Europlanet 2024 RI Transnational Access (TA) Facilities
TA1 Planetary Field Analogue sites
Europlanet 2024 RI’s TA1 Planetary Field Analogues (PFA) provide the most realistic terrestrial geological-geomorphological analogues for volcanic, dry-and humid-cold, hot, highly saline and metalliferous and impact conditions for studies in support of current and forthcoming missions to Mars, the Moon and the icy moons of Jupiter. Europlanet 2024 RI offers free ‘transnational access’ to five diverse PFA sites around the world to carry out research projects.
TA1.1: Geothermal field at Krysuvik. Credit: Matis.
TA1.1: Microbial sampling at Eyjafjallajökull lava field. Credit: Matis.
TA1.1: Source of the Morilla sub-glacial river. Credit: Matis.
TA1.1: Drilling to sample the Skaftarkatlalon sub-glacial lake. Credit: Matis.
TA1.4: Kangerlussuaq field site, Greenland. Credit: AU.
TA1.4: Kangerlussuaq field site, Greenland. Credit: AU.
TA1.4: Kangerlussuaq field site, Greenland. Credit: AU.
TA1.4: Kangerlussuaq field site, Greenland. Credit: AU.
TA1.2: Truck laboratory in Rio Tinto to support researchers in the field. Credit: F Gomez.
TA1.2: Iron precipitates in acidic conditions in Rio Tinto. Credit: F Gomez.
TA1.2: Rio Tinto, south-west Spain is a very acidic 100 km river with intense red dark colour. Credit: F Gomez.
TA1.5: Makgadikgadi Salt Pans, Botswana. A thin carpet of microbial mat on the dried surface of the pan at the beginning of the rainy season. Credit: B. Cavalazzi/F. Franchi.
TA1.5: Makgadikgadi Salt Pans, Botswana. One of the numerous natural springs of artesian water along the southern edge of the Makgadikgadi pan. Credit: B. Cavalazzi/F. Franchi.
TA1.5: Makgadikgadi Salt Pans, Botswana. Students collecting a core of sediments from the pan for sedimentological and geomicrobiological studies. Credit: B. Cavalazzi/F. Franchi.
TA1.5: Makgadikgadi Salt Pans, Botswana. Wrinkled surface of the clay from the Sua pan at the beginning of the rainy season. Credit: B. Cavalazzi/F. Franchi.
TA1.5: Makgadikgadi Salt Pans, Botswana. The flat surface of the Sua pan covered by a crust of evaporitic minerals (e.g., halite, gypsum). Credit: B. Cavalazzi/F. Franchi.
TA1.5: Makgadikgadi Salt Pans, Botswana. Mud cracks on the surface of the pan at the beginning of the rainy season. Credit: B. Cavalazzi/F. Franchi.
TA1.5: Makgadikgadi Salt Pans, Botswana. Flamingos are breeding in some of the salty ponds during the rainy season (Dec – Mar). Credit: B. Cavalazzi/F. Franchi.
TA1.5: Makgadikgadi Salt Pans, Botswana. The surface of the pan is flat and barren, covered in smal pebbles and ventifacts; it represents an ideal analogue for Martian landing sites. Credit: B. Cavalazzi/F. Franchi.
The Danakil field site. Credit: B. Cavalazzi.
The Danakil field site. Credit: B. Cavalazzi.
The Danakil field site. Credit: B. Cavalazzi.
VLUU L200 / Samsung L200
The Danakil field site. Credit: B. Cavalazzi.
VLUU L200 / Samsung L200
The Danakil field site. Credit: B. Cavalazzi.
The Danakil field site. Credit: B. Cavalazzi.
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TA2 Distributed Planetary Laboratory Facility
TA2 Distributed Planetary Laboratory Facility (DPLF) provides access to 24 facilities within 13 research centres that enable the simulation or characterisation of planetary conditions and materials.
TA2.1: Recent high profile research conducted in the laboratory included the analysis of melt inclusions: Melt inclusion in olivine from Mariana Arc ~75 µm diameter. Credit: Igor Nikogosian
TA 2.1: Sampling silver cups from the Piet Hein silver at the Rijksmuseum with GGIF. Credit: Joosje van Bennekom
TA 2.1: A portable laser ablation system in the GGIF at VU Amsterdam allows sampling in situ onto Teflon filters. Credit: Alice Knaf.
TA 2.1: A portable laser ablation system in the GGIF at VU Amsterdam allows sampling in situ onto Teflon filters. Credit: Alice Knaf.
TA2.1: Recent high profile research conducted in the laboratory included the validation of the analysis of fluid inclusions (Fluid and gas inclusions in quartz shown here). Credit: Igor Nikogosian
TA2.1: Recent high profile research conducted in the laboratory included the analysis of diamond inclusions: 1 cm wide polished central plate from a Jwaneng diamond. The inclusions were liberated and dated using the Sm-Nd method. Credit: Igor Nikogosian
Miniaturised chromatographic columns (below) have been developed at VU Amserdam GGIF to limit the blank contribution. Credit: G Davies.
The rate limiting aspect of the GGIF at VU Amsterdam is cleanliness of the chemical preparation in the clean lab. Credit: Michael Gress.
TA 2.1: Triton Plus (at VU Amserdam GGIF) with state-of-the-art collection system allowing the precise analysis of extremely small sample size (> 10pg Sr-Nd-Pb). Credit: G. Davies.
TA 2.1: Users at the Geology and Geochemistry radiogenic and non-traditional stable Isotope Facility, VU Amsterdam. Credit: G Davies.
TA2.2 Electron microscope image showing experiment performed to assess sulphide melt segregation from silicate magma in eucrites and angrites. Round holes in sulphide and melt indicate laser ablation spots made to determine precise chemical compositions of the phases, produced using VU High pressure laboratory [Steenstra et al. 2020, Geochimica et Cosmochimica Acta]
TA2.2 False-color electron microscope image of a high-pressure experiment simulating the reaction between silicon carbide (top) and oxidised silicate melt, and metal (bottom) in rocky exoplanets, produced using VU High pressure laboratory [Hakim et al. 2018, Astronomy and Astrophysics]
TA2.2 Electron microscope image of a high-pressure experiment simulating crystallisation in the lunar magma ocean produced using VU High pressure laboratory. Px = pyroxene, Plag = plagioclase, Glass = quenched magma [Lin et al. 2019, Geochemical Perspectives Letters].
TA 2.2. 800 ton multi-anvil press at high-pressure, high-temperature laboratory at Vrije Universiteit Amsterdam. Credit: Vrije Universiteit Amsterdam.
TA 2.2. Piston cylinder press at high-pressure, high-temperature laboratory at Vrije Universiteit Amsterdam. Credit: Vrije Universiteit Amsterdam.
TA 2.4: The AWTSI chamber at the Planetary Environment Facility, Aarhus University. Credit: AU.
TA 2.4: Schematic of the AWTSII chamber at the Planetary Environment Facility, Aarhus University. Credit: AU.
TA 2.4: The ExoMars2016 DREAMS team visiting the Planetary Environment Facility, AU supported by Europlanet 2020 RI. Credit: AU.
TA 2.4: Inside the test section of the AWTSII wind tunnel at the Planetary Environment Facility, Aarhus University. Credit: AU.
TA 2.4: Laser Doppler velocimeter measuring inside the AWTSII wind tunnel at the Planetary Environment Facility, Aarhus University. Credit: AU.
TA 2.4: The AWTSII chamber at the Planetary Environment Facility, Aarhus University. Credit: AU.
TA 2.4: The AWTSII chamber at the Planetary Environment Facility, Aarhus University. Credit: AU.
TA 2.4: The inside of the AWTSII wind tunnel at the Planetary Environment Facility, Aarhus University during testing of Mars2020 instrumentation. Credit: AU.
TA 2.4: The AWTSII chamber at the Planetary Environment Facility, Aarhus University. Credit: AU.
TA 2.5: 2D mid-IR reflectance map for a space-weathered meteorite from DLR PSL. Credit
TA 2.5: Emissivity spectra of a quartz sample taken in vacuum at increasing temperatures at DLR PSL. Credit: DLR
TA 2.5: The Laboratory set-up at PSL with view of the 3 spectrometers and the microscope visible in foreground. Credit: DLR
TA 2.3: False colour element map of QUE 99177 carbonaceous chondrite using facilities at Natural History Museum PMCF. Credit: NHM
TA 2.3: Visualisation from micro-CT data showing vesicles in an Apollo 15 basalt using facilities at Natural History Museum PMCF. Credit: NHM
TA 2.3: Cathodoluminescence image of a chondrule from the Kota Kota enstatite chondrite using facilities at Natural History Museum PMCF. Credit: NHM
TA 2.3: FEI Quanta 650 Field Emission SEM at Natural History Museum PMCF. Credit: NHM
TA 2.3: Cameca SX100 Electron Microprobe at Natural History Museum PMCF. Credit: NHM.
TA 2.3: JXA-8530 Field Emission Electron Microprobe Analyser. Credit: NHM.
TA 2.7: Side view of impact onto inclined sand, with ejecta shown. The impact was from the right, moving horizontally, it struck half way along the target and the ejecta is visible moving leftwards. Credit: University of Kent.
TA 2.7: Interior of the target chamber. This is set up for a vertical shot into a sand target. Credit: University of Kent.
TA 2.7: University of Kent light gas gun, top view. The projectile is fire from the bottom of the image along the barrel into the white target chamber at the far end. Credit: University of Kent.
TA 2.7: University of Kent light gas gun. The projectile moves from the extreme right into the white chamber at the extreme left. Credit: University of Kent.
TA 2.8: Complete set of spectra of Mukundpura CM2 meteorite acquired in bidirectional reflectance distribution function mode. Each panel corresponds to an incidence angle [Potin et al. 2019].
TA 2.8: Vis-NIR reflectance spectra of several minerals and their mixtures with different grain sizes and temperatures (140-300 K) [Galiano et al. submitted].
TA 2.8: Near-IR bidirectional reflection spectra (i=0°, e=30°) of Smectite SWy-2 for different grain sizes at 298K [Pommerol & Schmitt [2008] (doi: 10.26302/SSHADE/EXPERIMENT_BS_20121213_002)
TA 2.8: Vis-NIR bidirectional reflection spectra of spherical water ice particles for different sizes (2 to 100 µm) and temperatures (173 and 223 K) (doi: 10.26302/SSHADE/EXPERIMENT_OP_20171130_001)
TA 2.8: Some of the sample holders available for SHADOWS. The smallest one (D=2mm, depth=0.5mm) is on top. Credit: IPAG.
TA 2.8: MIRAGE thermal environmental cell for the SHADOWS goniometer (up to 250°C). Credit: IPAG.
TA 2.8: ICEBERG cryogenic environmental cell inside for the SHADOWS goniometer (down to 60K) Credit: IPAG.
TA 2.8: CarboN-IR cryogenic environmental cell inside the SHINE goniometer (down to 70K). Credit: IPAG.
TA 2.8: The SHINE Spectro-Gonio Radiometer with its stabilized monochromatic source and detection electronics, and the goniometer with illumination mirror and detectors, an open sample holder with sulfur powder. Credit: Brissaud et al. 2004.
TA 2.8: The SHADOWS Spectro-Gonio Radiometer with its optical and electronic table. Credit: Potin et al. 2018
TA 2.9: Typical sample types that are analysed in the IPF facility. Credit: CRPG
TA 2.10: He analyses at the rare gas laboratory: Mass spectrometer SFT. Credit: CRPG.
TA 2.10: He analyses at the rare gas laboratory: purification line. Credit: CRPG.
TA 2.10: He analyses at the rare gas laboratory: induction furnace to extract noble gases from samples at Credit: CRPG.
TA 2.10: EA-IRMS systems are easy-to-use solutions for μg- to mg-level elemental and isotope analysis for CNOSH. Credit: CRPG.
TA 2.10: The purified lines under vacuum are used for many applications: D/H and d13C of fluid inclusions, dissolved inorganic carbon, isotopic measurments of gas mixtures. Credit: CRPG.
TA 2.10: The Picarro L2140-i isotopic water analyser enables simultaneous measurements of δ18O, δ17O, δD and determines 17O-excess for paleoclimate, (eco) hydrology, and atmospheric science applications. Credit: CRPG.
TA 2.10: The Thermo Scientific GasBench II is a solution for high precision on-line isotope ratio determination of carbonates and dissolved inorganic carbon. Credit: CRPG.
TA 2.10: Anton Paar High Pressure Asher, used for sample digestion at temperatures up to 300oC and pressures up to 100 bar. Credit: CRPG.
TA 2.10: Thermo Neptune Plus MC-ICPMS installed at CRPG. Credit: CRPG.
TA 2.10: Thermo Triton Plus Thermo-ionization mass spectrometer (TIMS) installed at CRPG. The door of the ion source is open, revealing the sample holder with places for 23 samples. Credit: CRPG
TA 2.9: Internal age variations (in Ma) in a zircon grain, obtained by in situ analyses on the CRPG Cameca 1270 E7 ion probe. Credit: CRPG
TA 2.9: CAMECA IMS 1270 E7 at the Ion Probe Facility of CRPG. Credit: CRPG
The Europlanet ICA support team. Credit: Atomki
TA 2.11: The Europlanet ICA support team. Credit: Atomki
TA 2.11: The shape of the ion beam at the surface of the ice deposited on the ZnSe substrate. Credit: Atomki
TA 2.11: The ice chamber and the FTIR spectrometer. Credit: Atomki
TA 2.11: The Europlanet ICA beamline. Credit: Atomki
TA 2.11: The Tandetron Laboratory of Atomki. Credit: Atomki
TA 2.11: An IR spectra of carbon dioxide ice after irradiation by a beam of 1 MeV protons. CO3 and ozone are observed to have been cre-ated. Credit: Atomki
TA 2.19: Team at the Center for Microbial Life Detection at the Medical University Graz. Credit: Medical University of Graz
TA 2.19: DNA extraction laboratory at the Center for Microbial Life Detection at the Medical University Graz. Credit: Medical University of Graz
TA 2.19: Anaerobic chamber (on the right) at the Center for Microbial Life Detection at the Medical University Graz. Credit: Medical University of Graz
TA 2.13: Emission spectrum of hydrogen induced by electron impact. Credit: Comenius University.
TA 2.13: Basic scheme of the experimental setup. Credit: Comenius University.
TA 2.13: Electron induced fluorescence apparatus. Credit: Comenius University.
TA 2.14: Ion exchange columns in the clean room laboratory at ETH Zürich. Credit: ETH Zürich
TA 2.14: Multi-Collector Inductively Coupled Plasma Mass Spectrometer (MC-ICP-MS) Laboratory at ETH Zürich. Credit: ETH Zürich
TA 2.15: Users of the ETH Zurich Geo- and Cosmochemistry Noble Gas Laboratory. Credit: ETH Zurich.
TA 2.15: Users of the ETH Zurich Geo- and Cosmochemistry Noble Gas Laboratory. Credit: ETH Zurich.
TA 2.15: Users of the ETH Zurich Geo- and Cosmochemistry Noble Gas Laboratory. Credit: ETH Zurich.
TA 2.15: “TOM Dooley” mass spectrometer equipped with compressor source. Credit: ETH Zurich
TA 2.15: UV laser ablation system and “TOM Dooley” gas cleaning and separation line. Credit: ETH Zurich
TA 2.15: CSSE and parts of the gas cleaning and separation line. Credit: ETH Zurich
TA 2.15: The noble gas mass spectrometer “ALBATROS” including parts of the gas cleaning and separation line. Credit: ETH Zurich
TA 2.24: Dr Christian Schröder working at the Wissel Mössbauer transmission setup with ICEoxford cryostat. Credit: C. Schröder.
TA 2.24: Example of a non-destructive Mössbauer spectroscopy measurement using the MIMOS II instrument. Credit: C. Schröder.
TA 2.24: Sensor head of the miniaturised Mössbauer spectrometer MIMOS II. MIMOS II instruments were successfully deployed during the NASA Mars Exploration Rover Spirit and Opportunity missions. Credit: C. Schröder.
TA 2.24: Dust ejection from CO2 ice slab during simulation of Martian surface processes. Credit: U. Stirling
TA 2.24: Dust ejection from CO2 ice slab during simulation of Martian surface processes. Credit: U. Stirling
TA 2.24: Solar simulator (l) and thermal vacuum chamber (DTVC, r). The chamber is an upright cylinder 69 cm in diameter. Credit: U. Stirling
TA 2.16: Gas Interface use, during GIS AMS analyses of small (< 0.1 mg C) samples at AMS14C facility. Credit: Isotoptech Zrt.
TA 2.16: Ion source of the EnvironMICADAS AMS. Credit: Isotoptech Zrt.
TA 2.16: EnvironMICADAS (ETHZ) C-14 AMS system at AMS14C facility. Credit: Isotoptech Zrt.
TA 2.16: Microscope(visual) check of a sample for AMS C-14 analyses. Credit: Isotoptech Zrt.
TA 2.16: Small snail samples for AMS C-14 analyses. Credit: Isotoptech Zrt.
TA 2.16: AMS graphites at AMS14C facility. Credit: Isotoptech Zrt.
TA 2.16: Gas handling line at AMS14C facility. Credit: Isotoptech Zrt.
TA 2.16: Vacuum sealing at AMS14C facility. Credit: Isotoptech Zrt.
TA 2.16: Graphitization reactors at AMS14C facility. Credit: Isotoptech Zrt.
TA 2.16: Cryogenic CO2 gas cleaning at AMS14C facility. Credit: Isotoptech Zrt.
TA 2.17: Detector system of the MAT253 Plus MS at ISIL facility. Credit: Isotoptech Zrt.
TA 2.17: Carbonate handling line for the MAT253 Plus MS. Credit: Isotoptech Zrt.
TA 2.17: Thermo Scientific MAT253 Plus and its KIEL IV interface line at ISIL facility. Credit: Isotoptech Zrt.
TA 2.17: Gas cleaning chromatographic columns in the Flash IRMS EA at ISIL facility. Credit: Isotoptech Zrt.
TA 2.17: Flash IRMS EA and TC on-line interfaces at ISIL facility. Credit: Isotoptech Zrt.
TA 2.17: Sample loading at EA interface of the IRMS system at ISIL facility. Credit: Isotoptech Zrt.
TA 2.17: Gas transport needle of the Delta plus XP IRMS. Credit: Isotoptech Zrt.
TA 2.17: Carbonate and TC sample handling line at ISIL facility. Credit: Isotoptech Zrt.
TA 2.17: Thermo Finnigan Delta plus XP isotope ratio mass spectrometer (IRMS) at ISIL facility. Credit: Isotoptech Zrt.
TA 2.6: DLR Planetary Analog Simulation Lab (PASLAB). Credit: DLR
TA 2.6: DLR Mars Simulation Facility (MSF) Lab. Credit: DLR
TA 2.6: Interior of the Mars Chamber. Credit: DLR
TA 2.6: DLR PASLAB: Planetary Analog Simulation Lab. Credit: DLR
TA 2.21: NanoSIMS 50L at the Open University. Credit: OU.
TA 2.21: NanoSIMS 50L at the Open University. Credit: OU.
TA 2.18: Noble gas handling and cleaning line for the Helix MS at INGIL facility. Credit: Isotoptech Zrt.
TA 2.18: Helix Noble Gas MS system at INGIL facility. Credit: Isotoptech Zrt.
TA 2.18: Detection system of the MM5400 mas spectrometer. Credit: Isotoptech Zrt.
TA 2.18: Noble gas handling and cleaning line for the VG5400 MS at INGIL facility. Credit: Isotoptech Zrt.
TA 2.18: Stainless Steel water container bulbs for 3He-ingrowth method MS at INGIL facility. Credit: Isotoptech Zrt.
TA 2.18: VG5400 Noble Gas MS at INGIL facility. Credit: Isotoptech Zrt.
TA 2.22: Oxygen isotope composition of achondrite meteorites – showing relationship between angrites, HEDs and pallasite stony-iron meteorites. D17O is a measure of deviation from the terrestrial fractionation line – therefore mass fractionation lines are horizontal in this plot. Credit: Greenwood et al 2017.
TA 2.22: 50W CO2 laser producing 10.6 micrometer radiation used to heat samples in the presence of bromine pentafluoride in order to quantitatively liberate oxygen gas for isotope analysis. The sample chamber is on the lab jack and is held in a fixed position while the laser is moved. The sample chamber can hold up to 22 samples and standards. Credit: OU.
TA 2.22: Thermo MAT 253 mass spectrometer used to perform high precision oxygen 3 isotope ratio measurements. Credit: OU.
TA 2.22: Laser assisted fluorination system at the Open University. Credit: OU.
TA 2.20: OU Mars Chamber. Credit: OU.
TA 2.21: Oxygen isotope map of an interplanetary dust particle showing large isotopic variations that span almost the entire breadth of variation observed in planetary materials in a grain <15 microns across. d18O scale in ‰ on right. Credit: Starkey et al 2013.
TA 2.21: Most planetary materials are poor conductors and therefore need to be coated with a conducting layer prior to analysis. Both gold and carbon coaters are available. Credit: OU.
TA 2.20: OU Mars Chamber. Credit: OU.
TA 2.21: Sample preparation facilities supporting NanoSIMS at the Open University include clean benches, clean rooms, optical microscopes, etc. Credit: OU.
OU Mars Chamber
TA 2.20: OU Mars Chamber. Credit: OU.
TA 2.21: NanoSIMS 50L at Open University, showing sample chamber with storage vessel to the left that can accommodate up to 8 sample holders. The NanoSIMS operates only with UHV conditions and therefore providing samples in advance helps maximise outcome of visits. Credit: OU.
Open University Flow Through Chambers. Credit: Nisha Ramkissoon
TA 2.23: Chamber 1 setup for low pressure flow-through experiments at Open University Flow Through Chambers. Credit: Nisha Ramkissoon
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Europlanet 2024 RI has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 871149.
Europlanet AISBL (Association Internationale Sans But Lucratif – 0800.634.634) is hosted by the Department of Planetary Atmospheres of the Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Avenue Circulaire 3, B-1180 Brussels, Belgium.
![TA2.2 Electron microscope image showing experiment performed to assess sulphide melt segregation from silicate magma in eucrites and angrites. Round holes in sulphide and melt indicate laser ablation spots made to determine precise chemical compositions of the phases, produced using VU High pressure laboratory [Steenstra et al. 2020, Geochimica et Cosmochimica Acta]](https://www.europlanet.org/wp-content/uploads/2020/02/VUHP5.png)
![TA2.2 False-color electron microscope image of a high-pressure experiment simulating the reaction between silicon carbide (top) and oxidised silicate melt, and metal (bottom) in rocky exoplanets, produced using VU High pressure laboratory [Hakim et al. 2018, Astronomy and Astrophysics]](https://www.europlanet.org/wp-content/uploads/2020/02/VUHP4.png)
![TA2.2 Electron microscope image of a high-pressure experiment simulating crystallisation in the lunar magma ocean produced using the VU High pressure laboratory. Px = pyroxene, Plag = plagioclase, Glass = quenched magma [Lin et al. 2019, Geochemical Perspectives Letters].](https://www.europlanet.org/wp-content/uploads/2020/02/VUHP3.png)
