|People||Data Base Description||Institute / Team||Short description of service (few lines)||Use case(s)||Representative image (e.g. data/plot/graph/map)||ppt or alike as presented||URL (when relevant)||q.rd for your service (if relevant)||SQL script to build the database|
|Trompet Loïc||SOIR/SPICAV/VEX||Royal Belgian Institute for Space Aeronomy / Planetary Aeronomy|
|Alan Macfarlane||PSA PDS3 Data sample||European Space Agency / PSA|
|Vyacheslav Zakharenko, Serge Yerin||UTR-2-JUNO-ground||Institute of radio astronomy NASU / RINANU|
|Manuel Scherf, Tarek Al-Ubaidi||VEx-MAG, IMPEx tree||IWF-ŒAW, Graz|
VEx-MAG: Update of service from EPN-TAP V1.0 to EPN-TAP V2.0. VEx-MAG-Graz is the Venus Express magnetic field data center of IWF-OeAW at Graz, currently hosting magnetic field data (4s sampling) from 2006/04/24 to 2012/12/28. Data also available via AMDA.
IMPEx tree: Update of service from EPN-TAP V1.0 to EPN-TAP V2.0. The IMPEx data model, developed during the IMPEx-FP7 project gives access to a wide variety of plasma and magnetic field simulation data of various different Simulation Data Bases (SMDBs), namely of SINP-MSU, FMI-HYBRID, FMI-GUMICS and LATMOS. It also provides access to data by CDPP-AMDA and IRAP-CLWeb. All data and services can also be accessed via the IMPEx Portal.
VEx-MAG: Study of the induced magnetosphere of and Space Weather at Venus. The magnetic field data can e.g. also be compared with simulational data via the tools CDPP-AMDA or CDPP-3DView.
IMPEx tree: The IMPEx data model was originally developed to make observational data easily comparable with simulation data and to fill observational gaps with numerical models. At Mars e.g. simulations of the magnetic field can now be combined with measurements of the plasma environment by Mars Express. See also the IMPEx Demonstrators and Tutorials Website.
|The IMPEx Data Model and Protocol||IWF-EPN-TAP Data Center|
build_vexmag_input.ph extracts the relevant meta data from the source files and insert them in a meta data (text) file. This file is then further processed by the resource descriptor (vexmag_epn20.rd) that generates the epn_core table and inserts the meta data accordingly.
|Patrick Guio, Nicholas Achilleos||MDISC||UCL, London|
Access to UCL Magnetodisc model output. The magnetostatic model computes the magnetic field and plasma distribution for different system size of the Jovian and Kronian magnetospheres.
We have identified the necessary EPN-TAP v2 parameters to implement and need to deploy a database which will serve model outputs to the user in both mat and netCDF format.
|A candidate use case would be to use our model in Jovian mode, together with the CDPP-3Dview software, in order to predict the magnetic field components which the Juno spacecraft will observe.|
Above is a figure from Achilleos, Guio and Arridge (2010) showing some plots of model outputs. See this paper and the .pdf presentation for more details of model background and plots.
|Jan Soucek, David Pisa||Cluster Prime Parameter, (future: PSWS tables)||IAP, Prague||As a didactic example, we created a EPN-TAP interface for accessing Cluster CIS prime parameter data in CDF.||Not for actual science use. The database is created to train IAP team.||IAP EPN-TAP server|
|Jon Juaristi-Campillo||PVOL||Planetary Sciences Group, UPV/EHU, Bilbao||Image database (photometric, images, maps, graphs) from amateur astronomers.||Research on different bodies (Gas giants and their satellites, Mars, Venus).||PVOL_VESPA.pdf||Current PVOL website|
|Patrick Maeght, Jean-Michel Glorian||Climso||IRAP||Images of the photosphere and low corona with two coronagraphs (on H-α, He I, Fe XIII) and two telescopes (on H-α, Ca II)||Sun-Earth relation contribution.|
|Gangloff Michel, Myriam Bouchemit, Vincent Génot, Nicolas André, Nathanael Jourdane||CDPP/AMDA||IRAP||Provides access to the general AMDA database|
Upgrades the V1 implementation to V2. Worked on Cassini SKR data
|Nathanael Jourdane, Arnaud Beth, Vincent Génot||Illumination 67P||IRAP + Imperial College||Provides illumination maps for Chury; both numerical and image data will be accessed||Shows the comet illumination for a given lat/lon of the Sun in the comet frame. Next step: shows the comet illumination for a given time||illu_67P_q.rd|
|Angelo Pio Rossi, Mikhail Minin||MRO/CRISM (future: Chandrayan/M3)||JacobsUni, Bremen||PlanetServer (Planetary Science Data Service of EarthServer-2 H2020 e-Infra project) provides access, visualisation and analytical capabilities to Mars (Moon to come soon) image and hyperspectral data with sub-granule query capability (spatial and spectral subsets, multi-band spectra) using OGC Web Services (WCS, WCPS mainly, as well as WMS)|
|YIN ZI||MCD (GCM of Mars)||LMD, Paris|
Stavro Ivanovski, Maria Teresa Capria
|KHTM (Kelvin Helmhotz Tearing Mode) Earth+67P||IAPS, Rome|
Provide access to MHD mixing layer model output. The model is utilized for simulating coupled Kelvin-Helmholtz and tearing mode instabilities at the Earth's magnetopause layer and has been updated for cometary environment.
We have been working on the implementation of the necessary EPN-TAP v2 parameters to create a database which will serve model outputs to the user in ASCII format.
|In order to support the interpretation of published magnetometric data, a candidate case would be to investigate the magnetic field configurations and flow shear at the magnetic cavity at 67P. It could complement the studies on the position and the dynamics of the magnetic cavity boundary.|
Density and magnetic field component By, shown as illustration of developed Kelvin Helmholtz and tearing mode instabilities (Model setup and description, Ivanovski et al. 2011).
|Stéphane Erard||VEx VIRTIS||LESIA, Meudon||Imaging spectroscopy of Venus from the Venus-Express mission. EPN-TAP v1 test service updated to v2 & enlarged to extended mission phases and M-visible channel|
- Essentially for studies of the atmosphere, either nadir looking or at the limb.
- Surface is also visible at some wvl on the night side (signal fct of elevation and emissivity)
(presentation of v1 service and dev plan)
Luisa M. Lara
|Atmosphere: absorption cross sections|
|Absorption cross sections for gaseous species of atmospheric interest||Computation of photodissociation coefficients and of atmospheric heating due to VUV-UV stellar radiation.|