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Grant Agreement




Project full title

Planetary mapping


D 7.3

Deliverable Name

Data Management Plan Update

Nature of deliverable


Dissemination level


Scheduled delivery date`

31st May 2019



Prepared by:

Verified by:

Approved by:

Table of Contents

Executive Summary

The updated Planmap Data Management Plan (DMP) is provided. Map-wide metadata structure and fields for planmap mapping products are described and exemplified. The long-term data repository venues for Planmap products are listed and specified. Delivery file formats are updated, as reflected by deliverables. Described aspects in this DMP include: beneficiaries producing data, adherence to FAIR principles, data types, formats and standards, metadata, documentation, intellectual property and data storage, archiving and curation during and after the proejct.

List of acronyms

ASCIIIAmerican Standard Code For Information Interchange
ASIAgenzia Spaziale Italiana
CC-BYCreative Commons Attribution (license)
CRISMCompact Reconnaissance Imaging Spectrometer for Mars
CRSCoordinate Reference System
CTXContext Camera
DoADescription of Action
DOIDigital Object Identifier
EPN-TAPEuroPlaNet Table Access Protocol (TAP)
ESAEuropean Space Agency
FELICSFast Efficient & Lossless Image Compression System
FTPFile Transfer Protocol
HRSCHigh Resolution Stereo Camera
ISISIntegrated Software for Imagers and Spectrometers
GDALGeospatial Data Abstraction Library
GNUGNU's Not Unix (recursive acronym)
GPLGNU General Public License
H2020Horizon 2020 (Framework Programme)
HiRISEHigh Resolution Imaging Science Experiment
OMEGAObservatoire pur la Minéralogie, l'Eau, les Glaces et l'Activité
LROCLunar Reconnaissance Orbiter Camera
M3Moon Mineralogy Mapper
MESSENGERMErcury, Surface, Space ENvironment, GEochemistry and Ranging
MDISMercury Dual Imaging System
MLAMercury Laser Altimeter
MOCMars Orbiter Camera
NACNarrow Angle Camera
OGCOpen Geospatial Consortium
PDSPlanetary Data System (archive, organisation, standard)
PSAPlanetary Science Archive (ESA planetary archive)
RDRReduced Data Record
ROIRegion of Interest
SMESmall, Medium Enterprise
SNRSignal to Noise Ratio
SPICESpacecraft  Planet Instrument C-matrix (orientation) Events
SWIRShort-Wave InfraRed (spectral range)
TAPTable Access Protocol (VO)
USGSUnited States Geological Survey
VESPAVirtual European Solar and Planetary Access
VICARVideo Image Communication And Retrieval
VNIRVisible and Near Infrared (spectral range)
VOVirtual Observatory
WACWide Angle Camera
WPWork Package


PLANMAP will both use and produce data. Different data categories can be distinguished in the framework of PLANMAP:


Complementing metadata related to invidivual units, each map of Planmap include several map-wide field, exemplified below :

FieldField description (and example entries)
Map name (PM_ID)PM-MER-MS-H02_3cc_01
Target bodyMercury
Title of mapGeologic Map of the Victoria Quadrangle (H02), Mercury
Bounding box - Min Lat-22.5°
Bounding box - Max Lat65°
Bounding box - Min Lon (0-360)270°
Bounding box - Max Lon (0-360)360°

Valentina Galluzzi; Laura Guzzetta; Luigi Ferranti; Gaetano di Achille; David A. Rothery; Pasquale Palumbo

Output scale1:3M
Original Coordinate Reference System

Lambert conformal conic

Center longitude: 315°

Standard parallel 1: 30°

Standard parallel 2: 58°

Datum: 2440 km (non-IAU, MESSENGER team datum)

Data used

MESSENGER MDIS BDR v0 uncontrolled basemap (166 m/pixel)

MESSENGER MDIS 2013 complete uncontrolled basemap (250 m/pixel)

MESSENGER MDIS uncontrolled mosaics v6, v7, v8 (250 m/pixel)

MESSENGER MDIS partial mosaic (USGS) (200 mpp)

MESSENGER MDIS 2011 albedo partial mosaic (USGS) (200 m/pixel)

Mariner 10 + MESSENGER flyby uncontrolled basemap (USGS) (500 m/pixel)


MESSENGER MDIS M2 flyby stereo-DTM (DLR) (1000 m)

Standards adhered toMapping scale: Tobler (1987); Output scale: USGS; Symbology: USGS FGDC and other new symbols
AimsMorpho-stratigraphic analysis of Mercury's units and BepiColombo target selection.
Short description

Mercury’s quadrangle H02 ‘Victoria’ is located in the planet’s northern hemisphere and lies between latitudes 22.5° N and 65° N, and between longitudes 270° E and 360° E. This quadrangle covers 6.5% of the planet’s surface with a total area of almost 5 million km2. Our 1:3,000,000-scale geologic map of the quadrangle was produced by photo-interpretation of remotely sensed orbital images captured by the MESSENGER spacecraft. Geologic contacts were drawn between 1:300,000 and 1:600,000 mapping scale and constitute the boundaries
of intercrater, intermediate and smooth plains units; in addition, three morpho-stratigraphic classes of craters larger than 20 km were mapped. The geologic map reveals that this area is dominated by Intercrater Plains encompassing some almost-coeval, probably younger,
Intermediate Plains patches and interrupted to the north-west, north-east and east by the Calorian Northern Smooth Plains. This map represents the first complete geologic survey of the Victoria quadrangle at this scale, and an improvement of the existing 1:5,000,000 Mariner 10-based map, which covers only 36% of the quadrangle.

Related products

Geologic Map of the Hokusai Quadrangle (H05), Mercury

Geologic Map of the Shakespeare Quadrangle (H03), Mercury (pre-Planmap)

Geologic Map of the Kuiper Quadrangle (H06), Mercury (pre-Planmap)

Units Definition (polygon styling)

Smooth Plains, sp, 255-190-190

Northern Smooth Plains, spn, 245-162-122

Intermediate Plains, imp, 245-122-122

Intercrater Plains, icp, 137-90-68

Crater material-well preserved, c3, 255-255-115

Crater material-degraded, c2, 92-137-68

Crater material-heavily degraded, c1, 115-0-0

Crater floor material-smooth, cfs, 255-255-175

Crater floor material-hummocky, cfh, 205-170-102

Stratigraphic info

This map has an associated database of craters larger than 5 km used for basic crater frequency analysis for N(5), N(10), and N(20).

Other comments

Since the mapping scale (~1:400k) was much higher than the output scale (1:3M) the polylines of the map were not smoothed.

This map is currently being updated to fit the new controlled MESSENGER's end-of-mission basemaps.

A post-release boundary merging was done with the H03 and H05 quadrangles.

This map uses a legend also for feature labels.

Heritage usedformer Mariner 10 map by McGill and King (1983)
Link to other repositories

(crater database link)

(shapefiles database link)

Acknowledgements beyond Planmap

This research was supported by the Italian Space Agency (ASI) within the SIMBIOSYS project [ASI-INAF agreement number I/022/10/0]. Rothery was funded by the UK Space Agency (UKSA) and STFC.

Table 1: Exemplary map-wide metadata for Planmap products, implemented for a Planmap in-kind contribution (Geologic map by Galluzzi et al., 2016) see


PLANMAP will use existing datasets both as previously and externally processed, mosaicked and merged data ("Base Maps") and selected subsets of datasets, including multiple data products used individually and/or in combination. Individual datasets used or envisaged are listed in the Annex. The list and information contained is subject to updates and improvement throughout the course of the project and the mapping activities.

Base data

Planetary BodyProductResolutionAdditional info/datasetsURL

Mars HRSC MOLA Blended DEM Global

200 m/pixel
MarsMOLA463 m/pixelMEGDR/PEDR
MarsTHEMIS daytime mosaic100 m/pixelIR day
MarsTHEMIS nighttime mosaic100 m/pixeIR night

Viking MDIM2.1 Grayscale Global Mosaic

232 m/pixel
MoonLRO LROC-WAC Global Morphology Mosaic100m/pixel
MoonLROC WAC DTM GLD100118 m/pixel
MoonLRO NAC Frames and Higher Level Data Products

LRO LOLA Elevation Model (LDEM GDR)


MoonClementine UVVIS Warped Color Ratio Mosaic200 m/pixel
MoonClementine UVVIS FeO Color Binned1 km/pixel

LRO LOLA and Kaguya Terrain Camera DEM Merge

59 m/pixel

From 60N to 60S

MercuryBDR (map-projected Basemap RDR)166 m/pixelmonochrome morphology mosaic

MercuryHIE (map-projected High-Incidence angle basemap illuminated from East RDR)166 m/pixelmonochrome morphology mosaic with Sun from East
MercuryHIW (map-projected High-Incidence angle basemap illuminated from West RDR)166 m/pixelmonochrome morphology mosaic with Sun from West
MercuryLOI (map-projected LOw-Incidence basemap RDR)166 m/pixelmonochrome low-incidence angle mosaic

MercuryUSGS M10+MESSENGER500 m/pixelMariner 10 + MESSENGER flybys combined mosaic

CTX (Malin et al., 2007)

Dataset reference and name and acronymContext Camera (CTX)
OrganisationMalin Space Science Systems, Inc.
Instrument description

CTX is a linescan camera with a 5000-element linear CCD (Kodak KLI-5001G) with 7x7 micron pixels. The CTX telescope is a 350 mm f/3.25 catadioptric with two front and two rear correcting elements. Its field of view is about 5.7 degrees, covering a 30-km swath from 300 km altitude at a resolution of 6 meters/pixel. Its mechanical structure is a composite configuration in which the metering structure is graphite/cyanate-ester (GR/CE), the primary mirror is Zerodur, and the elements are mounted in Invar and titanium cells.

Dataset Description

The Mars Reconnaissance Orbiter (MRO) 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.

Spatial extent

Swath width: 30 km

Swath length: variable between 50 km and 300 km

nearly 80% of Mars covered at 2018

Spectral Rangenone
Temporal extent2006-still active
Archive contact (e.g. PDS)
Data format (raw).IMG
Data format (processed)JP2, PNG, GeoTIFF, OGR web services
Archiving URL (archive)
Preservationperformed by NASA PDS

Table X: Dataset description for the MRO CTX dataset


Dataset reference and nameHigh Resolution Stereo Camera
OrganisationDLR Institute of Planetary Research, Freie Universität Berlin
Instrument Description
Dataset Description


The High Resolution Stereo Camera (HRSC) Digital Terrain Map Reduced Data Record (DTMRDR) data products are 8-bit orthoimages for the Nadir channel and the 4 color channels and 16-bit DTMs (1 m numeric height resolution).  The orthoimages are based on the DTMs, and are thus available exclusively for areas covered by the DTMs.

The DTM and the adjusted orientation data are finally applied for orthoimage production.  The only additional pre-processing step for orthoimages consists of a histogram-based linear contrast stretch which does not affect the linear metrics of the radiometric image calibration.

Dataset Description


DTM generation is based on multi-image matching using pyramid-based least-squares correlation after pre-processing by adaptive (variable bandwidth) Gaussian low pass filtering of the stereo images to reduce the effects of image compression.  3D Point determination by least-squares forward intersection is followed by DTM grid interpolation (distance weighted averaging within a local interpolation radius).  The overall process involves automatic procedures in combination with standardized quality checks.  DTM generation uses adjusted orbit and pointing data.

Based on the high-resolution DTM result, the quality of co-registration with the Mars Orbiter Laser Altimeter (MOLA) DTM is evaluated, and final improvements to the exterior orientation data are derived.

Dataset Description


The High Resolution Stereo Camera (HRSC) Version 3 Map-Projected Reduced Data Record (REFDR3) data products are standard IMAGE objects derived from the RDRV3 data products.  Version 3 products were produced after an improved radiometric calibration.  REFDR3 products are also produced in JPEG 2000 format in addition to the typical IMG format. Footprints are also calculated for each image along with map projection.

Spatial Resolution

DTM: 100 m

RDR V3.0: 12.5 m/pixel

Spatial Extent

Swath width: 52 km

Swath length: 300 km (minimum)

Spectral Range

Panchromatic: 675±90 nm Nadir, 2 stereo, 2 photometric

Near-IR: 970±45 nm

Red: 750±20 nm

Green: 530±45 nm

Blue: 440±45 nm

Temporal Extent2003-present
Upstream contact (e.g. PDS)


Data Format (raw).IMG (VICAR)
Data Format (processed)JP2, PNG, GeoTIFF, OGR web services
Access URL (archive)
PreservationPerformed by ESA PSA
AcknowledgementsESA planetary Science Archive, HRSC Principal Investigator(s): G. Neukum (Freie Universitaet, Berlin, Germany),

Table X: Dataset description for the MEX HRSC dataset

Hirise (McEwen et al., 2007)

Dataset reference and nameHigh Resolution Imaging Science Experiment

OrganisationUniversity of Arizona

Instrument Description

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 imaging Mars at a resolution of ~0.25 m/pixel. Color information can be derived from RED (covering the whole swath) Blue-Green and NIR channels. HiRISE is designed to take stereo couples that can be used to reconstruct with photogrammetry the topography of Mars at 1m of horizontal resolution and tens of centimeters of vertical accuracy.

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 (in addition, ODE presents the Anaglyphs as a fourth data type - see below). EDRs are raw images from the spacecraft. RDRs are combined and processed images based on several EDRs. DTMs are sets of digital elevation models along with the ortho images used to create them.

Dataset Description


HiRISE reduced data records without embedded map projection

The High Resolution Imaging Science Experiment (HiRISE) Reduced Data Record (RDR) products are combined and processed radiometrically-corrected, geometrically-mapped images based on several EDRs at nominal resolution of 30 cm/pixel from 300 km altitude.  Due to a mid-2008 change in RDR format to include embedded map projection information within the JPEG 2000 files, the majority of RDR products are Version 1.1.

Dataset Description


HiRISE Reduced Data Records with embedded map projection


The High Resolution Imaging Science Experiment (HiRISE) Experiment Data Record (EDR) products are the permanent record of the HiRISE raw image data collection.  An EDR contains unprocessed image data (except as noted below), ancillary engineering data, and information about the instrument commanding used to acquire the image.  An EDR image has the inherent properties of raw and unprocessed data.  Data gaps may exist in an EDR primarily due to telemetry communication problems between Mars and Earth.  The image pixel values are raw counts not yet radiometrically corrected. No geometric processing has been applied to the data to correct for optical distortion or view geometry.

The format is nearly identical to the original from of the data stream as produced by the instrument.  Some processing was applied to the data for (1) FELICS decompressing an image (if the data were optionally compressed on the spacecraft), (2) identifying and filling gaps with “no-data” values, (3) mirroring the pixel order of an image line for data read out in reverse order, and (4) adding a PDS label to the beginning of the file.

Dataset Description


HiRISE images are usually 0.25 - 0.5 m/pixel, so the post spacing is 1-2 m with vertical precision in the tens of centimeters. 

  • The DTM in standard PDS image object (.IMG) format with an embedded label 
  • Orthoimages at the same resolution as the DTM, in JPEG2000 format with detached label 
  • Orthoimages at the resolution of the original image, in JPEG2000 format with detached label


Spatial Resolution0.25 m/pixel

Spatial Extent

local, targeted

Swath width(Blue-Green-NIR): 1.2 km

Swath width(RED): 6 km

Swath length: 12 km

Spectral Range

Blue-Green (BG): 400 to 600 nm
Red: 550 to 850 nm
Near infra-red (NIR): 800 to 1000 nm

Temporal Extent2006-present

Upstream contact (e.g. PDS)


Data Format (raw).IMG

Data Format (processed).JP2

Access URL (archive)

PreservationPerformed by NASA PDS

AcknowledgementsNASA/JPL/University of Arizona, A. McEwen (UoA)

Table X: Dataset description for the MRO HiRISE daset


CaSSIS (Thomas et al., 2017)

Dataset reference and name and acronymCaSSIS - Colour and Stereo Surface Imaging System
OrganisationUniversity of Bern
Instrument description

CaSSIS will characterise sites that have been identified as potential sources of trace gases and investigate dynamic surface processes – for example, sublimation, erosional processes and volcanism – which may contribute to the atmospheric gas inventory. The instrument will also be used to certify potential landing sites by characterising local slopes, rocks and other possible hazards by acquiring stereoscopic images. The rotation mechanism will be able to turn the entire telescope system by 180° while its support structure remains fixed. This rotation system will also enable the camera to acquire stereo images with only one telescope and focal plane assembly. A stereo image pair will be acquired by first rotating the telescope to point 10° ahead of the spacecraft track to acquire the first image, then rotating it 180° to point 10° behind for the second stereo image. Optimal correlation of the stereo signals will be ensured as there will be identical illumination conditions every time a stereo image pair is acquired. The imager will cover an eight-kilometre-wide swathe of the planet's surface in four different wavelength ranges.

Dataset Description

4 color (PAN, IR, RED, BLUE) with stereo acquisition along track.

Stereo angle from 400 km altitude 22.39°

DTM: n/a, available in late 2018

StandardsPDS4 to be implemented
Spatial Resolution4.62 m/pixel
Spatial extent

Swath width: 7-9 km

Swath length: variable 40-50 km

Spectral Range

Pan: 675 nm / 250 nm

Blue-Green: 485 nm / 165 nm

Red: 840 nm / 100 nm

IR: 985 nm / 220 nm

Temporal extentNominal mission: 2018-still active
Archive contact (e.g. PDS)n/a
Data format (raw).dat, .xml
Data format (processed).cub, JP2, PNG, GeoTIFF, OGR web services
Archiving URL (archive)n/a
PreservationUniversity of Bern, to be continued by PSA/PDS
AcknowlegementsProf. Nicolas Thomas, University of Bern, Dr. Gabriele Cremonese, INAF OaPD


Dataset reference and nameObservatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité (OMEGA)
OrganisationInstitut d’Astrophysique Spatiale, Orsay, France
Instrument Description

OMEGA is a mapping spectrometer, with co-aligned channels working in the 0.38-1.05 μm visible and near-IR range (VNIR channel) and in the 0.93-5.1 μm short wavelength IR range (SWIR channel) in 352 contiguous spectral elements (spectels). The signal-to-noise ratio(SNR) is >100 over the whole spectral range for observations obtained in nadir mode and considering low solar zenith angles. Due to the MEx spacecraft elliptic orbit, the scan widths in each orbit are changed (16, 32, 64, 128 pixels) accordingly to the variation of the observing distance. The spatial resolution of OMEGA is in the range 0.3-4-5 km/pixel . The SWIR detector (covering the 1-2.5 µm diagnostic wavelength range) is not functioning any more since 2010.

Dataset Description

The data products constitute three-dimensional ‘image-cubes’, with two spatial and one spectral dimensions. OMEGA provides global coverage at medium-resolution (2-5 km) for altitudes from 1500 km to 4000 km, and high-resolution (< 350 m) spectral images of selected areas, amounting to a few percent of the surface, when observed from near-periapsis (< 300 km altitude).

Spatial Extent and Resolution

Images can vary between 16, 32, 64, 128 pixels of swath depending on the distance. On the ground images are circa from 5-7 km X 3000 km (with 360m/px) up to 300-600 km X 3000 km (with 5km/px).

Spectral Range and Resolution

0.35-5.1um divided into three range: VNIR with a spectral sampling ranging from 7 nm between 0.38 and 1.05 um; SWIR-C with 14 nm between 0.93 and 2.73 um; and SWIR-L with 20 nm between 2.55–5.1 um.

Temporal Extent

Nominal Mission (19 Feb 2003 - 19 Jan 2006; cruise through orbit 2595)
Extended Mission 1 (22 Jan 2006 - 23 Oct 2007; orbits 2607-4890)
Extended Mission 2 (4 Nov 2007 - 3 Jan 2010; orbits 4931-7697)
Extended Mission 3 (4 Jan 2010 - 19 Oct 2012; orbits 7701-11193)
Extended Mission 4 (20 Oct 2012 - 11 Jan 2015)
Extended Mission 5 (14 Jan 2015 - 9 Jan 2017)
Extended Mission 6 (10 Jan 2017 - 3 Jun 2017)

Upstream contact (e.g. PDS)


High level products

The OMEGA Mars Global Maps data products are primarily available in PDS format in the DATA directory of this data set. Raster maps are formatted using the PDS IMAGE object, and vector maps are formatted using the PDS SPREADSHEET object.

NIR Albedo Map

Ferric Oxide Map

Dust Map

Hydrated Mineral Map

Olivine Maps (3 maps)

Pyroxene Map

Data Format (raw)

The OMEGA files extensions are .QUB for the data (level 1B in the "cube" PDS format) and .NAV for the geometry.

Files are named from the corresponding OMEGA observation: ORBNNNN_S where NNNN is the orbit number (format I4.4) and S is the rank of the OMEGA observation on that orbit (starting with 0).

Data Format (processed)

for data: .sav, .txt

for images: .png, .tiff/.geotiff

Access URL (archive)

PreservationPerformed by ESA PSA
AcknowledgementsESA planetary Science Archive, OMEGA PI Dr. Jean-Pierre Bibring, Institut d'Astrophysique Spatiale, Orsay, France


Dataset reference and nameShallow Subsurface Radar
OrganisationASI, NASA
Instrument DescriptionThe first hundred meters of the subsurface are investigated with a vertical resolution of about 20 metres, horizontal at about one hundred metres in trajectory, while perpendicularly the resolution is in the order of a kilometre depending on subsurface characteristics and local surfaces. The radar instrument points to the nadir with functioning and impulses on two modalities of radar and altimeter. In order to isolate, the reflectors of the subsurface use the synthetic aperture technique. The instrument consists of an antenna and an electronic system working at a wavelength range centred at MHz +/- 5 MHz This configuration enables the analysis of dielectric properties in the subsurface, thereby maintaining low clutter at the surface. The frequencies selected can penetrate the ionosphere. The total cycle of transmission and reception of each impulse is a few milliseconds
Dataset Description

Raw Data Products - EDR (SHARAD Operations, Italy)


The Shallow Radar (SHARAD) Experiment Data Record (EDR) for SHARAD is a data product produced by the Italian SHARAD team that consists of the instrument telemetry correlated with the auxiliary information needed to locate observations in space and time and to process data further.  Apart from editing of data to remove duplicates and transmission errors, no processing is applied to the scientific data of the instrument.

Each Data Product contains data from one or more data blocks collected continuously using the same operation mode, instrument status and on-board processing scheme; that is, using a single Operation Sequence Table (OST) line.  The content of each SHARAD data product is highly variable in terms of number of data blocks, and depends on how operations for the instrument were planned during a given data collection period.  The natural organization for data blocks within a Data Product is a table, in which each line contains data from a single data block, and each column contains the value of a single parameter or time sample across different data blocks.

Each Data Product consists of three files:

1) A binary file containing the scientific telemetry of the instrument.  This is a sequence of echoes, each of which is preceded by a header containing information on the collection and on-board processing of the data.  This file is called the Science Telemetry file.

2) A binary table containing geometric quantities generated on-ground from spacecraft navigation data, parameters extracted from instrument and spacecraft housekeeping telemetry, and flags describing the completeness and usability of the associated scientific telemetry.  This file is called the Auxiliary Data file and contains one record for every data block in the Science Telemetry file.

3) A detached ASCII label file describing the content of the data product.  The label is written according to standards defined by the Planetary Data System (PDS), and lists parameters describing both the observation in which data were acquired and the structure of the files in which data are stored.

Dataset Description

Derived Data Products - RDR (SHARAD Operations, Italy)


The Shallow Radar (SHARAD) Reduced Data Record (RDR) for SHARAD is a data product produced by the Italian SHARAD team that consists of received echoes that have been Doppler filtered, range compressed, and converted to complex voltages, correlated with the auxiliary information needed to locate observations in space and time and to process data further.  Data users must be aware that processed echoes may contain artifacts due to off-nadir surface reflections, the so-called clutter, reaching the radar after nadir surface echoes, and thus appearing as subsurface reflections.

Each Data Product is the result of the processing of all echoes acquired continuously in time using the same operation mode, instrument status and on-board processing scheme.  There is one RDR data product for every Experiment Data Record (EDR) data product acquired in subsurface sounding mode, which in fact constitutes the input for the RDR product generation.  Each processed radar observation in an RDR data product is the result of range and azimuth processing of a variable number of raw echoes.  The natural organization for processed echoes within a Data Product is a table, in which each line contains data from a single processed echo, and each column contains the value of a single parameter or time sample across different processed echoes.

Each Data Product consists of two files:

1) A binary file containing the scientific data of the instrument:  a sequence of processed echoes, each of which is preceded by a header containing information on the instrument setting and on-board processing of the data, and followed by parameters characterizing the ground processing of the echoes, by geometric quantities generated on-ground from spacecraft navigation data, and by parameters extracted from instrument housekeeping telemetry.

2) A detached ASCII PDS label file describing the content of the data product.

Dataset Description

Derived Data Products (Radargrams) (SHARAD Science Team, U.S.)


The Shallow Radar (SHARAD) Reduced Data Record of Radar backscatter power (USRDR) is a data product produced by the U.S. SHARAD team.  The image product, the radargram, is a backscatter power presented with along-track distance in the horizontal dimension and round-trip time delay along the vertical axis.

The U.S. radargram processing uses a uniform amplitude model for the frequency components of the SHARAD linear frequency-modulated chirp signal.  This leads to asymmetric offset of the characteristic transform sidelobes, with greater sidelobe amplitude on the downrange (greater delay) side of any echo.  This approach preserves a two-fold oversampling (i.e., 3600 complex samples from 3600 real samples) of the signal after range compression, which allows for flexibility in later interpolation.  Ionospheric distortion is compensated using a model for the frequency dependence of the phase errors.  The resulting correction term is approximately linear with total electron content (TEC), and thus with the change in delay time for signals from the surface and subsurface.  The image-restoring and range corrections are applied where the solar zenith angle (SZA) is less than 100°.  A Hann window function is applied to the frequency-domain data prior to the inverse Fourier transform to reduce sidelobe levels in the range-compressed echo.

Two basic parameters define the processing of SHARAD data.  The first is the coherence time or aperture length, TC (in seconds).  The frequency resolution (in Hz) of the resulting Doppler spectrum is 1/TC, independent of the time spacing between the pulses that make up the synthetic aperture.  The degree of pre-summing, which reduces the pulse repetition frequency (PRF) from the initial value of 700.28 pulses per second, affects only the Doppler frequency bandwidth (in Hz) of the Doppler spectrum, which is given by 1/PRF.  The second parameter specifies the Doppler frequency bandwidth (in Hz), B, of echoes about the center of the Doppler spectrum to be included in the radar backscatter mapping.  If this frequency width is less than 1/TC, the output map will have only one sample for each output pixel location.  This is a one-look radar image.  If the frequency width is larger than 1/TC, more than one Doppler resolution cell will be averaged, yielding a multi-look image.

Each 32-bit floating-point format radargram file is accompanied by a TIFF image that logarithmically scales the backscattered power over an 8-bit range corresponding to -3 dB to +32 dB with respect to the noise background (i.e., each DN step is about 0.137 dB).  The noise-scaling factor was determined from the average behavior over the period between orbits 7500 and 32999.  Tracks collected before about orbit 7200 have a slightly higher (about 1.4 dB) background noise, so their TIFF radargram products will appear slightly brighter due to the use of the lower scaling factor.  A reduced-quality JPEG version of each TIFF is provided for browsing the archive.

The Shallow Radar (SHARAD) Geographic, geometric, and ionospheric properties (USGEOM) data file accompanies each U.S. Reduced Data Record of Radar backscatter power (USRDR).  The ASCII-format table file contains location information for each radargram column, the spacecraft and surface radius values required to change the reference planetary shape, and the phase correction value related to the correction of ionospheric distortion and delay.  The coordinate system of planetocentric, with longitude positive toward the east.  Radius values tabulated in the GEOM files are interpolated using a polynomial fit between the along-track elapsed time and data from Mars Orbiter Laser Altimeter (MOLA).  The topographic information for the polynomial fit is drawn from the MOLA 128-ppd (pixels per degree) areoid gridded database for non-polar tracks, and from the 512-ppd gridded dataset for tracks that cross the polar terrain.

Spatial ResolutionVertical resolution 20 m

Spatial Extent

linear, along track.

Spectral Rangenone
Temporal Extent


Upstream contact (e.g. PDS)


Data Format (raw).dat, .lbl
Data Format (processed)

.img, .lbl, .tab

Access URL (archive)

PreservationPerformed by NASA, PDS
AcknowledgementsASI, NASA, Principal Investigator Dr. Roberto Seu of the INFOCOM Department of the Università “La Sapienza” of Rome.


Dataset reference and name Compact Reconnaissance Imaging Spectrometer for Mars (CRISM)

OrganisationNASA - The Johns Hopkins University/Applied Physics Lab

Instrument Description

CRISM is a hyperspectral imager covering wavelengths from 0.36 to 3.92 microns. The SNR is .... The MRO will operate from a sun-synchronous, near- circular (255x320 km altitude), near-polar orbit with a mean local solar time of 3 PM. ...

Dataset Description

The data products consist in image cubes. In targeted mode (Gimbaled, Hyperspectral Modes), CRISM acquires hyperspectral images from circa 0.4 to 4.0 mm in 544 channels (VNIR 107+ IR 438) at a spatial resolution up to 18 meters per pixel; whereas in global mode (pushbroom modes) images have different spectral sampling in the VNIR (from 19 to 107 channel) and IR (from 0 to 438 channel) with spatial resolution between 100-200 m .

This datasets are defined as:

1) Gimbaled: Full Resolution (FRT); Half resolution short (HRS); Half resolution long (HRL); Full resolution short (FRS); Along-track oversampled (ATO); Along-track undersampled (ATU)

2) Pushbroom: Multispectral Window (MSW); Multispectral VNIR (MSV); Multispectral Survey (MSP); Hyperspectral Mapping (HSP); Hypersepctral VNIR (HSV); Tracking Optical Depth (TOD); Flat Field Calibration (FFC)


Spatial Extent and Resolution

Full Resolution (FRT): Spatial pixels unbinned for target – 18 m/pixel @ 300 km,  

Half resolution short (HRS): Spatial pixels 2x binned for target – 36 m/pixel @ 300 km, same swath length as above

Half resolution long (HRL): Spatial pixels 2x binned for target – 36 m/pixel @ 300 km, twice swath length as above

Full resolution short (FRS): Spatial pixels unbinned for target – 18 m/pixel @ 300 km; half swath length as above

Along-track oversampled (ATO): Spatial pixels unbinned for target – 18 m/pixel cross-track, up to ~3 m/pixel downtrack, requires special processing for increased resolution; half swath length as above

Along-track undersampled (ATU): Spatial pixels unbinned for target – 18 m/pixel cross-track, 36 m/pixel downtrack; half swath length as above

Spectral Range and Resolution

0.36 to 3.92 microns at 6.55 nanometers/channel

Temporal Extent


EDR / CDR Volume Coverage
MROCR_0001 Sept. 27, 2006 - Dec. 31, 2007
MROCR_0002 Jan. 1, 2008 - Aug. 8, 2008
MROCR_0003 Aug. 9, 2008 - Aug. 8, 2010
MROCR_0004 Aug. 9, 2010 - Aug. 8, 2011
MROCR_0005 Aug. 11, 2011 - Aug. 3, 2012
MROCR_0006 Sept. 14, 2012 - Aug. 8, 2013
MROCR_0007 Aug. 9, 2013 - Aug. 8, 2014
MROCR_0008 Aug. 9, 2014 - Nov. 8, 2015
MROCR_0009 Nov. 9, 2015 - Nov. 8, 2016
MROCR_0010 Nov. 9, 2016 - Nov. 8, 2017
MROCR_0011 Nov. 9, 2017 - Feb. 8, 2018

Upstream contact (e.g. PDS)


High level products


Data Format (raw) and derived

Crism file extensions are:

Experiment Data Record (EDR) Raw data from the telemetry stream rearranged but unmodified except for lossless decompression.

Calibration Data Record (CDR) Derived values needed to convert a scene-viewing EDR into units of radiance.

Whereas derived CRISM files are:

Derived Data Record (DDR) A companion file for each EDR or TRDR pointed at Mars's surface that contains physical parameters such as latitude, longitude, and incidence, emission, and phase angle. Used for map projection, photometric correction, and to locate correction information in an ADR.

Limb Data Record (LDR) A companion file for each EDR or TRDR pointed at Mars's limb that contains physical parameters such as latitude, longitude, and incidence, emission, and phase angle. Used to locate measurement tangent relative to the surface and model the radiance.

Targeted Reduced Data Record (TRDR) Image data from an EDR converted to units of radiance or I/F using CDRs. A TRDR also contains a set of derived spectral parameters (summary products) that provide an overview of the data set.

Ancillary Data Record (ADR) Reference information used to correct scene measurements for photometric, thermal emission, or atmospheric effects.

Multispectral Reduced Data Record (MRDR) One of many tiles that make up a global mosaic, an MRDR contains map-projected data in units of radiance (extracted from TRDRs), plus I/F, summary products, and the DDR data used to generate them.

Targeted Empirical Record (TER) A spatially reconciled, full spectral range I/F targeted observation central scan image cube in the IR (L-detector) sensor space that has been corrected for geometric, photometric, atmospheric, and instrumental effects.

Map-Projected Targeted Reduced Data Record (MTRDR) Similar in concept to an MRDR, MTRDRs are map-projected versions of TER data products.

Data Format (processed)

for data: .sav, .txt

for images: .png, .tiff/.geotiff

Access URL (archive)

PreservationPerformed by NASA, PDS

AcknowledgementsCRISM Principal Investigator: Scott Murchie, The Johns Hopkins University/Applied Physics Lab


Dataset reference and name and acronymMars Advanced Radar for Subsurface and Ionosphere Sounding
OrganisationUniversità La Sapienza, Roma
Instrument description

The 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.

Dataset Description

Nominal Mission


Nominal Mission


For more information about the dataset

Spatial extent

2-3 km in depth

Spectral Rangenone
Temporal extent2003-present

Archive contact (e.g. PDS)
Data format (raw).dat, .lbl
Data format (processed)
Archiving URL (archive)

MARSIS Principal Investigator: Roberto Orosei, MARSIS Principal Investigator from Istituto di Astrofisica e Planetologia Spaziali, Bologna, Italy.

Formerly Prof. Giovanni Picardi, Universita di Roma 'La Sapienza', Rome, Italy angelo.rossi


See here for labels and format etc.:

LROC NAC (Chin et al., 2007; Robinson et al., 2010)

Dataset reference and name and acronymLROC NAC
OrganisationNASA PDS
Instrument description

The Lunar Reconnaissance Orbiter Camera (LROC) has been designed to address two of the measurement requirements:
Landing site certification
Polar illumination
LROC acquires images to assess meter and smaller scale features to facilitate safety analysis for potential lunar landing sites near polar resources and elsewhere on the Moon. Synoptic 100 m/pixel imaging of the poles during every orbit for a year will unambiguously identify regions of permanent shadow and permanent or near-permanent illumination.

Dataset Description

The Lunar Reconnaissance Orbiter Camera (LROC) Experiment Data Record Narrow Angle Camera (EDRNAC) data product is a NAC panchromatic image corresponding to a single observation (either full resolution or summed), with Digital Number (DN) counts in 8-bit format, companded from 12-bit in the instrument.  The image data consists of one series of contiguous lines up to 52,224 lines with 5,000 samples in full resolution mode, or 104,448 lines with 5,000 samples in 2x cross-track summation mode.

The image file is composed first of the even pixels from each line (with a 20 byte CTX heritage header every 1 MB) and padded to a 1 MB boundary, followed by the odd pixels in the same style.  The EDR file generation process extracts the odd and even pixels, interleaving them to reconstruct original scan lines.  If compression was enabled at image acquisition, the data stream is first de-compressed before the interleaving is performed.  Information from the meta-file, housekeeping, and the SOC database are combined to generate the PDS label with the binary data to compose the EDR file.

Specifications for the right and left NACs are in the table below.  The NAC-L is off-pointed ~2.85° from the NAC-R so that the footprints of the two images overlap ~130 pixels.

Spatial extent

0.5 m/pixel scale panchromatic images over a 5 km swath and a wide-angle camera component (WAC) to provide images at a scale of 75 m/pixel in five visible bandpasses and 400 m/pixel (source LROC RDR SIS)

Spectral Range
Temporal extent
Archive contact (e.g. PDS)
Data format (raw).IMG
Data format (processed)JP2, PNG, GeoTIFF, OGR web services
Archiving URL (archive)
Preservationperformed by NASA PDS

M3  (Pieters et al., 2009)

Dataset reference and name and acronymMoon Mineralogy Mapper
Instrument description

M3 is a broad spectral range imaging spectrometer, measuring from 430 to 3000 nm with 10 nm spectral sampling (### channels), with one detector, through a 24 degree field of view with 0.7 milliradian spatial sampling. It was designed to measurecompositionallydiagnosticspectralabsorptionfeaturesfromawidevariety ofknownandpossiblelunarmaterials. The instrument's SNR was greater than 400 for the specified equatorial reference radiance and greater than 100 for the polar reference radiance. Chandrayaan‐1 had a nominal 100 km inertially fixed polar orbit, but from the 19th of May 2009, for mission safety, the orbit of Chandrayaan‐1 was raised from 100 km to 200 km.

Dataset DescriptionDataset was defined with two instrument measurement modes, defined as “Target Mode” and "Global Mode". Target Mode is characterized by a full resolution with 260 spectral detector elements for every along‐track sample with a nominal spatial sampling of 70 m. Global Mode was defined to collect rapid full lunar coverage at reduced spatial (140 m/pixel) and spectral sampling (86 spectral channels). 825 nominally illuminated Global Mode and 79 Target Mode images were acquired. 336 contiguous Global Mode images strips provide nearly full coverage of the lunar surface. The acquired M3 measurements provide 95%complete Global Mode coverage of the Moon.
Spatial extent and Resolution

40 km swath and 70 m spatial sampling from the nominal 100 km orbit

Spectral Range and Resolution430 to 3000 nm with 10 nm of spectral sampling
Temporal extent

OP1A   Nov  18 2018  -­‐  Jan  24 2019   119   100  km  extended commissioning  
OP1B     Jan  25  -­‐  Feb  14   247   100  km   operational,  high  solar  zenith  angles  
OP2A   Apr  15  -­‐  Apr  27   197   100  km   operational,  high  solar  zenith  angles  
OP2B   May  13    -­‐  May  16   20   100  km S/C  emergency,  orbit  raised  
OP2C   May  20  -­‐  Aug  16   375   200  km   operational,  variable  conditions

Archive contact (e.g. PDS)
Data format (raw).IMG
Data format (processed)

for data: .sav, .txt

for images: JP2, PNG, GeoTIFF, OGR web services

Archiving URL (archive)
Preservationperformed by NASA PDS

SELENE (Kaguya) Terrain Camera 

Dataset reference and name and acronym
Instrument description

Dataset Description
Spatial extent

Spectral Range
Temporal extent
Archive contact (e.g. PDS)
Data format (raw)
Data format (processed)
Archiving URL (archive)
Preservationperformed by JAXA


MDIS-NAC/WAC (Hawkins, S.E. III et al., 2007, Space Sci. Rev.)

Dataset reference and name and acronymMDIS - MESSENGER Mercury Dual Imaging System

NASA/Johns Hopkins University Applied Physics Laboratory

Instrument description

MDIS consists of a monochrome narrow-angle camera (NAC) and a multispectral wide-angle camera (WAC). The NAC has a single medium-band filter centered at 747.7 nm to match to the corresponding WAC filter for monochrome imaging. The WAC has a 12-position filter wheel (FW) provides color imaging over the spectral range of the CCD detector. Eleven spectral filters spanning the range 395-1,040 nm are defined to cover wavelengths diagnostic of different potential surface materials. The WAC's 10.5° x 10.5° FOV is sufficient that overlap occurs between nadir-pointed image strips taken on adjacent orbits, even at northern mid-latitudes where low altitudes occur. The NAC's 1.5° FOV is sufficiently narrow that 375 m/pixel sampling is attained at 15,000 km altitude. MESSENGER was placed in a highly eccentric orbit with a periapsis altitude of 200 km, a periapsis latitude of ~60° and an apoapsis altitude of 15,200 km. The orbit has a 12-hour period, is inclined 80° to the planet's equatorial plane, and is not Sun synchronous.

Dataset Description

MDIS dataset consists of single wavelength images at variable scales and with variable filters combination. They provided global coverage on B/W, three colors, five colors or eight colors of Mercury surfaces. Targeted region can be characterized by very high spatial resolution from few tens of meters for NAC filter up to few hundred of meters for 8 color image.

Spatial Extent and Resolution

NAC: ~5 m/px at 200-km altitude, 380 m/px at 15,200-km altitude

WAC: ~ 36 m/px at 200-km altitude, 2720 m/px at 15,200-km altitude

Spectral Range and resolution

NAC: single medium-band filter (721–770 nm) centered at 747.7 nm, WAC: 395–1040 nm in 12 filters

Filter numberFilter letter

System wavelength

measured at -26°C (nm)

System bandwidth

measured at -26°C (nm)


Temporal extent

Mercury flyby 1 → 14 January 2008

Mercury flyby 2 → 6 October 2008

Mercury flyby 3 → 29 September 2009

Orbital phase → March 2011 - April 2015

Archive contact (e.g. PDS)


High Level Products

Mercury Messenger Global Mosaic 2010

This mosaic represents the best geodetic map of Mercury's surface as of 2010.

Mercury MESSENGER MDIS Basemap Enhanced Color Global Mosaic 665m (64ppd)

This view uses a global mosaic with 430, 750, and 1000 nm bands and places the second principal component, the first principal component, and the 430/1000 ratio in the red, green, and blue channels respectively.

Mercury MESSENGER MDIS Global Basemap BDR 166m (256ppd)

The Map Projected Basemap RDR (BDR) data set consists of a global monochrome map of reflectance at a resolution of 256 pixels per degree (~166 m/px).

Mercury MESSENGER MDIS Basemap MD3 Color Global Mosaic 665m (64ppd)

The mosaic shows Mercury's colors as viewed by placing images from MESSENGER's 1000 nm, 750 nm, and 430 nm narrow-band filters in the red, green, and blue channel respectively.

Mercury MESSENGER MDIS Basemap LOI Global Mosaic 166m (256ppd)

The Map Projected Low-Incidence Angle Basemap RDR (LOI) data set consists of a global monochrome map of reflectance at a resolution of 256 pixels per degree (~166 m/px).

Mercury MESSENGER MDIS Color Global Mosaic 665m v3

The color mosaic is comprised of photometrically corrected I/F (radiance factor) for 3 narrow-band color filters of the Mercury Dual Imaging System (MDIS) Wide Angle Camera (WAC), placing the 1000-nm, 750-nm, and 430-nm filters in the red, green, and blue channels, respectively.

Mercury MESSENGER Global DEM 665m (64ppd) v2 Oct. 2016

The map is a colorized shaded-relief of the original digital elevation model (DEM)

Mercury MESSENGER Global Colorized Shade 2km

Global DEM of Mercury from a least-squares bundle adjustment (jigsaw in ISIS3 [Becker 2016]) of common features, measured as tie point coordinates in overlapping NAC and WAC-G filter images.

MESSENGER Global Mosaic

8-color (MDR) 64 ppd (all backplanes)

5-color (MP5) 128 ppd (all backplanes)

3-color (MP3) 128 ppd (all backplanes)

Moderate incidence angle (BDR) 256 ppd (image plane only), 43 ppd (all backplanes)

Low incidence angle (LOI) 256 ppd (image plane only), 43 ppd (all backplanes)

East illumination (HIE) 256 ppd (image plane only), 43 ppd (all backplanes)

West illumination (HIW) 256 ppd (image plane only), 43 ppd (all backplanes)

Data format (raw)

MDIS file extensions are:

Experiment Data Record (EDR)

Calibrated Data Record (CDR)

Derived Data Record (DDR)

Map Projected Multispectral RDR (MDR)

and the raw format is:


Data format (processed)For images: .jpg, .PNG, For data: .GeoTiff, .cub, .dat
Archiving URL (archive)
PreservationPerformed by NASA PDS

Mapping products - Standard


Compositional basemaps (see D4.2-public) are specific data dependiing on the target body. Those used for RGB display of different spectral index products are exemplified in Table 2 and are used as basemaps for geological maps integrated with spectral and compositional information.

Index NameParameterChannelFormulationRationale on Mercury
R750Reflectance at 750 nm (Fig. 1)MDIS-WACR750 nmReflectance variations. High values →  brigth fresh material, pyroclastic deposits, northern smooth plains. Low values →  dark terrain. Intermediate  values →  intercrater and intermediate plains.
RGB “False Color Mosaic”R: R996 nm, G: R750nm, B: R430 nm (Fig. 2)MDIS-WACR: R996 nm, G: R750nm, B: R430 nmColor variations. Red → reflectance at longer wavelength. Green → reflectance at intermediate  wavelength. Blue → reflectance at shorter wavelength.
PC1PCA first channel (Fig. 3)MDIS-WACPC1reflectance variation. High values →  brigth fresh material, pyroclastic deposits, northern smooth plains. Low values →  dark terrain. Intermediate  values →  intercrater and intermediate plains.
PC2PCA second channel (Fig. 4)MDIS-WACPC2Spectral variabilities not due to reflectance. High values: → pyroclastic deposits, northern smooth plains. Low values → dark material, smooth plains (western area), Intercraterplains and intermediate plains (western area).
RGB “Enhanced Color Mosaic”R: PC2, G: PC1, B: 430/996nm  (Fig. 5)MDIS-WACR: PC2, G: PC1, B: 430/996nmIdentification of the main terrain units. Orange region → pyroclastic deposits, northern smooth plains, volcanic material. Light blue: crater rays, ejecta, fresh material. Dark blue → dark and very dark material.
RGB “Clementine-like Color Mosaic“R: R748 nm/R430 nm, G: R748 nm/R828 nm, B: R430 nm/R748 nm (Fig. 6)MDIS-WACR: R748 nm/R430 nm, G: R748 nm/R828 nm, B: R430 nm/R748 nmMaturity, mafic or glassic components, secondary elements locally concentrated. Yellow →  high-reflectance material and blue areas indicate low-reflectance material and crater rays. Green →  higher intermediate slope. Red → steeper visible slopes relative to bluer areas. Orange/red → steepest visible slopes.
S430_996Spectral slope between 430 and 996 nm (Fig. 7)MDIS-WAC(R996−R430)/((996−430)R433)Maturity, compositional variation, grain size. Low values → fresh terrains, dark terrain. High values → older terrains,   volcanic  materials, space weathering.
S430_558Spectral slope between 430 and 558 nm (Fig. 8)MDIS-WAC(R558−R430)/((558−430)R430)Opaque mineralogical phases. Low values → possible presence or opaque phases. High values → pyroclastic deposits and northern smooth plains.
 S748_996Spectral slope between 748 and 996 nm (Fig. 9)MDIS-WAC(R996−R748)/((996−748)R748)1 µm band absorption. Low values → possible absorption at 1µm
RGB “Spectral Slopes”R: S430_996, G: S748_996, B: S430_996  (Fig. 10)MDIS-WACR: S430_996, G: S748_996, B: S430_996

Spectral slope variations.

Table 2. Summary of delivered spectral indicies for the Hokusai Quadrangle.


The numerical representation of three dimensional surfaces can be straightforwardly achieved by storing a list of vertices, faces and edges (see e.g. When it comes to geological models the relationship occurring between different surfaces must indeed be specified in an explicit way by grouping one or more surfaces in a geologically meaningful object (e.g. a horizon, a fault, an unconformity). This kind of representation requires dedicated software and formats. Although there have been recent efforts (see Pellerin, 2017, which also constitutes a good introduction to the numerical representation of geological models) to create an unified library for the definition of 3d geological elements, there is still no widely-accepted representation standard, which must be evaluated case by case, depending on the specific needs. The following table illustrates the expected outputs of 3D geological modeling software and its usage depending on the context. Each row (namely native/exchange/pure3d) represents a decreasing level of compexity and completeness of a 3D geological model as it is reduced to different numerical representations.

Product completeness level

DefinitionMain expected usageProCons


gocad/3dmove/leapfrog (or any other 3D geomodeling software packages) in native formats (projects)


Perfect during model development and short term preservation.

Bad for archiving, programmatic access and injection in other WPs, because it is strongly tied to the specific software


Formats maintaining specific geological information about the surfaces and volumetric meshes. E.g. RINGMesh-supported formats or any other geological-aware data exchange format that might be suitable for a specific software-to-software exchange task


The format can be accessed by the software packages of interest and maintain most of the geological information.

The formats might still not be the perfect solution for long-term preservation. Commercial packages can drop the retro-compatibility with some formats.


Pure mesh representation (e.g. triangular meshes) without any predefined way of storing the geological meaning of the surfaces/volumes.



Perfect for long term preservation. Mainly ascii based formats and well-establishes IO libraries for accessing the files

These formats leave out information that is instead present in native and exchange level representations. Some of the information might be provided through metadata.

These different data representations are connected with a sort of data reduction pipeline going from high-to-low completeness. All the levels will be stored once generated although no level is mandatory. E.g. "native" level data can be transformed to "pure3d" level data for composing a deliverable without obtaining "exchange" level data. In the other hand "pure3d" level data might be directly generated for simple task where complex geomodeling software packages are not needed (via ad-hoc modeling strategies).


Base formats depending on data type

Dataset typeFormatCommon extensions



GeoTiff with appropriate type and signedness (compressed or not).gtiff, .tif, .tiffImagery, possibly multi-band imagery and Digital Terrain Models
jpeg2000 (lossy or lossless).jp2 .jk2Imagery for basemaps/mosaic for which higher compression rates is desirable
Portable network graphics.pngImagery for web publication and GIS, imagery intended only for visualization (i.e. grayscale/colour mosaics)
ASCII Gridded formats supported by gdal (arc/Info, GRASS, etc)any [e.g. .txt, .grid, etc ]alternative to geotiff for Digital Terrain Modelsgeotiff is still preferable (e.g. no round-off errors)
World (georeferencing) files.twf, .pwf, .jwf (or similar)Gereferencing information for raster dataset which is coupled with each raster file

Geopackage (OGC)



.shp (.dbf, .shx , .sbn, .prj)

All mapping products in vector format

Geographical markups: JSON (GeoJSON)/XML (GML).json, .xmlGeoreferenced products shareable on the web, WFS-served dataset

Relational DB (PostgreSql + PostGIS / SpatiaLite)----Dataset meant to be served by Web Feature Services [WFSs]Internal use only

Styled Layer Descriptors.xmlXML files describing the styles to be used when displaying vector layers
3DStanford Triangle Format, Wavefront OBJ, Stereolithography  and comparable.ply, .obj, .stl

Three dimensional meshes. Geological meaning must be provided by metadata.

Neutral file formats must be preferred.

Might be equipped with texture files (i.e. for terrain with orthophoto)

VTK File Formats.vtu, .vtp, .vtkCommodity format for data exchange. Useful for products that require the preservation of scalar fields associated to triangles or vertices of the meshes and scientific analysis via VTK.

Geological Aware Formatsapplication-specific3D geological models from 3D geomodeling software packages

Neutral file formats must be preferred

Hierarchical archivesPlanteary Data System (v3,v4).pds, .imgArchived dataset with variable content

Other formats

Specific file formats might be used for either accessing mission-specific dataset or for use with specific software. These includes: