The Visual and Infrared Mapping Spectrometer (VIMS) instrument
onboard the Cassini spacecraft observed the system of Saturn,
acquiring spectral cubes in the range 0.4-5.2 microns. This service
focuses on Saturn satellites, and provides access to calibrated and
ancillary data, computed as described here:
https://vims.univ-nantes.fr/info/isis-calibration. It also provides
direct links to a larger web site with previews.
Paris Astronomical Data Centre - Constructor University
Description:
The Mars Crater Catalog by S.J. Robbins was generated from THEMIS
Daytime IR and Viking MDIM 2.1 global mosaics of Mars. Craters were
selected using 5 points along the rim. The table is statistically
complete to the diameter of ~1.0 km. The table contains morphologic
and morphometric data for craters with diameter larger than 3 km. The
Prometheus basin has been excluded from the Catalog due to technical
issues.
Reference: "A New Global Database of Mars Impact Craters ≥1 km: (1)
Database Creation, Properties, and Parameters", S.J. Robbins and B.M.
Hynek, Journal of Geophysical Research - Planets, v.117. (2012) DOI:
10.1029/2011JE003966
Paris Astronomical Data Centre - Constructor University
Description:
A catalogue of Mars craters by Lagain et al. (2020), extending the previous
catalogue from Robbins and Hynek (2012, DOI:10.1029/2011JE003966). 185 craters
were added by Lagain, the object IDs are compatible with the previous work.
Reference: "Impact cratering rate consistency test from ages of layered ejecta on Mars",
Lagain et al., Planetary and Space Science, v.180. (2020)
DOI: 10.1016/j.pss.2019.104755
Mars_dust provides a multiannual climatology of Martian airborne dust as measured by various space missions. The retrieved column dust optical depth is mapped for each Martian year and formatted as cubes with time in the 3rd dimension. Two versions are available: irregularly gridded maps, and regular maps produced by kriging. These latter maps are used as column-integrated dust scenarios in the Mars Climate Database (MCD v5). The detailed description of the methodology and dataset can be found in: Montabone et al (2015) Icarus 251, pp. 65-95https://doi.org/10.1016/j.icarus.2014.12.034 ; Montabone et al (2020) JGR-Planets https://doi.org/10.1029/2019JE006111
The database contains some outputs of the MCD for all the scenarios
available, at different positions of latitude and longitude. These MCD
outputs are provided as Votables containing profiles of temperatures,
pressures, density and abundances of O2 and O3 for altitudes between 0
and 249.5 km from the surface.
MCD is a database of atmospheric statistics compiled from Global Climate Model (GCM) numerical simulation of Martian atmosphere (<a href=http://www-mars.lmd.jussieu.fr>http://www-mars.lmd.jussieu.fr</a>). The GCM computes in 3D the atmospheric circulation and climate taking into account radiative transfer through the gaseous atmospheres and the dust and ice aerosols, includes a representation of the CO2 ice condensation and sublimation on the ground and in the atmosphere, simulates the water cycle (with modelling of cloud microphysics), the dust multisize particle transport, the atmospheric composition controlled by the photochemistry and the local non-condensible gas enrichment and depletion induced by CO2 condensation and sublimation, and has been extended into the thermosphere and to model ionospheric processes (due to chemistry). The database extends up to exobase (the top of the thermosphere, roughly at 300km in altitude); in addition to statistics on temperature, wind, pressure, radiative fluxes, it provides data such as atmospheric composition (including dust water vapor and ice content) and make use of 'dust and Extreme Ultra Violet (EUV) scenarios' to represent the variation of dust in the atmosphere and solar EUV conditions. User Manual of the service : <a href=http://vo.lmd.jussieu.fr:8080/MCD_VESPA_service_user_manual.pdf>User Manual of the service </a> .
Since 1973, the 18-cm lines of the OH radical have been
systematically observed in a number of comets with the Nançay radio
telescope. This allowed an evaluation of the cometary water production
rates and their evolution with time, as well as a study of several
physical processes: the excitation mechanisms of the OH radio lines,
the expansion of the cometary atmospheres, their anisotropy in
relation with non-gravitational forces, the Zeeman effect in relation
with the cometary magnetic field. The Nançay observations of 53
cometary apparitions between 1982 and 2009 are now organized in this
database.
The database contains some outputs of the VCD for the scenarios : {1)
Standard cloud albedo Scenario, solar EUV average conditions ; 2)
Standard cloud albedo Scenario, solar EUV minimum conditions ; 3)
Standard cloud albedo Scenario, solar EUV maximum conditions ; 4) Low
cloud albedo Scenario, solar EUV average conditions ; 5) High cloud
albedo Scenario, solar EUV average conditions available}, at different
positions of latitude and longitude. These VCD outputs are provided as
Votables containing profiles of temperatures, pressures, density and
abundances of main species for altitudes between 0 and 349.5 km from
the surface.
The ephemeris were produced by simulating the ejection of meteoroids
from the sunlit hemisphere of cometary nuclei, typically from 0 to 3
au, followed by the propagation of orbits of meteoroids in the Solar
System, taking into account the gravity of the Sun, the 8 planets,
Pluto, and the Moon, as well as the radiation pressure and the
Poynting-Robertson drag. Note that asteroid parent bodies were
considered as active (i.e. comet-like bodies) even if they are not
active today. The showers are predicted when a planet enters a large
enough set of meteoroids, at a distance less than typically 0.01 au.
See Vaubaillon J., Colas F., Jorda L. 2005 A new method to predict
meteor showers. I. Description of the model, Astronomy and
Astrophysics, Volume 439/2 p.751-760, as well as: Vaubaillon J. 2017 A
confidence index for forecasting of meteor showers, Planetary and
Space Science, Volume 143 p.78-82
