JAXA Virtual Planet: Quick Guide

JAXA Virtual Planet (VP) is a web-based GIS for exploring and analyzing lunar datasets from Kaguya. There is an “Basic” mode for the general public, and an “Advanced” mode for researchers which features enhanced analytical functions.

VP demo — This figure shows an example of layers displayed via JAXA Virtual Planet. This example shows feature names over the lunar global topography layer.

About JAXA Virtual Planet (VP)

VP has an Basic mode (high-operability system for the general public) and an Advanced mode (system with sophisticated analytical functions for researchers). They can be accessed at the URLs below.

Access URLs

Select a mode based on what you want to do.

Mode	Purpose	URL
Basic	Data browsing	https://vp.darts.isas.jaxa.jp/moon/?lang=en
Advanced	Data analysis	https://vp.darts.isas.jaxa.jp/moon/?lang=en&pro=1

*Analyses can be performed by displaying the layer containing the necessary information and using the tools included in the toolbox, after first selecting a mode and a view to display.

Available views

Mode	View	Coordinate System (Click to show WKT)
Basic/Advanced	3D globe	GCS_Moon_2000 (ESRI:104903) `GEOGCS["GCS_Moon_2000",DATUM["D_Moon_2000",SPHEROID["Moon_2000_IAU_IAG",1737400.0,0.0]],PRIMEM["Reference_Meridian",0.0],UNIT["Degree",0.0174532925199433]]`
Basic/Advanced	Equidistant cylindrical 3D	SIMPLE_CYLINDRICAL_MOON `PROJCS["SIMPLE_CYLINDRICAL_MOON",GEOGCS["GCS_MOON",DATUM["D_MOON",SPHEROID["MOON",1737400.0,0.0]],PRIMEM["Reference_Meridian",0.0],UNIT["Degree",0.0174532925199433]],PROJECTION["Plate_Carree"],PARAMETER["false_easting",0.0],PARAMETER["false_northing",0.0],PARAMETER["central_meridian",0.0],UNIT["Meter",1.0]]`
Basic/Advanced	North polar stereographic 3D	PolarStereographic_Moon (Stereographic_North_Pole) `PROJCS["PolarStereographic_Moon",GEOGCS["GCS_Moon",DATUM["D_Moon",SPHEROID["Moon_polarRadius",1737400.0,0.0]],PRIMEM["Reference_Meridian",0.0],UNIT["Degree",0.0174532925199433]],PROJECTION["Stereographic_North_Pole"],PARAMETER["false_easting",0.0],PARAMETER["false_northing",0.0],PARAMETER["central_meridian",0.0],PARAMETER["standard_parallel_1",90.0],UNIT["Meter",1.0]]`
Basic/Advanced	South polar stereographic 3D	PolarStereographic_Moon (Stereographic_South_Pole) `PROJCS["PolarStereographic_Moon",GEOGCS["GCS_Moon",DATUM["D_Moon",SPHEROID["Moon_polarRadius",1737400.0,0.0]],PRIMEM["Reference_Meridian",0.0],UNIT["Degree",0.0174532925199433]],PROJECTION["Stereographic_South_Pole"],PARAMETER["false_easting",0.0],PARAMETER["false_northing",0.0],PARAMETER["central_meridian",0.0],PARAMETER["standard_parallel_1",-90.0],UNIT["Meter",1.0]]`
Advanced only	Equidistant cylindrical 2D	SIMPLE_CYLINDRICAL_MOON `PROJCS["SIMPLE_CYLINDRICAL_MOON",GEOGCS["GCS_MOON",DATUM["D_MOON",SPHEROID["MOON",1737400.0,0.0]],PRIMEM["Reference_Meridian",0.0],UNIT["Degree",0.0174532925199433]],PROJECTION["Plate_Carree"],PARAMETER["false_easting",0.0],PARAMETER["false_northing",0.0],PARAMETER["central_meridian",0.0],UNIT["Meter",1.0]]`
Advanced only	North polar stereographic 2D	PolarStereographic_Moon (Stereographic_North_Pole) `PROJCS["PolarStereographic_Moon",GEOGCS["GCS_Moon",DATUM["D_Moon",SPHEROID["Moon_polarRadius",1737400.0,0.0]],PRIMEM["Reference_Meridian",0.0],UNIT["Degree",0.0174532925199433]],PROJECTION["Stereographic_North_Pole"],PARAMETER["false_easting",0.0],PARAMETER["false_northing",0.0],PARAMETER["central_meridian",0.0],PARAMETER["standard_parallel_1",90.0],UNIT["Meter",1.0]]`
Advanced only	South polar stereographic 2D	PolarStereographic_Moon (Stereographic_South_Pole) `PROJCS["PolarStereographic_Moon",GEOGCS["GCS_Moon",DATUM["D_Moon",SPHEROID["Moon_polarRadius",1737400.0,0.0]],PRIMEM["Reference_Meridian",0.0],UNIT["Degree",0.0174532925199433]],PROJECTION["Stereographic_South_Pole"],PARAMETER["false_easting",0.0],PARAMETER["false_northing",0.0],PARAMETER["central_meridian",0.0],PARAMETER["standard_parallel_1",-90.0],UNIT["Meter",1.0]]`

Displayable layers

The following layers are available. Initially, only the base map is displayed.

See the links below for source data and references.

Layer information (Click to expand)

Layer name	Detailed description
Nomenclature	Lunar nomenclature is cited from the USGS Gazetteer of Planetary Nomenclature.
Graticule	The geographic coordinate system is based on GCS_Moon_2000 (ESRI:104903). WKT `GEOGCS["GCS_Moon_2000",DATUM["D_Moon_2000",SPHEROID["Moon_2000_IAU_IAG",1737400.0,0.0]],PRIMEM["Reference_Meridian",0.0],UNIT["Degree",0.0174532925199433]]`
Lunar global topography	Lunar global topography [km] map acquired by SELENE Laser Altimeter (LALT) observations. The product is represented by 360-degree spherical harmonics referenced to a 1737.4 km sphere at the lunar center of mass. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/lalt_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lalt-5-topo-ggt-map-v2.0/ https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lalt-5-topo-gt-np-img-v2.0/ https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lalt-5-topo-gt-sp-img-v2.0/ References `This data should be cited as follows when used in papers, etc.: Araki, H., Tazawa, S., Ishihara, Y., et al. Lunar global shape and polar topography derived from Kaguya-LALT laser altimetry. Science, 323, 5916, 897-900 (2009). https://doi.org/10.1126/science.1164146`
Mare unit age	Polygons representing the estimated ages [Gyr] of lunar maria based on stratigraphic relationships of mare basalt units interpreted from SELENE Lunar Radar Sounder (LRS). The source data were obtained from Figure 5 in Oshigami et al. (2014). The absolute ages were determined based on crater size–frequency distributions reported in Hiesinger et al. (2000, 2003, 2010), Kodama and Yamaguchi (2003), and Morota et al. (2011). References Oshigami, S., Watanabe, S., Yamaguchi, Y., et al. Mare volcanism: Reinterpretation based on Kaguya Lunar Radar Sounder data. Journal of Geophysical Research Planets, 119, 1037–1045 (2014). https://doi.org/10.1002/2013JE004568 Hiesinger, H., Jaumann, R., Neukum, G., et al. Ages of mare basalts on the lunar nearside. Journal of Geophysical Research Planets, 105, 29229–29275 (2000). https://doi.org/10.1029/2000JE001244 Hiesinger, H., Head III, J. W., Wolf, U., et al. Ages and stratigraphy of mare basalts in Oceanus Procellarum, Mare Nubium, Mare Cognitum, and Mare Insularum. Journal of Geophysical Research Planets, 108, E7, 5065 (2003). https://doi.org/10.1029/2002JE001985 Morota, T., Haruyama, J., Ohtake, M., et al. Timing and characteristics of the latest mare eruption on the Moon. Earth and Planetary Science Letters, 302, 255–266 (2011). https://doi.org/10.1016/j.epsl.2010.12.028 Kodama, S., and Yamaguchi, Y. Lunar mare volcanism in the eastern nearside region derived from Clementine UV/VIS data. Meteoritics & Planetary Science 38, Nr 10, 1461–1484 (2003). https://doi.org/10.1111/j.1945-5100.2003.tb00251.x
LRS subsurface reflection points	The unit boundary depths of mare basalts determined by Ishiyama and Kumamoto (2019), based on radargrams obtained by SELENE Lunar Radar Sounder (LRS), are shown. By clicking on a point displayed in Mare Smythii, the depths of four echoes (i.e., unit boundaries) at that location are displayed. Elevation of surface indicates the depth of the surface echo read from the LRS radargram, Elevation of echo 1–4 indicate the depths of subsurface echoes read from the LRS data, Apparent depth is the difference between the surface echo and the subsurface echoes, and Depth is the true depth calculated assuming a dielectric constant of 6. References `This data should be cited as follows when used in papers, etc.: Ishiyama, K. and Kumamoto, A. Volcanic history in the Smythii basin on SELENE radar observation. Scientific Reports, 9, 14502 (2019). https://doi.org/10.1038/s41598-019-50296-9`
SP radiance & diffuse reflectance	Hyperspectral visible and near-infrared reflectance spectra based on the SP Level2C Product derived from observations by the SELENE Spectral Profiler (SP). The SP acquired hyperspectral data over areas of ~500 m × 500 m across the Moon. By clicking on an observation point in this layer displays the radiance [W/m²/μ/Sr] and diffuse reflectance. Spectra from the VIS and NIR1 detectors are calibrated following Yokota et al. (2011), and the NIR2 detector is calibrated following Yamamoto et al. (2014). The "thinned" layer achieves faster rendering by reducing the number of full observation points. For faster loading, the 2D view is recommended over the 3D view. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/tc_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-sp-4-level2c-v3.0/ References This data should be cited as follows when used in papers, etc.: Yokota, Y., Matsunaga, T., Ohtake, M., et al. Lunar photometric properties at wavelengths 0.5-1.6 μm acquired by SELENE Spectral Profiler and their dependency on local albedo and latitudinal zones. Icarus, 215, 639-660 (2011). https://doi.org/10.1016/j.icarus.2011.07.028 Yamamoto, S., Matsunaga, T., Ogawa, Y., et al. Calibration of NIR 2 of Spectral Profiler onboard Kaguya/SELENE. IEEE Transactions on Geoscience and Remote Sensing, 52, 6882-6868 (2014). https://doi.org/10.1109/TGRS.2014.2304581
SAR data	A 2D subsurface cross-sectional image derived from reflection echoes acquired by the Kaguya Lunar Radar Sounder (LRS), processed using along-track synthetic aperture lengths of 5 km, 10 km, and 40 km. Clicking on a survey line displays the product. The horizontal axis represents the along-track direction of the spacecraft. The vertical axis shows the apparent depth calculated assuming a dielectric constant of ε = 1, which differs from the actual depth. Surface and subsurface discontinuities appear as variations in echo intensity. The spatial resolution is approximately 75 m in the horizontal direction and ~75 m in apparent depth on the vertical axis. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/lrs_e.htm Data source: 5km: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lrs-5-sndr-ss-sar05-power-v1.0/ 10 km: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lrs-5-sndr-ss-sar10-power-v1.0/ 40 km: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lrs-5-sndr-ss-sar40-power-v1.0/ References Ono, T., Kumamoto, A., Kasahara, Y., et al. The Lunar Radar Sounder (LRS) Onboard the KAGUYA (SELENE) Spacecraft. Space Science Reviews, 154, 145-192 (2010). https://doi.org/10.1007/s11214-010-9673-8 This data should be cited as follows when used in papers, etc.: Kobayashi, T., Kim, J. H., Lee, S. R., et al. Synthetic aperture radar processing of Kaguya Lunar Radar Sounder data for lunar subsurface imaging. IEEE Transactions on Geoscience and Remote Sensing, 50, 6082437, 2161-2174 (2012). https://doi.org/10.1109/TGRS.2011.2171349
LRS Radargram	2D high-resolution subsurface cross section of reflected echo intensity obtained by SELENE Lunar Radar Sounder (LRS). Clicking on a survey line displays the product. The horizontal axis is the satellite ground track. The vertical axis represents the apparent depth calculated with dielectric constant ε = 1, which differs from the actual depth. Surface and subsurface discontinuities appear as variations in echo intensity. The spatial resolution is ~75 m on the horizontal axis and ~75 m on the apparent depth of the vertical axis. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/lrs_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lrs-5-sndr-ss-high-v2.0/ References `Ono, T., Kumamoto, A., Kasahara, Y., et al. The Lunar Radar Sounder (LRS) Onboard the KAGUYA (SELENE) Spacecraft. Space Science Reviews, 154, 145-192 (2010). https://doi.org/10.1007/s11214-010-9673-8`
MI FeO & TiO₂ abundance	Abundance (wt%) of FeO and TiO₂ based on SELENE Multiband Imager (MI) observations. This product was calculated from the MI_MAP product using the method by Otake et al. (2012). This layer covers latitudes from 85°N to 85°S with a spatial resolution of 128 pix/degree. References `This data should be cited as follows when used in papers, etc.: Otake, H., M. Ohtake, and N. Hirata, Lunar iron and titanium abundance algorithms based on SELENE (Kaguya) Multiband Imager data, Lunar and Planetary Science Conference, 43rd (2012), Abstract 1905. https://ui.adsabs.harvard.edu/abs/2012LPI....43.1905O`
MI reflectance	Visible and near-infrared reflectance spectral data based on the MI_MAP Product derived from observations by the SELENE Multiband Imager (MI). The MI_MAP product is a 9-band data cube covering latitudes from 85°N to 85°S with a spatial resolution of 2048 pix/degree. This layer allows viewing of the reflectance spectrum at a selected position by clicking. Two reflectance values are plotted at 1000 nm because this is observed by both the VIS and NIR detectors. For an overview of the instrument, see below: https://www.selene.jaxa.jp/en/equipment/tc_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-mi-5-map-v3.0/ References `Ohtake, M., Haruyama, J., Matsunaga, T., et al. Performance and scientific objectives of the SELENE (KAGUYA) Multiband Imager. Earth, Planets and Space 60, 257–264 (2008). https://doi.org/10.1186/BF03352789`
Nuclide map	The mass concentration distribution of K/Th/U/Ca based on observations by the SELENE Gamma-Ray Spectrometer (GRS) at an altitude of ~100 km. The product covers the entire lunar surface with an intrinsic spatial resolution of ~150 km. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/grs_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-grs-5-nuclide-map-v1.0/ References `Kobayashi, S., Hasebe, N., Shibamura, E. et al. Determining the absolute abundances of natural radioactive elements on the lunar surface by the Kaguya Gamma-ray Spectrometer. Space Science Reviews 154, 193–218 (2010). https://doi.org/10.1007/s11214-010-9650-2`
TC reflectance map (low Sun)	Surface reflectance map acquired by SELENE Terrain Camera (TC) under low solar illumination from the east (morning) and from the west (evening). This product covers most of the globe at a resolution of 10 m/pixel, except for some high-latitude areas longitudinal areas. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/tc_e.htm Data source: Morning: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-tc-5-morning-map-v4.0/ Evening: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-tc-5-evening-map-v4.0/ References `Haruyama, J., Ohtake, M., Matsunaga, T., et al. Data products of SELENE (Kaguya) Terrain Camera for future lunar missions. 45th Lunar and Planetary Science Conference, p. 1304 (2014). https://ui.adsabs.harvard.edu/abs/2014LPI....45.1304H`
TC ortho map	TC ortho data acquired by SELENE Terrain Camera (TC). This product covers most of the globe at a resolution of 10 m/pixel, except for some high-latitude areas longitudinal areas. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/tc_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-tc-5-ortho-map-v2.0/ References `Haruyama, J., Ohtake, M., Matsunaga, T., et al. Data products of SELENE (Kaguya) Terrain Camera for future lunar missions. 45th Lunar and Planetary Science Conference, p. 1304 (2014). https://ui.adsabs.harvard.edu/abs/2014LPI....45.1304H`
TC DTM (SLDEM2013)	DTM map based on the SLDEM2013 product which combined observations from the SELENE Terrain Camera (TC), Multiband Imager (MI), and NASA Lunar Orbiter Laser Altimeter (LOLA). The DTM was primarily generated from TC (10 m/pix), with gaps filled using MI (20 m/pix) and LOLA (60 m/pix). The product covers the entire Moon. Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-tc-5-sldem2013-v1.0/ References `Haruyama, J., Ohtake, M., Matsunaga, T., et al. Data products of SELENE (Kaguya) Terrain Camera for future lunar missions. 45th Lunar and Planetary Science Conference, p. 1304 (2014). https://ui.adsabs.harvard.edu/abs/2014LPI....45.1304H`
Bouguer gravity anomaly	Bouguer gravity anomaly [mGal] model based on the SGM100h lunar gravity field model with degree 100. The gravity model was derived from the 4-way Doppler observations using SELENE RSAT and VRAD Satellite. The bouguer gravity anomaly is calculated from SGM100h and a LALT topographic model (STM-359_grid-03) assuming the crustal density of 2800 kg/m³. The high-frequency “spotty” signatures are likely due to the less accurate gravity coefficients above degree 70. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/rsat_e.htm Data source: SGM100h grid data, RISE Project References `This data should be cited as follows when used in papers, etc.: Matsumoto, K., Goossens, S., Ishihara, Y., et al. An improved lunar gravity field model from SELENE and historical tracking data: Revealing the farside gravity features. Journal of Geophysical Research: Planets, 115, E06007 (2010), https://doi.org/10.1029/2009JE003499`
Free air gravity anomaly	Bouguer gravity anomaly [mGal] model based on the SGM100h lunar gravity field model with degree 100. The gravity model was derived from the 4-way Doppler observations using SELENE RSAT and VRAD Satellite. For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/rsat_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-rise-5-grav-map-v1.0/ SGM100h grid data, RISE Project References `This data should be cited as follows when used in papers, etc.: Matsumoto, K., Goossens, S., Ishihara, Y., et al. An improved lunar gravity field model from SELENE and historical tracking data: Revealing the farside gravity features. Journal of Geophysical Research: Planets, 115, E06007 (2010), https://doi.org/10.1029/2009JE003499`
Crustal thickness	Lunar crustal thickness map derived from the SGM100h lunar gravity field model and STM-359_grid-03 lunar topography model. The gravity model was derived from the 4-way Doppler observations using SELENE RSAT and VRAD Satellite. The topography model is derived from SELENE LALT observations. This product was created with the condition that the Bouguer gravity anomaly is explained by Moho topography without having the mantle exposed at the lunar surface. Assumed densities of the crust, mantle, and mare basalt layer are 2800 kg/m³, 3360 kg/m³, and 3200 kg/m³, respectively. Data source: Grid data of crustal thickness model, RISE Project References `This data should be cited as follows when used in papers, etc.: Ishihara, Y., Goossens, S., Matsumoto, K., et al. Crustal thickness of the Moon: Implications for farside basin structures. Geophysical Research Letters, 36, L19202 (2009). https://doi.org/10.1029/2009GL039708`
Magnetic anomaly	Lunar magnetic anomaly mosaic data acquired by SELENE Lunar Magnetometer (LMAG) observations at an altitude of 100 km. This product shows the components of the lunar magnetic anomaly vector (X: east–west; Y: north–south; Z: radial; F: total magnetic field intensity). For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/lmag_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lmag-5-ma-map-v1.0/ References `Tsunakawa, H., Shibuya, H., Takahashi, F., et al. Lunar magnetic field observation and initial global mapping of lunar magnetic anomalies by MAP-LMAG onboard SELENE (Kaguya). Space Science Reviews, 154, 219-251 (2010). https://doi.org/10.1007/s11214-010-9652-0`
Magnetic anomaly OP	Lunar magnetic anomaly mosaic data derived from SELENE Lunar Magnetometer (LMAG) observations at an altitude of ~30 km. This product shows the components of the lunar magnetic anomaly vector (X: east–west component; Y: north–south component; Z: radial component; F: total magnetic field intensity). For an overview of the instrument, see below: https://www.kaguya.jaxa.jp/en/equipment/lmag_e.htm Data source: https://data.darts.isas.jaxa.jp/pub/pds3/sln-l-lmag-5-ma-map-option-v1.0/ References Tsunakawa, H., Shibuya, H., Takahashi, F., et al. Lunar magnetic field observation and initial global mapping of lunar magnetic anomalies by MAP-LMAG onboard SELENE (Kaguya). Space Science Reviews, 154, 219-251 (2010). https://doi.org/10.1007/s11214-010-9652-0 Tsunakawa, H., Takahashi, F., Shimizu, H., et al. Regional mapping of the lunar magnetic anomalies at the surface: Method and its application to strong and weak magnetic anomaly regions. Icarus, 228, 15, 35-53 (2014). https://doi.org/10.1016/j.icarus.2013.09.026
Microrelief map "IN-YOU-ZU"	A global lunar map produced using "IN-YOU-ZU", a microtopography visualization technique developed by AERO TOYOTA Corporation. Topographic shading is represented by brightness, and topographic convexity and concavity (local highs and depressions) are represented by hue. Specifically, a hillshade rendered using nadir illumination is overlaid with a hue layer in which lower terrain relative to its surroundings is assigned cool colors and higher terrain is assigned warm colors, followed by color tone adjustment. The source topographic data used are SLDEM2013, which was constructed from observation data acquired by the Kaguya Terrain Camera (TC), Multiband Imager (MI), and NASA’s Lunar Orbiter Laser Altimeter (LOLA). When reproducing figures displaying the IN-YOU-ZU layer, “AERO TOYOTA Corporation” must be credited within the figure. For details of IN-YOU-ZU, see below (only in Japanese): https://www.aerotoyota.co.jp/spatialinfo/inyouzu/ References `Akiyama, Y. and Sekoguchi, R. (2007). Map, Journal of the Japan Cartographers Association, 45, 1, 37–46 (in Japanese). https://doi.org/10.11212/jjca1963.45.37`

Toolbox

Use the tools included in the toolbox in each mode. Tools available in the toolbox differ for each mode.

Mode	Tools
Basic/Advanced	Distance Measurement (3D views only) Area Measurement (3D views only) Search by Name
Advanced only	Elevation Profile (*3D views only) Memo Print Custom Visualization Download Add Point by Coordinates Subsolar/Sub-Earth points

How to use

Many different types of displays are available on JAXA Virtual Planet through selections of views, layers, and tools.

An explanation of JAXA Virtual Planet and details on how to use it can be downloaded from the following link.

Download operation manual

Analysis example from JAXA Virtual Planet

Perform many different types of analyses on JAXA Virtual Planet. An example of an analysis via band ratioing using MI reflectance data can be downloaded from the following link.

Download instructions for data analysis procedures