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PeopleData Base DescriptionInstitute / TeamShort description of service (few lines)Use case(s)Representative image (e.g. data/plot/graph/map)ppt or alike as presentedURL (when relevant)q.rd for your service (if relevant)SQL script to build the database
Trompet LoïcSOIR/SPICAV/VEXRoyal Belgian Institute for Space Aeronomy / Planetary Aeronomy       
Alan MacfarlanePSA PDS3 Data sampleEuropean Space Agency / PSA       
Vyacheslav Zakharenko, Serge YerinUTR-2-JUNO-groundInstitute of radio astronomy NASU / RINANU   

 

 

   
          
Manuel Scherf, Tarek Al-UbaidiVEx-MAG, IMPEx treeIWF-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.

VEx-MAG:

 

IMPEx:

The IMPEx Data Model and ProtocolIWF-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.

vexmag_epn20.rdbuild_vexmag_input.ph

 

 

Patrick Guio, Nicholas AchilleosMDISCUCL, 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.

nach_ucl_presn_for_vespa.pdf  

mdisc_db.sql

mdisc_views.sql

Jan Soucek, David PisaCluster Prime Parameter, (future: PSWS tables)IAP, PragueAs 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-CampilloPVOLPlanetary Sciences Group, UPV/EHU, BilbaoImage database (photometric, images, maps, graphs) from amateur astronomers.Research on different bodies (Gas giants and their satellites, Mars, Venus). PVOL_VESPA.pdfCurrent PVOL website  
Patrick Maeght, Jean-Michel GlorianClimsoIRAPImages 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 JourdaneCDPP/AMDAIRAPProvides access to the general AMDA database

Upgrades the V1 implementation to V2. Worked on Cassini SKR data

     
Nathanael Jourdane, Arnaud Beth, Vincent GénotIllumination 67PIRAP + Imperial CollegeProvides illumination maps for Chury; both numerical and image data will be accessedShows 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 MininMRO/CRISM (future: Chandrayan/M3)JacobsUni, BremenPlanetServer (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)
  • surface composition of Mars, Moon
  • Surface (composition) changes on planetary surfaces
  • Illumination studies of Moon polar areas

 

http://epn1.epn-vespa.jacobs-university.de

http://planetserver.eu

  
YIN ZIMCD (GCM of Mars)LMD, Paris       

Stavro Ivanovski, Maria Teresa Capria

KHTM (Kelvin Helmhotz Tearing Mode) Earth+67PIAPS, 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 ErardVEx VIRTISLESIA, MeudonImaging 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)

 

http://voparis-europlanet.obspm.fr/utilities/Tuto_TopCat_VEx.pdf

(presentation of v1 service and dev plan)

   

Luisa M. Lara

Jaime Jimenez

Atmosphere: absorption cross sections

IAA-CSIC

Granada

Absorption cross sections for gaseous species of atmospheric interestComputation of photodissociation coefficients and of atmospheric heating due to VUV-UV stellar radiation.   
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