Dual Imaging System (MDIS) instrument consists of two cameras, a multispectral Wide Angle Camera (WAC) and a monochrome Narrow Angle Camera (NAC), mounted on a common pivot platform. MDIS data will be used to construct a global image base map, a digital terrain model, global maps of color properties, and mosaics of high-resolution image strips.
ODE supports the search, exploration, and download of MDIS EDR (uncalibrated) and CDR (calibrated) data products, which include post-launch checkout images, flyby images of Earth, Venus, and Mercury, and the Moon, and in-flight calibration images.
The MDIS data sets are archived at the PDS Imaging Node. In addition to ODE, you may also search MDIS images through the PDS Imaging Node's various search tools. The ODE website complements the PDS Imaging Node's Atlas website by providing cross mission and instrument searches for imaging and non-imaging data products.
More information about MDIS can be found in:

Tell me more about MESSENGER's MLA (Mercury ODE)
The MESSENGER Mercury Laser Altimeter (MLA) instrument is a solid-state pulsed laser that measures the distance between the spacecraft and the surface of Mercury to a 30-cm precision at ranges up to 1000 km. Data from the MLA will be used to map northern hemisphere topography and the altimetry of polar craters.
ODE supports the search, exploration, and download of MLA EDR (uncalibrated) data products, which include raw laser ranges, instrument status, and hardware diagnostic information.
More information about MLA can be found in:

Tell me more about MESSENGER's Radio Science Experiment (ODE Mercury)
The MESSENGER Radio Science (RS) experiment consists of radio observations carried out using the MESSENGER spacecraft and Earth-based observing systems of the NASA Deep Space Network (DSN). The observations are designed to generate high-resolution gravity field models of Mercury.
ODE supports the search, exploration, and download of RS EDR (uncalibrated) data products.
More information about the RS experiment can be found in:
Tell me more about the Clementine Mission (Lunar ODE)
Clementine (Nozette et al., 1994; McEwen and Robinson, 1997) was a 1994 joint NASA/ Department of Defense (DoD) mission to the Moon. Clementine carried four cameras, one with a laser-ranging system. The cameras included an ultraviolet-visual (UVVIS) camera, a long wavelength infrared (LWIR) camera, a Laser Image Detection and Ranging (LIDAR) high-resolution (HiRes) camera, and a near-infrared (NIR) camera. The spacecraft also had two star tracker cameras (STC), used mainly for altitude determination but also as wide-field cameras for various scientific and operational purposes. The following table provides basic information about all the Clementine cameras.

Table 1 Clementine instrument parameters (Nozette et al., 1994)
UVVIS Star tracker NIR LWIR HiRes LIDAR
receiver*		 LIDAR
transmitter**
Focal plane array Thomson
CCD		 Thomson CCD Amber InSb Amber HgCdTe Intensified CCD SiAPD  
Pixel format 384 x 228 384 x 576 256 x 256 128 x 128 384 x 288 Single Cell  
Pixel size (mm) 23 x 23 23 x 23 38 x 38 50 x 50 23 x 23 0.5 mm2  
Clear aperture (mm) 46 14 29 131 131 Shared with HiRes 38
Focal length (mm) 90 17.5 96 350 1250 Shared with
HiRes		 99
Array field of view (degrees) *** 5.6 x 4.2 28 x 43 5.6 x 5.6 1.0 X 1.0 0.4 x 0.3 0.057  
Bandpass filters (mm) 0.415± 0.020
0.750±0.005
0.900±0.015
0.950±0.015
1.000±0.015
0.4 to 0.95		 0.4 to 1.1 1.1± 0.03
1.25± 0.03
1.5± 0.03
2.00 ± 0.03
2.60±0.03
2.78 ± 0.06		 8.0 to 9.5 0.415± 0.020
0.560± 0.005
0.650± 0.005
0.750±0.010
0.4 to 0.8 		0.4 to 1.1 1.064 and 0.532
Integration times (ms) 0.2 to 773 0.2 to 773 11, 33, 57, 95 0.144, 1.15, 2.30, 4.61 0.2 to 773    
Gains 150, 350, and 1000 e/bit 75, 150, and 350 e/bit 0.5 to 36x 0.5 to 36x 150, 350, and 1000 e/bit 100x  
Offsets (bits) 5 5 8 8 5 None  
Power (W) 4.5 4.5 11.0 13.0 9.5 Housed in HiRes 6.8 at 1 Hz; 2.6 quiescent
Weight (g) 410 290 1920 2100 1120 Housed in HiRes 1250

* The A/D resolution of the LIDAR receiver was 14 bits (40 m per bit), whereas all of the cameras had a resolution of 8 bits.

** The laser used for the LIDAR was an Nd-YAG that produced a pulse of width <10 ns. At a wavelength of 1.064 mm, it produced a pulse with an energy of 171 mJ and a divergence of <500 mrad. At a wavelength of 0.532 mm, it produced a 9-mJ pulse with a 4-mrad divergence.

*** see Figure 1 (Nozette et al., 1994).

For over two months, Clementine mapped the 38 million square kilometers of the Moon, producing the first multispectral global digital map of the Moon, the first global topographic map, and contributing several other important scientific discoveries, including the possibility of ice at the lunar South Pole. Clementine was the first mission known to conduct an in-flight autonomous operations experiment (Nozette et al., 1994; Sorensen and Spudis, 2005). More information about the mission can be found in the following documents:
  • Nozette, S., P. Rustan, L.P. Pleasance, D.M. Horan, P. Regeon, E.M. Shoemaker, P.D. Spudis, C.H. Acton, D.N. Baker, J.E. Blamont, B.J. Buratti, M.P. Corson, M.E. Davies, T.C. Duxbury, E.M. Eliason, B.M. Jakosky, J.F. Kordas, I.T. Lewis, C.L. Lichtenberg, P.G. Lucey, E. Malaret, M.A. Massie, J.H. Resnick, C.J. Rollins, H.S. Park, A.S. McEwen, R.E. Priest, C.M. Pieters, R.A. Reisse, M.S. Robinson, R.A. Simpson, D.E. Smith, T.C. Sorenson, R.W. Vorder Bruegge, and M.T Zuber (1994), The Clementine Mission to the Moon: Scientific Overview: Science Vol. 266, pp. 1835-1839.
  • McEwen, A.S., M. Robinson (1997), Mapping of the Moon by Clementine: Adv. Space Research, Vol. 19, No. 10, pp. 1523-1533.
  • Sorensen T.C. and P.D. Spudis (2005), The Clementine Mission - A 10-year perspective: J. Earth System Sci. Vol. 114, 6, pp. 645-668.

Tell me more about Clementine's UVVIS Camera (Lunar ODE)
TheClementine Ultraviolet/Visible (UVVIS) camera (Kordas et al., 1995; Malaret et al., 1998; Jolliff, 1999; Gaddis et al., 2000) had a catadioptric telescope with fused silica lenses focused onto a metachrome-coated charge-couple-device (CCD) imager. Active wavelength response was limited on the short wavelength end by the transmission of fused silica and the optical blur of the lens. Wavelength response on the long end was limited by the response of the CCD. The camera had a filter wheel with six filters allowing observations at the 415, 750, 900, 950, 1000 nm, and a broad band between 400 to 950 nm wavelengths.

The UVVIS imaging instrument was primarily used to support lunar mineral mapping investigations. Pole-to-pole nadir observations with solar phase angles kept to less than 30 degrees at mid-latitudes were the predominant viewing conditions during the two month systematic mapping phase of the mission.

ODE supports the search, retrieval, and download of UVVIS Experiment Data Record (EDR) products, and two additional data sets: the Clementine Basemap Mosaic and the Clementine UVVIS Digital Image Model (DIM) Mosaic. More information about UVVIS products can be found in:
Tell me more about Clementine's NIR camera (Lunar ODE)
The Clementine Near-Infrared (NIR) camera used a catadioptric lens with a 256 x 256 indium antimonide (InSb) focal plane array (FPA) mechanically cooled to cryogenic temperature. The FPA was operated at 70 ± 0.5 K at the Moon. The instrument has six bands at wavelengths of 1100, 1250, 1500, 2000, 2600, and 2780 nm. NIR camera electronic design was virtually identical to the LWIR camera. The NIR and LWIR cameras also shared a common cryocooler and dewar design, with minor modifications made to accommodate cold shield and cold filter differences.

ODE supports the search, retrieval, and download of NIR Experiment Data Record (EDR) products. Information about NIR EDR products can be found in:
Tell me more about Clementine's LWIR camera (Lunar ODE)
The Clementine Long Wavelength Infrared (LWIR) camera used a catadioptric lens with a 128 x 128 mercury cadmium telluride (HCT) focal plane array (FPA). The FPA was operated at 65 K. Wavelength range was controlled by the cold filter to 8.0 to 9.5 microns. LWIR camera electronic design was virtually identical to the NIR camera. The NIR and LWIR cameras also shared a common cryocooler and dewar design, with minor modifications made to accommodate cold shield and cold filter differences.

ODE supports the search, retrieval, and download of two LWIR data sets, the Experiment Data Record (EDR) data set and the Reduce Data Record (RDR) data set. EDRs are raw images from the spacecraft. RDRs are calibrated brightness temperature images. Information about LWIR products can be found in:
Tell me more about Clementine's HiRes camera (Lunar ODE)
The Clementine High-Resolution (HiRes) camera combined a lightweight beryllium telescope with an image intensifier-coupled frame transfer CCD imager. Spectral response was limited in the system by the S-2 photocathode between 0.4 and 0.8 microns. Five spectral bands at wavelengths of 415, 560, 650, 750, and a broad band between 400 to 800 nm were selectable from a filter wheel. A sixth filter position was allocated to an opaque filter for the image intensifier's protection.

ODE supports the search, retrieval, and download of HiRes Experiment Data Record (EDR) and HiRes Mosaic products. Information about HiRes products can be found in:
Tell me more about Clementine's Star tracking cameras (Lunar ODE)
The Clementine Star tracking cameras (STC: A-STAR and B-STAR) used silicon CCD technology with a 384 x 576 pixel array sensitive between 0.4 and 1.1 micrometers. It had a wide field of view, 28 degrees x 43 degrees, to make more stars available for attitude determination. Its instantaneous field of view (IFOV) was 1.3 mrad. STCs were primarily used for spacecraft navigation and orientation. The scientific uses of these cameras are secondary. The line-transfer electronic shuttering limited imaging to dim targets such as the lunar surface illuminated by earthshine. Information about STC products can be found in:
Tell me more about Clementine's LIDAR (Lunar ODE)
The Clementine Laser Image Detection and Ranging (LIDAR) unit shared the telescope of the HiRes camera, splitting the 1064 nm return signal from the Nd-yttrium-aluminum-garnet (Yag) source off to an avalanche photodiode (APD) detector with a dichroic filter. Range was determined by the number of clock cycles since a laser output start pulse was received. The clock counter had only 14 bits, owing to the hardware limitations. In order to allow returns up to the 640 km maximum range required in the lunar orbit, returns from the discriminator were binned 4 to a clock count, turning the 23 MHz response into a 39.972 meter height bin. Internal memory in the LIDAR unit saved up to 6 "returns" per laser firing, with up to 4 saved between programmable search range minimum/maximum values. Threshold was set for the best compromise between missed detection and false alarms.

ODE supports the search, retrieval, and download of LIDAR topography reduced data products. Information about LIDAR products can be found in:
Tell me more about Clementine's Radio Science Experiments (Lunar ODE)
Two different types of Radio Science (RS) experiments were conducted with Clementine: radio tracking experiments in which the magnitude and direction of the planet's gravity field were derived from the Doppler and ranging measurements and radio propagation experiments in which modulation on the signal received on Earth could be attributed to properties of the intervening medium. Two types of radio propagation experiments were carried out: radio occultations by the lunar limb and bistatic radar scattering from the lunar surface.

The Clementine spacecraft telecommunications subsystem served as part of a Radio Science instrument for investigations of the Moon. The remainder of the 'instrument' was located at ground stations of the NASA Deep Space Network (DSN). Much of the equipment at both ends was shared, being used for routine telecommunications as well as for Radio Science.

ODE supports the search, retrieval, and download of data from the bistatic surface scattering measurements (raw, partially processed FND, and reduced data) and gravity measurements. Information about RS experiment products can be found in:
Tell me more about the Lunar Prospector Mission (Lunar ODE)
Lunar Prospector (LP) (Andolz, 1998; Binder, 1998) was a spin-stabilized spacecraft, operating in a 100 km circular, polar orbit around the Moon during its Primary Mission in 1998. The orbit was lowered to 30 km for the Extended Mission that began in January 1999. The mission ended on July 31, 1999, when the spacecraft was targeted to impact a crater near the lunar south pole to try to vaporize part of the suspected water deposits.

The science goals of LP were to map the Moon's surface composition and its magnetic and gravity fields, to determine the frequency and location of gas release events, and to search for polar ice deposits. To meet these objectives, LP had five science instruments (Feldman et al., 2004) located on three booms: a Gamma Ray Spectrometer (GRS), a Neutron Spectrometer (NS), an Alpha Particle Spectrometer (APS), a Magnetometer (MAG), and an Electron Reflectometer (ER). In addition, Doppler tracking data was used to derive gravity measurements. The three spectrometers determined the composition and evolution of the lunar surface to a depth of more than ten centimeters. The GRS mapped crustal composition, the APS sensed volatile release activity, and the NS mapped hydrogen distribution. The spatial resolution of the three spectrometers was about 200 km at the nominal LP mapping altitude of 100 km, and about 60 km at the low altitude orbit of 30 km. The MAG/ER produced a high resolution map of the lunar magnetic field, and the spacecraft's downlink carrier signal was examined for gravity-induced Doppler shifts from which a high resolution global gravity map was generated. More information about the LP mission can be found in the following documents:
  • Andolz, F.J. (1998), Lunar Prospector Mission Handbook, Document No. LMMS/P458481, Lockheed Martin Missiles and Space Company, 63p [Url: http://pds-geosciences.wustl.edu/missions/lunarp/schandbk.pdf].
  • Binder, Alan B. (1998), Lunar Prospector: Overview: Science, Vol. 281, pp. 1475-1476.
  • Feldman, W.C., K. Ahola, B.L. Barraclough, R.D. Belian, R.K. Black, R.C. Elphic, D.T. Everett, K.R. Fuller, J. Kroesche, D.J. Lawrence, S.L. Lawson, J.L. Longmire, S. Maurice, M.C. Miller, T.H. Prettyman, S.A. Storms, G.W. Thornton (2004), The Gamma-Ray, Neutron, and Alpha-Particle Spectrometers for the Lunar Prospector Mission, J. Geophys. Res., Vol. 109, E07S06, doi:10.1029/2003JE002207.
  • Lunar Prospector Spacecraft Handbook
Tell me more about the Lunar Prospector's Gamma Ray Spectrometer Instrument (Lunar ODE)
The Lunar Prospector's Gamma Ray Spectrometer (GRS) instrument measured gamma rays emitted from the lunar surface in the energy range 0.3 to 9 MeV with a channel energy width of 17.6 keV. This allowed identification of elements, such as Fe, Ti, Th, K, Si, O, Mg, Al, and Ca to depths of 20 cm, and their abundances.

ODE supports the search, exploration, and download of GRS MDR (Level 0, raw) and GRS RDR (corrected) data products. Level 0 data consist of a set of 19 volumes containing raw data from the three spectrometers (GRS, NS, APS), the magnetometer, and the electron reflectometer, along with ancillary files. RDR data contain fully corrected 32-second data accumulations from GRS. Several GRS special products may be of interest to the geoscience community. These special products are available at the PDS Geoscience Node. Additionally, GRS Level 1 data are also available to be downloaded from the Geosciences Node. The level 1 dataset includes counting rate data for integrated spectra, as well as thorium and potassium. More information about the GRS can be found in:
Tell me more about the Lunar Prospector's Neutron Spectrometer Instrument (Lunar ODE)
The Lunar Prospector's Neutron Spectrometer (NS) instrument measured the flux of ejected neutrons in four energy ranges [thermal neutrons (0 to 0.4 eV), epithermal neutrons (0.4 eV to 0.7 MeV), moderated neutrons (0 to 0.8 MeV) and fast neutrons (0.8 MeV to 8 MeV)]. Neutron measurements from LP were used to determine the surface abundance of hydrogen at both poles of the Moon (Feldman et al., 1998, 2000, 2001), as well as to provide an initial estimate of solar wind implanted hydrogen over the entire lunar surface (Johnson et al., 2002; Genetay et al., 2003). In addition, LP measurements were used to map the distribution of Gd + Sm abundances (Elphic et al., 1998, 2002), titanium abundances (Elphic et al., 2002), as well as the mean atomic mass of the surface soils (Maurice et al., 2000; Gasnault et al., 2001) on the Moon.

ODE supports the search, exploration, and download of NS MDR (Level 0, raw) and NS RDR (corrected) data products. Level 0 data consists of a set of 19 volumes containing raw data from the three spectrometers (GRS, NS, APS), the magnetometer, and the electron reflectometer, along with ancillary files. RDR data contains fully corrected 32-second data accumulations from NS. The data products include thermal and epithermal neutron counts at high and low altitude with either an 8-second or 32-second sample period, fast neutron counts at high and low altitude with a 32-second sample period, moderated neutron counts at low altitude with a 32-second sample period, and position information files for both altitudes and both sample periods. Several NS special products may be of interest to the geoscience community. These special products are available in PDS Geoscience Node. Additionally, NS Level 1 data are also available to be downloaded from the Geosciences Node. This dataset includes counting rate data for thermal and epithermal neutrons. More information about the NS can be found in:
  • LP Level 0 Volume Software Interface Specification
  • LP Spectrometer Software Interface Specification (SIS) (PDF:V001, V002, V003)
  • NS PDS Catalog Files
  • HTTP/FTP access to NS data set volumes
  • Additional references
    • Elphic, R.C., D.J. Lawrence, W.C. Feldman, B.L. Barraclough, S. Maurice, A.B. Binder, and P.G. Lucey (1998), Lunar Fe and Ti abundances: Comparison of Lunar Prospector and Clementine data, Science, 281, pp. 1493 - 1496.
    • Elphic, R.C., D.J. Lawrence, W.C. Feldman, B.L. Barraclough, O.M. Gasnault, S. Maurice, P.G. Lucey, D.T. Blewett, and A.B. Binder (2002), Lunar Prospector neutron spectrometer constraints on TiO2, J. Geophys. Res., Vol. 107(E4), 5024, doi:10.1029/2000JE001460.
    • Feldman, W.C., B.L. Barraclough, S. Maurice, R.C. Elphic, D.J. Lawrence, D.R. Thomsen, and A.B. Binder (1998), Major compositional units of the Moon: Lunar Prospector thermals and fast neutrons, Science, 281, pp. 1483 - 1493.
    • Feldman, W.C., D.J. Lawrence, R.C. Elphic, B.L. Barraclough, S. Maurice, I. Genetay, and A.B. Binder (2000), Polar hydrogen deposits on the Moon, J. Geophys. Res., Vol. 105, pp. 4175 - 4195.
    • Feldman, W.C., et al. (2001), Evidence of water ice near the lunar poles, J. Geophys. Res., 106, 23,231 - 23,252.
    • Gasnault, O., W.C. Feldman, S. Maurice, I. Genetay, C. d'Uston, T.H. Prettyman, and K.R. Moore (2001), Composition from fast neutrons: Application to the Moon, Geophys. Res. Lett., 28, pp. 3797 - 3800.
    • Genetay, I., S. Maurice, W.C. Feldman, O. Gasnault, D.J. Lawrence, R.C. Elphic, C. d'Uston, and A.B. Binder (2003), Lunar neutrons at energies less than 500 keV, Planet. Space Sci., 51(3), pp. 271 - 280.
    • Johnson, J.R., W.C. Feldman, D.J. Lawrence, S. Maurice, T.D. Swindle, and P.G. Lucey (2002), Lunar Prospector epithermal neutrons from impact craters and landing sites: Implications for surface maturity and hydrogen distribution, J. Geophys. Res., Vol. 107(E2), 5008, doi:10.1029/2000JE001430.
    • Maurice, S., W.C. Feldman, D.J. Lawrence, O. Gasnault, C.d'Uston, I. Genetay, and P.G. Lucey (2000), High-energy neutrons from the Moon, J. Geophys. Res., Vol. 105, pp. 20,365 - 20,375.
Tell me more about the Lunar Prospector's Alpha Particle Spectrometer Instrument (Lunar ODE)
The Lunar Prospector's Alpha Particle Spectrometer (APS) instrument measured the number and distribution of transient lunar outgassing events and their role as sources of the tenuous lunar atmosphere. The experiment investigated possible correlations of outgassing events with locations of young impact craters and tectonic features. APS consisted of five pairs of 3 cm by 3 cm square ion-implant silicon detectors, each pair placed on one face of a cube. They were covered by thin, Al-coated polypropylene foils to exclude sunlight. The sensors had a spectral resolution of about 100 KeV at 5.5 MeV. The combined field-of-view for the 5 sensor pairs was nearly 3-pi steradians, with the only blind spot being in the direction of the spacecraft bus. The APS had a mass of 4 kg and uses about 7 W of power (Binder et al., 1998).

ODE supports the search, exploration, and download of APS MDR (Level 0, raw) data products. Level 0 data consist of a set of 19 volumes containing raw data from the three spectrometers (GRS, NS, APS), the magnetometer, and the electron reflectometer, along with ancillary files. Additionally, APS Level 1 data are available to be downloaded from the PDS Geosciences Node. This dataset is organized by time. Each file contains approximately one day of data. Each record includes time of day, latitude, longitude, height of spacecraft above the surface, APS face number, look angle, and energy level. More information about the APS can be found in:
  • Binder, A.B., W.C. Feldman, G.S. Hubbard, A.S. Konopliv, R.P. Lin, M.H. Acuna, and L.L. Hood (1998), Lunar Prospector searches for polar ice, a metallic core, gas release events, and the moon's origin, Eos, Trans. AGU, 79, 97.
  • Lawson, S.L., W.C. Feldman, D.J. Lawrence, K.R. Moore, R.C. Elphic, R.D. Belian, and S. Maurice (2005), Recent outgassing from the lunar surface: The Lunar Prospector Alpha Particle Spectrometer, J. Geophys. Res., VOL. 110, E09009, doi: 10.1029/2005JE002433.
  • LP Level 0 Volume Software Interface Specification
  • LP Spectrometer Software Interface Specification (SIS) (PDF: V001, V002, V003)
  • APS PDS Catalog Files
  • FTP access to APS data set volumes
Tell me more about the Lunar Prospector's Magnetometer Instrument (Lunar ODE)
The Lunar Prospector's Magnetometer (MAG) instrument was based on the instrument flown on the Mars Global Surveyor spacecraft (Acuna et al., 1992). Some changes were made to the Lunar Prospector version to account for the spinning spacecraft. Also, there was only one magnetometer sensor on Lunar Prospector. The MAG instrumentation consisted of a 3-axis fluxgate magnetometer and an electronics box. The electronics box was common to the MAG and its companion instrument, the Electron Reflectometer (ER). The MAG sensor was a wide-range (up to +/- 65,536 nT), low-noise (6 pT RMS), high-sensitivity (as low as +/- 2 pT), triaxial fluxgate magnetometer. The MAG sensor was an 11 x 6.5 x 9 cm box.

The MAG/ER experiment investigated the origin and nature of lunar crustal magnetic fields and constrained the size of a metallic core. The experiment provided global maps of the lunar crustal magnetic fields and provided estimates of the lunar induced magnetic dipole moment (Binder et al., 1998). More information about the MAG can be found in:
Note: The browse directory contains plots (in GIF87A format) which summarize the MAG and ER data, in one-month subdirectories. Each of these files contains plots of 12 hours of data. Since all MAG data are stored in ASCII files containing one day of data per file, ODE Bunter combines two separate browse data from 0-12 and 12-24 time intervals in one image, and output it in PNG format. The naming convention of the output browse image is ffYYMMDD.PNG where ff is the dataset identifier and YYMMDD is the year, month and day of data in the file.
Tell me more about the Lunar Prospector's Electron Reflectometer Instrument (Lunar ODE)
The Lunar Prospector's Electron Reflectometer (ER) instrument was based on the instrument flown on the Mars Global Surveyor spacecraft (Acuna et al., 1992). Some changes were made to the Lunar Prospector version to account for the spinning spacecraft. The ER instrumentation consisted of a symmetric hemispherical electrostatic analyzer and an electronics box. The electronics box was common to the ER and its companion instrument, the Magnetometer (MAG). The ER had a 360 degree disk-shaped field-of-view. The electrostatic optics selected energy and focused the particles onto an imaging detector. The ER sensor was a 12 cm diameter cylinder and was 9 cm high.

The MAG/ER experiment investigated the origin and nature of lunar crustal magnetic fields and constrained the size of a metallic core. The experiment provided global maps of the lunar crustal magnetic fields and provided estimates of the lunar induced magnetic dipole moment (Binder et al., 1998). More information about the ER can be found in:
Note: The browse directory contains plots (in GIF87A format) which summarize the MAG and ER data, in one-month subdirectories. Each of these files contains plots of 12 hours of data. Since all ER data are stored in ASCII files containing one day of data per file, ODE Bunter combines two separate browse data from 0-12 and 12-24 time intervals in one image, and output it in PNG format. The naming convention of the output browse image is ffYYMMDD.PNG where ff is the dataset identifier and YYMMDD is the year, month and day of data in the file.
Tell me more about Lunar Prospector's Doppler Gravity Experiment (Lunar ODE)
The Lunar Prospector's Doppler Gravity Experiment (DGE) used Doppler tracking of S-Band radio signals to characterize the spacecraft orbit and determine the lunar gravity field. The experiment provided the first complete gravity map of the Moon. More information about the experiment and the data products can befound in: