Category: TA

The Future of Sample Return

June 24, 2024

The Future of Sample Return

With Insider Dr Enrica Bonato

By Peter McArdle, Hans Huybrighs, Prasanna Deshapriya, Ottaviano Ruesch, and the EPEC future research working group.

The field of sample return is developing rapidly around an increasing number of missions. What facilities and techniques are needed to handle such samples? Will sample return dominate other fields of planetary science? We discussed these questions and more with Dr. Enrica Bonato, who developed the Sample Return Lab at DLR and worked with samples from Hayabusa2 and legacy samples from Luna 24.

Acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany). The acceptance was attended by Dr. Enrica Bonato and Dr. Jörn Helbert (Head of the Planetary Laboratories at the DLR Institute for Planetary Research in Berlin-Adlershof). The instrument will be moved to the SAL laboratory facilities as soon as the setup of the clean room will be completed.
Sample of lunar regolith retrieved by the Soviet mission Luna24 in 1976 and donated to the Institute for Cosmos Research, which was part of the Academy of Sciences of the German Democratic Republic (GDR) during the GDR which after 1990 it became the DLR Institute for Planetary Research in Berlin-Adlershof. Credit: DLR.

Can you tell us about your academic background?

I earned my PhD in planetary science, undertaking my research jointly at the Natural History Museum (NHM) in London and the University of Glasgow. My project focused on the thermal metamorphism of carbonaceous chondrites. Following this, I took on a short postdoctoral position at the NHM, where I worked on lithium mining. I am passionate about public engagement, and I explored various outlets for this during my time at the NHM.

After completing my postdoc, I transitioned into the role of lab developer and manager for the newly established DLR sample return lab. When I started this role, there was no lab to speak of! I played a crucial role in planning and outfitting the lab in addition to getting it ready for its intended use as a sample return facility and curation center. As part of my responsibilities at DLR, I am proud to be a member of the Hayabusa 2 and MMX analysis teams.

What advice would you give to early career researchers who would be interested in a similar role to yours?

The key to securing my role as a lab developer manager was ‘delving behind the scenes’ of various instruments during my postdoc. This allowed me to become an independent user of these instruments, by becoming involved in everything from sample preparation, instrument set up and operation to data analysis. Attending numerous training events organised by instrument and software suppliers also proved invaluable experience.

For those intrigued by the prospect of joining sample return missions, I believe being in the right place at the right time is crucial. However, I suggest that early-career researchers (ECRs) with an interest in these missions reach out to existing team members. By doing so, they can explore opportunities to support the mission in various ways.

“I suggest that early-career researchers with an interest in these missions reach out to existing team members.”

Enrica Bonato

How do you see the future of sample return?

We are currently in a golden age for sample return. Multiple missions have successfully returned samples from asteroids (Hayabusa, Hayabusa2, OSIRIS-REx) and the moon (Chang’e 5) in recent years. At the same time new missions are in preparation to return samples from Mars and its moon Phobos (MMX, Mars Sample Return).

I believe that it won’t stop here. In the coming decades, we will witness sample return missions expanding to an increasing number of objects. I am particularly excited about the prospect of sample return missions from Ceres and comets. As part of the sample return mission process, we are also dedicated to enhancing the handling and analysis of samples already on Earth. The collection, transportation, and storage of samples from other planets demand a detailed understanding of material properties, necessitating a new specialisation within the field of planetary science.

“We are currently in a golden age for sample return.” 

Enrica Bonato

We can analyse samples much better in a lab on Earth than by using limited instruments on space missions. Will there be a shift towards sample return missions at the cost of traditional space missions?

Enrica Bonato carrying out acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany).
Enrica Bonato carrying out acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany). Credit: DLR..

“Sample return missions will complement other planetary science missions.”

Enrica Bonato

I believe that sample return missions will complement other planetary science missions. It’s crucial to bring a diverse array of instruments to the objects we’re interested in. On one hand, we need to assess and identify sites that are intriguing and suitable for sample return. On the other hand, we also need to conduct broader investigations of the objects to provide context for the analysis of the samples.

What are the main challenges for sample return in the coming decades?

Challenges will come from the new sample environments that we will access and new types of materials that we will sample, for example a potential future sample return mission from Venus’ surface. Building a spacecraft that can land on Venus’ extremely hostile surface and return a sample is extremely challenging. Challenges will also arise from returning a new type of sample: ice. So far the samples returned are rocks. Sampling ices from Ceres, comets or icy moons and keeping them frozen throughout cruise, the landing and later in storage on Earth brings unique challenges. Some of these technologies already exist in other fields, but a lot of new development is needed.

How did you plan the outfitting of the new sample return lab for DLR?

Dr Enrica Bonato and Dr Jörn Helbert (Head of the Planetary Laboratories at the DLR Institute for Planetary Research in Berlin-Adlershof) attending acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany). The instrument will be moved to the SAL laboratory facilities as soon as the setup of the clean room is completed. Credit: DLR

I was the only person working on this project, alongside the grant holder, who also served as my supervisor. Before my involvement, there were already some initial planning and key milestones in place. My goal was to implement and adapt this plan throughout my time at DLR. I focused on specific techniques, aiming to establish a unique and specialised niche for the lab. Considering both the institute’s requirements and the broader scientific community, I selected instruments and managed their procurement. The next step in the project would be to upgrade the lab to a curation facility.

What are the key features of a dedicated sample return lab? And how might these differ from an equivalent Earth science lab?

The features are quite similar to an Earth science lab. Analyses often take place in labs at universities or research institutes, not necessarily tailored for a particular incoming sample. One notable distinction is the need for personnel to wear lab clothing and adhere to specific standards in sample handling so as not to contaminate samples.

Does the sample return lab at DLR possess any distinctive instruments or employ unique techniques for the analysis of samples that are not currently accessible to the broader community elsewhere?

The sample holders for XRD (X-Ray Diffraction) analysis allow for preparation within a glove box and subsequent analysis of the samples without exposure to air. Additionally, another unique feature is a sample transport shuttle that facilitates vacuum conditions between the Electron Microprobe and SEM (Scanning Electron Microscope), ensuring a controlled environment for the sample.

Acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany). The acceptance was attended by Dr. Enrica Bonato and Dr. Jörn Helbert (Head of the Planetary Laboratories at the DLR Institute for Planetary Research in Berlin-Adlershof). The instrument will be moved to the SAL laboratory facilities as soon as the setup of the clean room will be completed
Acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany). The instrument will be moved to the SAL laboratory facilities as soon as the setup of the clean room has been completed. Credit: DLR.



Exciting years ahead for sample return. Thanks Enrica!

Europlanet Transnational Access on Show at ATOMKI-Hosted Workshop

May 7, 2024

Europlanet Transnational Access on Show at ATOMKI-Hosted Workshop

The HUN-REN Nuclear Research Institute (ATOMKI) recently hosted a two-day workshop on Radiation-Driven Chemistry in Astrophysics and Planetary Science. Around 45 international participants attended and discussed developments in astrochemistry and present the latest results of research. The first day finished with a round-table discussion on some of the challenges and opportunities for the astrochemistry community

Several presentations over the two days featured work carried out through the Europlanet 2024 Research Infrastructure (RI) Transnational Access programme in the ATOMKI laboratories.

Participants were given tours of both ATOMKI facilities offered fro (TA) through Europlanet, the Atomki Ice Chamber for Astrophysics/Astrochemistry (ICA) and the Atomki ECRIS Laboratory: Atomki-Queen’s University Ice Laboratory for Astrochemistry (AQUILA).

Find out more about the workshop.

Find out more about how the ATOMKI facilities have been developed through support from the Europlanet 2024 RI project.

Atomki Workshop - April 2024

Report from the Radiation-Driven Chemistry in Astrophysics and Planetary Science Workshop

(Reposted in English from the original on the ATOMKI website, with thanks to ATOMKI and the workshop organising committee.)

The HUN-REN Nuclear Research Institute (ATOMKI) recently hosted specialists researching chemical processes in outer space. The aim of the two-day event called Radiation-Driven Chemistry in Astrophysics and Planetary Science Workshop was to review the development directions of astrochemistry and to present the latest results of measurements carried out in the ATOMKI laboratories in the framework of international collaborations.

The starry sky is magical and enchanting. Humanity has been preoccupied with the regularities observed in the movement of celestial objects since its inception. In addition to observing with the naked eye, thanks to the development of technical devices, we first used binoculars and then spectroscopic (spectroscopic) methods to spy on the sky. And the space tools launched into outer space expanded our horizons and our possibilities explosively. Today, many disciplines deal with the study of our remote environment.

Astrophysics – hand in hand with astronomy – deals with the origin, history and structure of the world, the creation of chemical elements, and nuclear physical processes taking place in stars. Nuclear astrophysics research is largely carried out with the help of particle accelerators, where nuclear physics reactions are created, modeling the processes taking place in stars.

Astrochemistry studies the chemical processes taking place in outer space. How do more complex molecules form in the cradles of stars, in these very cold and distant molecular clouds, in the thin layers of ice containing atoms and smaller molecules deposited on the particles of cosmic dust? What chemical transformations take place on the surface and atmosphere of planets, moons, comets, and asteroids?

According to research, it is becoming more and more obvious that cosmic radiation and the high-energy particles emitted by stars, such as photons, ions and electrons, play a decisive role in these chemical processes. Their flow is called the stellar wind or, in the case of the Sun, the solar wind.

With the help of instruments on the ground and in space, we can also determine the chemical composition of very distant celestial bodies and nebulae. Among the hundreds of molecules detected in outer space, you can find the building blocks of living organisms, as well as larger organic molecules. Astrobiology deals with the study of the processes leading to the creation of life.

Molecules in the distant regions of outer space can be identified with the help of space telescopes (such as the James Webb Space Telescope) that use the method of radio astronomy and spectrum analysis in the infrared range (spectroscopy), and thus learn something about the chemical processes taking place there. In the closer places, within the Solar System, the probes of the space missions perform direct sampling and measurements.

However, in order to interpret the data, it is necessary to model the effect of cosmic radiation, the stellar wind, and the solar wind on molecules and thus on chemical processes here on Earth in laboratory conditions. Most of the processes taking place in the Solar System can be modeled with the help of high-energy ions and electrons created by ATOMKI’s particle accelerator equipment, ion and electron sources. Dozens of foreign groups come to the institute every year to take advantage of the facilities offered by the equipment.

With the particle beam, ices of a special composition are irradiated, such as are found on the surface of icy celestial bodies in our Solar System. Chemical changes are followed by infrared spectroscopic methods. In the research in this direction at the institute, the focus of attention is currently on the experimental modeling of the processes taking place on the icy moons of the planet Jupiter. With these experiments, ATOMKI supports the Jupiter Icy Moons Explorer (JUICE) mission of the European Space Agency (ESA).

April 25-26, 2024. The two-day meeting that took place between The majority of the 43 participating researchers came from Europe and America. The cooperating partners reported on the results of their measurements carried out in the laboratories of ATOMKI. The leading researchers of the profession analyzed the directions of the development of astrochemistry and reviewed the opportunities and challenges that arise in relation to astrochemistry in the fields of space research, space industry and climate research. The experts visited ATOMKI’s particle accelerator equipment and laboratories, where research conducted in international cooperation can continue in the future.

22-EPN3-037: Alteration and Element Mass Transfer from Source to Sink in Planetary Crusts

April 26, 2024

22-EPN3-037: Alteration and Element Mass Transfer from Source to Sink in Planetary Crusts

Virtual visit by Astrid Holzheid (Kiel University, Germany) to TA2 Facility 23 – Open University Flow Through Simulation Chambers (UK).
Dates of visit: 19-23 February 2024

Report Summary: Sound knowledge of the processes and conditions that drive hydrothermal systems is one of the prerequisites to understand not only the geological, geochemical, and geophysical evolution of our planet and other terrestrial planets, especially Mars, but also to shed light on the origin and early evolution of life since hydrothermal systems can be hospitable to certain life forms.

The use of the unique experimental set-ups of the reaction chambers at Open University allows determination of the mass transport of dissolved metals with either continuous sampling of the fluid or recirculation the fluid with built-in Ti gaze as precipitation traps. We used this set up to better understand environmental conditions during active hydrothermal alteration.

The source rocks of the experiments were fresh basalts from the Indian ocean ridge that served as analogue material to the Martian surface. The fluid was Indian ocean seawater sampled 100m above seafloor.

We observed precipitation of minerals like Ca-sulphates, NaCl, FeOOH and Fe-Mg-Na-containing clay minerals, but also native Ta and Fe-Ni-Cr alloy. While the ions of the mineral phases originated from leaching of the basalt, the metals might have come from the stainless-steel tube that served as container of the Ti gaze.

Based on the newly formed minerals, the pH – redox state – conditions can be deduced. This information is a prerequisite together with the cations enriched in the post-run fluid phase to allow geochemical reaction-path modelling which will be the next step after the post-run fluids are analysed at Kiel University.

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22-EPN3-092: Deciphering Traces of Life from the Dawn of Earth’s Biosphere

22-EPN3-092: Deciphering Traces of Life from the Dawn of Earth’s Biosphere

Visit by Nisha Ramkissooon (The Open University, UK) to TA2.2 VU (Exo)Planetary Interior Simulation Laboratory (PISL).
Dates of visit: 12-16 February 2024

Report Summary: In the search for evidence of ancient terrestrial life there are some obstacles. Purported biosignatures have been identified in a range of ancient mineral deposits, including silica. However, some of these signatures can also be generated under abiotic conditions, which brings into question their biological origin. In addition, the oldest fragments of the Earth’s crust are at least 3.8 Gyr, and would have experienced significant metamorphic alteration since their formation. Therefore, any preserved biosignatures could have also undergone extensive modification during metamorphism potentially making some of them unidentifiable. This project aimed to examine the effect of metamorphism on the modification of biosignatures preserved in silica deposits. 

Silica sinters were synthetically created in the laboratory via evaporation in the presence and absence of microbes. These samples were then exposed to simultaneous high temperature and high pressure conditions using the end-loaded piston-cylinder at the (Exo) Planetary Interior Simulation Laboratory (PISL), VU University, Amsterdam. Samples were individually subjected to pressures and temperatures of 650 °C and 12 kbar, respectively, for 20 hours. Raman spectroscopy and GC-MS will be used to assess changes in mineralogy and to quantify changes to organic molecules. Initial results obtained after returning to my home institution show that the high pressure and high temperature conditions experienced in these experiments led to changes in the crystalline structure of the samples. This resulted in samples transforming from silica glass to quartz. 

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22-EPN3-124: Unfolding Geochemical Evolution of the Subcontinental Lithospheric Mantle

22-EPN3-124: Unfolding Geochemical Evolution of the Subcontinental Lithospheric Mantle Recorded by Diamond-Forming Carbon and Water Rich (C-O-H) Mantle Fluids Throughout Time

Virtual visit by Yael Kempe and Ofir Tirosh (The Hebrew University of Jerusalem, Israel) to TA2.1 VU Geology and Geochemistry radiogenic and non-traditional stable Isotope Facility (GGIF).
Dates of visit: 9 November 2023 – 25 January 2024.

Report Summary: Fibrous diamonds from the Voorspoed, Venetia and Koffiefontein mines record deep mantle events involving C-O-H fluid types, alongside gem diamonds containing mineral inclusions that were related to modification episodes of the Kaapvaal lithospheric region. Although a connection has been made, the longstanding debate between diamond formation in the mantle and the relationship between gem diamonds and fibrous diamonds is yet to be resolved.

While we have extensive radiometric dating of mineral inclusions trapped in gem diamonds, alongside knowledge about the major and trace elements of C-O-H fluid microinclusions in diamonds, their radiogenic isotopic data is insufficient (e.g. Sr, Nd, and Pb isotopes). High-precision Sr-Nd-Pb isotope TIMS analyses of C-O-H mantle fluids in diamonds from these three prime locations in the Kaapvaal craton were preformed using a novel laser ablation diamond-in-water technique, combined with ultra-low blank column chromatography and 1013 Ohm resistors.

The team successfully processed and analysed 12 samples from Voorspoed, 5 from Venetia and 5 from Koffiefontein mines, as well as standards and blanks. The collected data show intriguing Sr-Nd-Pb relationships that vary between diamonds carrying different C-O-H fluids. The team has further data processing and calculations to complete, as well as correlate the isotopic ratios with trace element compositions to fully understand the results and their geological significance. The outcome of this Europlanet project is expected to provide new insights into the complex tectonic history of this lithospheric province, the fluids themselves and the connection between different diamond types and their formation mechanism.

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22-EPN3-063: The Origin of Early Archean Barite

22-EPN3-063: The Origin of Early Archean Barite – Insights from the Geochemical and Isotopic Composition of Associated Chert Deposits

Visit by Desiree Roerdink (University of Bergen, Norway) to TA2.1 VU Geology and Geochemistry radiogenic and non-traditional stable Isotope Facility (GGIF).
Dates of visit: 6-10 November 2023

Report Summary: The formation of bedded barite (BaSO4) deposits in the low-sulfate environments of the early Earth has been a long-standing paradox despite decades of field and geochemical studies. In this project, the team investigated the Si isotope geochemistry of chert (SiO2) dykes and beds found in association with barite to evaluate roles of hydrothermal fluids and seawater during barite formation. A total of 14 chert samples from three localities in the ~3.3 Ga Mapepe and Mendon Formations of the Barberton Greenstone Belt, South Africa were microdrilled and dissolved using sodium hydroxide digestion. Pure silicon fractions were obtained using cation exchange chromatography columns, and analysed for 29Si/28Si and 30Si/28Si isotope ratios by multi-collector inductively-coupled plasma mass spectrometry (MC-ICP-MS) in wet plasma mode using standard-sample bracketing for mass bias correction. Measured silicon isotope ratios (δ30Si) range from 0.27 to 1.29‰. Chert dykes (n = 6) and bedded cherts (n = 3) have similar silicon isotopic compositions, with an average δ30Si value of 0.88‰ for the dykes and 0.80‰ for the bedded cherts. Black chert from the Mendon formation is isotopically distinct (δ30Si = 0.45‰) from the Mapepe Formation cherts. These results tentatively suggest that the chert dykes and bedded cherts associated with barite formed from isotopically-heavy seawater (δ30Si > 0‰), and that the role of high-temperature hydrothermal fluids (δ30Si < 0‰) was limited. 

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20-EPN2-117: Exploring Mars’s Rootless Cones Based on the Geomorphometry of Icelandic Analogues

20-EPN2-117: To the Root of a Problem – Exploring Mars’s Rootless Cones Based on the Geomorphometry of Icelandic Analogues

Sebastiaan de Vet (TU Delft, Netherlands) and Lonneke Roelofs (Utrecht University, Netherlands) to TA1.1 – Iceland Field Sites, MATIS
Dates of visit: 04-12 July 2022

Rootless cones are created by steam explosions when lava flows interact with local water sources. Consequently, these landscape features offer a unique palaeo-environmental insight into the conditions at the time of the eruption. Rootless cones have also been identified on planet Mars. The aim of this project was to identify geomorphological and morphometric characteristics of Icelandic rootless cones and use these insights to infer the formation conditions and palaeo-environmental significance of rootless cones on the planet Mars. While features on Mars can only be studied remotely through satellite data, this project leverages the accessibility of lcelandic analogues to study their morphologies and properties in fine details. The rootless cone groups in the Younger Laxa Lava are uniquely and specifically suited for this purpose; they offer a morphological variety along various gradients of lava-water interactions.

During the field project the team intended to map representative rootless cones in the Younger Laxa Lava in high-resolution during a drone-assisted photogrammetric survey and analyse high-resolution Digital Terrain Models to quantitatively compare rootless cones on lceland and Mars. However, logistical issues arising in the aviation industry during Summer 2022 resulted in a temporary loss of fieldwork gear. The project was thus refocussed to carry out a field campaign to collect representative pilot-dataset to meet parts of the initial goals and prepare for a future follow-up campaign.

Banner image: A rootless cone at Myvatn Lake, Iceland. Credit: Hansueli Krapf/CC BY-SA 3.0

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22-EPN3-005: Spatial Relationship Between Biosignatures and Their Geologic Context by Large-scale Geoscientific Mapping at Rio Tinto, Spain

22-EPN3-005: Spatial Relationship Between Biosignatures and Their Geologic Context by Large-scale Geoscientific Mapping at Rio Tinto, Spain

Visit by Alessandro Frigeri (INAF, Italy) and Giacomo Panza (intern at INAF, University of Bologna, Italy) to TA1.2 Rio Tinto (Spain).
Dates of visit: 07-11 November 2023

Report Summary: Since the early 2000’s, Rio Tinto has been a critical witness plate for the investigation of extremophiles and it is recognized to be a mineralogical and geochemical analog of Mars (Amils et al., 2014). The Mars Analog Rio Tinto Experiment (MARTE), in particular, demonstrated that the Rio Tinto biosphere extends at least 900 meters below the land surface with a high potential of anaerobic microorganisms to be present (Stoker et al., 2008). Host rocks, however, are exposed at the surface in sediments and rocks of the Rio Tinto watershed, providing potential for key investigations.

The Rio Tinto 2023 field campaign was held between November 7th and November 18th 2023 at Rio Tinto Terrestrial Analogue. The campaign team was made by Alessandro Frigeri (INAF, Italy), James Skinner (USGS, US), Giacomo Panza (undergrad student at University of Bologna, intern at INAF) and Felipe Gomez as the TA Field expert (Centro de Astrobiologia, Madrid).

The campaign focused on geologic surveying and mapping the spatial relationship of the rocks where extremophile life develops today and has evolved through the geologic times. When bacteria proliferate within a solid media in a natural environment, microbial life alters the hosting environment chemically and physically. When the hosting media are soils and rocks, geological aspects like color, grain size, texture, and composition will be altered by the presence of life. Before the campaign, the team prepared a context cartographic base from remote sensing data from which they defined three sites of interest with different geological characteristics where to observe and map biosignatures.

In the field, the team applied traditional geological field large-scale mapping techniques coupled with photogrammetric drone surveys and drafted specific geoscientific mapping themes describing the geospatial setting of biosignatures at Rio Tinto Planetary Field Analogue in Spain.

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22-EPN3-77: Preservation of Organic Matter in Glacial Lakes: Implications for Martian and Icy Moon Biosignatures

22-EPN3-77: Preservation of Organic Matter in Glacial Lakes: Implications for Martian and Icy Moon Biosignatures

Visit by Charlotte Spencer-Jones (University of Durham, UK) and Sevasti Filippidou (Imperial College London, UK) to TA1.4 AU Greenland Kangerlussuaq Field Site (Greenland).
Dates of visit: 25 July – 02 August 2023

Report Summary: In the search for extra-terrestrial life, environments that have previously contained water are a key target. Glacial environments, such as those found in Greenland, are highly dynamic ephemeral systems with a range of habitat types that support many different species, from bacteria and archaea to large mammals and higher plants. Organic carbon (OC) compounds, the fundamental building blocks of life, can be used to trace different species and/or biogeochemistry. The aim of the fieldwork campaign was to characterise OC in the lake water column to establish OC synthesis patterns in glacial lakes. In this study we collected water, sediment, and soils from 13 sites from a range of lake types near Kangerlussuaq, Greenland.The second phase of this study will be to characterise organic compounds within the samples. The outcome of this work will be to establish the key parameters that control organic compound preservation with the potential to impact the interpretation of putative extra-terrestrial biosignatures.

Read the full scientific report with kind permission by Charlotte Spencer-Jones and Sevasti Filippidou.

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22-EPN3-127: Silcrete deposits of the Kalahari Desert as potential analogs for silica-rich deposits on Mars

22-EPN3-127: Silcrete deposits of the Kalahari Desert as potential analogs for silica-rich deposits on Mars

Visit by Maxime Pineau (Laboratoire d’Astrophysique de Marseille (LAM), France) and Simon Gouzy (Laboratoire de Planétologie et Géosciences (LPG), France) to TA1.5 Makgadikgadi Salt Pans (Botswana).
Dates of visit: 21-28 August January 2023

Report Summary: Hydrated silica occurs in various forms depending on the geological context and as such are good tracers for paleoenvironmental reconstitutions on Earth and Mars, as well as a prime exobiological target. Observed on Mars since the early 2000’s, hydrated silica minerals have been used to describe aqueous geological processes in diverse regions. However, geological origins of some deposits are still misunderstood because no satisfactory terrestrial analogues were found. Likewise, the exobiological potential of hydrated silica as a prime host of Mars organic matter remains to be fully ascertained.

The Makgadikgadi Salt Pans show a very high potential to be considered as a terrestrial analogue site for Mars hydrated silica, especially in fluvio-lacustrine geological settings. Maxime Pineau (LAM), Simon Gouzy (LPG), plus 2 other colleagues (Vassilissa Vinogradoff (PIIM) and John Carter (LAM)), spent 9 days at the pans (15 different locations) and sampled numerous samples (over 80s) of silicified clastic sedimentary rocks (i.e., silcretes) and conducted preliminary visible-near infrared spectra with a portable spectrometer.

Field observations and spectral analyses confirm the large amount of amorphous to (micro-)crystalline silica in the samples, along with different clays (e.g., glauconite, sepiolite) and salts (e.g., sulfates). This type of mineralogy, possibly indicating a formation in a fluvio-lacustrine context in semi-desert environments, is reminiscent of some silica-rich deposits on Mars in locations interpreted as potential paleo-lakes. These observations will be completed by further laboratory measurements (spectroscopy, microscopy, geochemical and organic analyses) in order to perform advanced studies in terrestrial geology, comparative planetology (e.g., Mars’ geology) and astrobiological exploration.

Read the full scientific report with kind permission by Maxime Pineau and Simon Gouzy.

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22-EPN3-065: Ion Bombardment of Glycine and Glycine Embedded Within Water Ice in Solar System and Interstellar Conditions

22-EPN3-065: Ion Bombardment of Glycine and Glycine Embedded Within Water Ice in Solar System and Interstellar Conditions

Visit by María Belén Maté and Ramón Javier Peláez (IEM-CSIC, Spain) to TA2.12 Atomki-Queen’s University Ice Laboratory for Astrochemistry (Hungary).
Dates of visit: 07-11 November 2023

Report Summary: The possibility that prebiotic precursors of life formed in the space and were then transported to the early Earth by comets, asteroids and meteorites is a fascinating hypothesis. We focus in this project on hydroxylamine, NH2OH, a key N-bearing species that has been proposed as an important precursor in the formation of amino acids like glycine or alanine. Very recently, hydroxylamine has been detected in the gas phase in dense clouds in the interstellar medium. It has been predicted to form efficiently on dust grains according to laboratory experiments and chemical models. Then, the presence of this species in ISM ices and on the surface of Solar System bodies is probable, and in those surfaces can react to form more complex prebiotic species like amino acids.

Although the chemical pathways leading to the formation of NH2OH in astrophysical ices have been thoroughly studied, the next step in the chemical evolution that would begin with NH2OH as a precursor in ice has, to our knowledge, not been addressed experimentally.

In this TA project the team studied the chemistry induced by Cosmic Rays on ices containing hydroxylamine. They studied pure NH2OH ices and mixtures with H2O, CO and D2O, at 20 K, irradiated with 15 keV H+ ions. In particular, we were interested in finding complex organic molecules in the processed ices, and learning how different ice composition affects the chemistry and the destruction efficiency of NH2OH by Cosmic Rays.

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22-EPN3-065: Ion Bombardment of Glycine and Glycine Embedded Within Water Ice in Solar System and Interstellar Conditions

22-EPN3-065: Ion Bombardment of Glycine and Glycine Embedded Within Water Ice in Solar System and Interstellar Conditions

Visit by Alfred Hopkinson (Aarhus University, Denmark) to TA2.12 Atomki-Queen’s University Ice Laboratory for Astrochemistry (Hungary).
Dates of visit: 04-08 December 2023

Report Summary: During this TNA visit, the simplest amino acid glycine (NH2CH2COOH), and its deuterated analogs, partially deuterated d3-glycine (ND2CH2COOD) and fully deuterated d5-glycine (ND2CD2COOD), were irradiated using 10 KeV protons. The subsequent products of this processing were then measured using infrared spectroscopy and a quadrupole mass spectrometer. The aim of this was to investigate the products of glycine destruction and investigate if this energetic processing could result in the formation of glycine peptides. The outcome of the TNA visit was the collection of infrared spectra of the irradiation of these molecules and then following this, temperature-programmed desorption measurements. These preliminary results show the formation of CO2, CO, and D2O.

Full scientific report published by kind permission of Alfred Hopkinson.

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22-EPN3-053: Proton Processing of Phenanthrene Ice Mixtures for Application to Titan’s Lower Atmosphere

22-EPN3-053: Proton Processing of Phenanthrene Ice Mixtures for Application to Titan’s Lower Atmosphere

Visit by Alessandra Candian and Annemieke Petrignani (University of Amsterdam, Netherlands) to TA2.11 Atomki Ice Chamber for Astrophysics / Astrochemistry (ICA) (Hungary).
Dates of visit: 4-8 March 2024

Report Summary: During this TNA visit, the three-ring PAH phenanthrene (C14H10), acetonitrile (CH3CN) and their 1:1 mixture were irradiated using 10 KeV protons. The subsequent products of this processing were then measured using infrared spectroscopy (5000-700 cm-1) and a quadrupole mass spectrometer.

The aim of these experiments was to investigate 1) if energetic processing can modify the structure of solid hydrocarbons and 2) if proton irradiation could trigger the formation of new species. During the visit to Atomki, the team collected infrared spectra of at different proton fluences and then following this, infrared spectra during temperature-programmed desorption (TPD). They also obtained the residues after TPD for ex-situ analysis. The preliminary results show a) the puckering of phenanthrene solid, b) the formation of ethanimine (C2H5N) in acetonitrile solid, c) a complex behaviour of the 1:1 mixture, with puckering and formation of new hydrocarbon species.

Full scientific report published by kind permission of Alessandra Candian and Annemieke Petrignani.

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22-EPN3-091: Evolution Under Radiation of Organics Pertaining to Europa

22-EPN3-091: Evolution Under Radiation of Organics Pertaining to Europa

Visit by Alexis Bouquet (Aix-Marseilles University, France) to TA2.11 Atomki Ice Chamber for Astrophysics / Astrochemistry (ICA) (Hungary).
Dates of visit: 19-24 February 2024

Report Summary: Several of the icy moons of Jupiter possess a liquid water ocean under a thick icy crust. In the especially promising case of Europa, a young surface (>100 Myr), and likely recent cryovolcanicactivity (within the last 8 years) imply the presence of ocean material on the surface. Therefore, observations performed by space missions could determine the ocean’s composition, and derive indications on its potential habitability (presence of chemical gradients providing metabolic energy, quantity and composition of available organic matter…). Characterising Europa’s ocean and its possible habitability requires to understand processes that alter organic and inorganic molecules in this environment. These processes include the processing by energetic ions coming from Jupiter’s magnetosphere and hitting the surface.

In this project, Alexis Bouquet visited the Atomki facility to study the effect of sulfur ion bombardment on methanol, a species that could be indicative of key characteristics of the ocean, pure and within an ice matrix. The alteration of the sample was followed using infrared spectroscopy, and the resulting complex organic residues were retrieved for ultra-high resolution mass spectrometry.

Full scientific report published by kind permission of Alexis Bouquet.

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20-EPN2-090 – A Search for Thiols Formation Pathways Under Space-Relevant Conditions

20-EPN2-090 – A Search for Thiols Formation Pathways Under Space-Relevant Conditions

Visit by Zuzana Kaňuchová (Astronomical Institute of the Slovak Academy of Sciences, Slovakia) and Tom Field (Queen’s University Belfast, UK) TA2.11 Atomki Ice Chamber for Astrophysics / Astrochemistry (ICA) (Hungary).
Dates of visit: 27 November – 8 December 2023

Report Summary: Despite being only the tenth most abundant element in space, sulfur is a component of several biomolecules, making it a key subject for astrochemistry studies. Sulfur containing molecules were observed in the solid phase on the surfaces of icy moons and in the icy mantles of interstellar grains. Despite the seemingly ubiquitous detection of sulfur-bearing species in space, the sulfur budget is still puzzling the scientific community. To address this, Zuzana Kaňuchová and Tom Field conducted an exploratory series of irradiation experiments to determine if species with thiol (-SH) groups may be formed in hydrocarbon-rich ices at temperatures relevant to interstellar matter, the surfaces of Solar System icy satellites, and Kuiper Belt objects.

They implanted 200 keV S+ ions in methane (CH4), ethane (C2H6), ethene (C2H4), and ethyne (C2H2) ices at 20 K and 60 K. Formation (and destruction) of species was monitored via FTIR spectroscopy and quadrupole mass spectrometry. Based on preliminary analysis performed during the TA they decided to conduct one extra (supplementary) experiment to explore the possibility of forming carbon and sulfur-bearing molecules by implanting high-energy carbon (750 keV) ions into hydrogen sulfide (H2S).
The preliminary analysis does not indicate the formation of thiols in the investigated hydrocarbon ices as a result of high-energy sulfur ions implantation. However, several new absorption bands appeared in the
spectra of all irradiated hydrocarbons, indicating the formation of various alkanes and alkenes. The emergence of a prominent band around ~1600 cm-1 could suggest the presence of carbon in an amorphous form.

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22-EPN3-028 – Energetic Ion Processing of Pyrene Ice

22-EPN3-028 – Energetic Ion Processing of Pyrene Ice

Visit by Alicja Domaracka (CIMAP-CNRS, France) and Anna Bychkovato (Normandie Université, France) TA2.11 Atomki Ice Chamber for Astrophysics / Astrochemistry (ICA) (Hungary).
Dates of visit: 16-20 October 2023

Report Summary: Over the last decades it became clear that we live in a “molecular universe”. Carbon forms the basis of the majority of the molecular species that so far have been identified in space. Although small carbon-based molecules, like CO and CO2, are some of the most abundant molecules in space, only a small fraction of the carbon is expected to be locked up in such species. It was proposed that a large portion of the interstellar carbon, up to 20%, is built in polycyclic aromatic hydrocarbons (PAHs) and fullerenes. There is a clear lack of information about interaction of energetic ions with pyrene in the solid phase.

In January 2022, Alicja Domaracka (CIMAP-CNRS, France) and Anna Bychkovato (Normandie Université) performed irradiations of pure pyrene 20 K by protons and carbon ions at the ATOMKI facility. Within the present TA, they studied pure pyrene ice at 20K irradiated with 6.4 MeV S3+, 4 MeV S2+, 2,4 MeV C2+, 400 KeV He+, 800 keV He+ and 800 keV H+ ion beams, respectively. In particular, we are interested in learning how the pyrene destruction cross sections depend on the projectile parameters (atomic number, energy).

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20-EPN2-116: Hypervelocity Impacts for DISC Calibration

March 11, 2024

20-EPN2-116: HIDISCC (Hypervelocity Impacts for DISC Calibration)

Visit by Vincenzo Della Corte, Osservatorio Astronomico Capodimonte Napoli, INAF (Italy), to TA2.7 Light Gas Gun Laboratory, University of Kent (UK)
Dates of visit: 27-29 March 2023

Report summary: The Comet Interceptor space mission is to launch in 2029 to study a dynamically new comet. Two of the three spacecraft involved will host copies of the Dust Impact Sensor and Counter
(DISC), which will measure the physical properties of cometary dust. The spacecraft’s velocity (7-70 km/s) will result in hypervelocity dust impacts on DISC. Combined with the range of dust particle sizes, this will create a wide range of impact momentum (10-11–10-3 kg/m/s). To cover the upper part of the momentum range, DISC calibration will be performed with hypervelocity simulated impacts induced by lasers. To perform DISC characterization and calibration in the lower momentum range, we carried out experiments at the Light Gas Gun Impact Facility at the University of Kent (UK).
To calibrate DISC and check the sensing element formed by the aluminum plate and the
piezoelectric transducers:

  • We performed 9 shots at the Light Gas Gun Impact Facility at the University of Kent.
    We used different particle sizes and materials and different speeds, utilising different
    approaches, i.e. single particles with diameters down to 400 nm and buck-shots of a
    mixture of minerals and very light hollow spheres.
  • The signals from the piezoelectrics will be used to verify DISC estimated
    performance and enable a generally-valid impact sensor calibration procedure.
    All 9 shots provided signals, this was for both single impacts and multiple buck- shot impacts.
    The results of the experiment confirmed the capability of the instrument to measure the
    momentum of particles impacting in the hypervelocity range.

Read the full scientific report, with kind permission from Vincenzo Della Corte.

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22-EPN3-006: An Isotopic Inventory of Mars analogue environments

February 11, 2024

22-EPN3-006: An Isotopic Inventory of Mars analogue environments

Visit by Michael Macey and Daniel Loy (OU, UK) to TA1.5 Makgadikgadi Salt Pans (Botswana).
Dates of visit: 17-25 January 2024

An international team of scientists from The Open University (OU) and the Botswana International University of Science and Technology (BIUST) conducted fieldwork across the Makgadikgadi Basin. The aim of the research conducted was to collect sediment cores and water samples to assess how viability of sulfur-cycling microbes varies across a gradient of salinities, desiccation, and UV-exposure, and how this might impact the formation of biosignatures. The timing of the trip allowed sampling across a spectrum of fluctuating environmental stressors in terms of the availability of water. During the trip, a total of 16 x 30 cm cores were collected for geochemical and microbiological characterisation. Furthermore, environmental variables were taken with pH, temperature, conductivity, redox potential, and UV monitored.  The trip was a success, with the collection of ideal samples to identify the relative abundance and diversity of sulfur cycling microbes across this analogue environment. 

Read the full scientific report with kind permission by Michael Macye and Daniel Loy.

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20-EPN2-098: Constraining the Thermal History of Water-Rich Asteroids Using Noble Gas Analysis of Heated CM Chondrites

January 23, 2024

20-EPN2-098: Constraining the Thermal History of Water-Rich Asteroids Using Noble Gas Analysis of Heated CM Chondrites

Visit by Ashley King and Helena Bates (Natural History Museum, UK) to TA2.15 ETH Zurich Geo- and Cosmochemistry Isotope Facility (Switzerland).
Dates of visit: 28 November – 08 December 2022

Report Summary:

In this TA visit, the team investigated the abundance and isotopic composition of noble gases (He – Xe) in CM chondrites that record both aqueous and thermal metamorphism. These unusual meteorites are likely good analogues for the types of material found on the surfaces of primitive C-type asteroids; however, the timing and mechanism of the metamorphism remains unknown.

The team measured He – Xe in five CM chondrites that experienced peak metamorphic temperatures of <300°C to >750°C using stepped-heating and the “ALBATROS” mass spectrometer at the ETH Zürich Geo- and Cosmochemistry Noble Gas Laboratory. Preliminary results show that the concentrations of 4He and 22Ne are depleted in the lowest temperature steps (300 and 450°C) for all samples, consistent with degassing during (a) metamorphic event(s). Peaks in the concentration of both light and heavy noble gases in the 660°C and 800°C steps agree with previous estimates of metamorphic temperatures based on mineralogy and H2O loss. Isotopic compositions are mainly a mixture of primordial (so-called Q/HL) and cosmogenic components. In addition, EET 96029 and WIS 91600 contain a trapped solar wind component, suggesting that these meteorites may have been heated by impacts during residence in the asteroid regolith. Comparison of the data to unheated CM chondrites will be used to further constrain the thermal history of C-type asteroids in the early Solar System.

Read the full scientific report with kind permission by Ashley King and Helena Bates.

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22-EPN3-019: Investigation of Ceres Bright Spots

22-EPN3-019: Investigation of Ceres Bright Spots – VIS-NIR Spectral Simulation of Haulani bright Areas by Means of Spectral Analysis on Produced Analogue Mixtures

Visit by Fabrizio Dirri and Giuseppe Massa (INAF-IAPS, Italy) to TA2.8 CSS (Cold Surfaces Spectroscopy) at IPAG (France).
Dates of visit: 22 May – 03 June 2023

Report Summary: In this project different bright areas of Haulani crater (i.e. Southern floor and Central Crater Peak, named ROI3 and ROI1) on Ceres have been studied by producing different analogue mixtures starting from previous results and comparing them with Dawn VIR data. The end-members have been identified based on previous studies (Tosi et al. 2018, Dirri et al. 2022) and the analogue mixtures have been produced with grain size 50-100 µm. The two initial mixtures, i.e. SF1 and CCP_#1 have been acquired in the VIS-NIR spectral range (0.4-4.5 µm) at T environment. The Band Center, Band Depth and FWHM of absorption bands at 2.7, 3.1, 3.4 µm, spectral slope (1.2-1.9 µm range) and reflectance level at 2.1 µm of the produced SFs and CCPs mixtures have been analysed and then compared with VIR data.

The best analogues are the SF_#5 and CCP_#6 mixtures and their spectra have been acquired at low temperatures, i.e. from 190K to 230K, similar to Haulani base temperature by using Cold Spectroscopy Facility (CSS) (IPAG, France). These mixtures exhibit values for the 2.7BD (Antigorite, Illite), 3.1BD (NH4-Montmorillonite) and 3.4 BD (NaCO3) similar to Haulani ROI3 and ROI1. In particular, different dark components have been used (i.e. magnetite plus carbon black) with the aims of better reproducing the Haulani spectral slope and reflectance level. Different carbonates mix involving trona, dolomite, hydrous and anhydrous natrite have been studied to assess their contribution to 2.7 µm spectral band and the three minima at 3.33, 3.42, 3.52 µm of Haulani ROI3.

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22-EPN3-038: Asteroidal source(s) of L chondrites and its collisional evolution

22-EPN3-038: Asteroidal source(s) of L chondrites and its collisional evolution – U,Pb geochemistry of phosphates in meteorite Antonin.

Visit by Monika Kusiak (Institute of Geophysics Polish Academy of Sciences (IG PAS), Poland) and Agata Krzesinska (University of Oslo) to TA2 Facility 26 – KBSI Sensitive High Resolution Ion MicroProbe / SHRIMP-IIe/MC (South Korea).
Dates of visit: 12-23 May 23

Report Summary: The main goal of the visit was to conduct in-situ U-Pb geochronological study of phosphate minerals in the Antonin L chondrite. Fall of the Antonin, on 15th July 2021, was recorded by European Fireball Network, and this recording led to reconstruction of the pre-atmospheric orbit of meteoroid. The orbital parameters of the Antonin differ from reconstructed orbits of other L chondrites, but suggest it was sourced from the inner asteroid belt. To track the orbit to the parent body, it is important to understand dynamic collisions experienced, which are recorded in minerals of the meteorite. U-Pb dating allows to decipher details on events that led to resetting of phosphates.

During the visit to KBSI facility, we collected SHRIMP (Sensitive High-Resolution Ion MicroProbe) analyses within multiple apatite and merrillite grains. Initial U-Pb results show minor discordance of ages of phosphates, indicating a mild collision after the crystallization of the minerals. The timing of reset event cannot be inferred with high precision, but it likely occurred between 500–100 Ma.

Additionally, formation of phosphates can be well constrained from collected data at ca. 4450 Ma. This age implies that phosphates formed/recrystallized in response to a collision as impacts were the only source of heat after cessation of accretional activity. Altogether, the results suggest two collisions in the evolution of parent body and will be combined with further data to pinpoint key events in dynamical evolution of parent body of L chondrites.

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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.