The total solar eclipse of 12 August 2026, visible along a path crossing the Russian Arctic, Greenland, Iceland, Portugal, and Spain, will provide an exceptional opportunity for both scientific observations and public engagement. As part of a broader observing campaign [1] (that includes observations from various sites along the path), a group of early career scientists will conduct a set of complementary experiments aimed at obtaining scientifically useful measurements, engaging wider society, and preparing observational strategies for the 2027 total solar eclipse. The optical experiments will include white light imaging of the solar corona using telescopes with different focal lengths. Our wide field setup will be used to image the corona from our observing site during totality. These observations will later be combined with measurements obtained by other sites within the broader campaign, enabling multi-site image stacking and the construction of a temporal sequence of the corona during totality [1,2]. A longer focal length setup will be used to carry out a modern version of the Einstein–Eddington experiment by measuring the apparent positional shifts of stars close to the eclipsed Sun, caused by gravitational light deflection. In addition, sky spectra will be recorded at different eclipse phases to study how the integrated sky spectrum changes as direct photospheric light is suppressed and the corona becomes visible [3,4]. The campaign will also include ionospheric experiments using radio observations and GNSS based measurements. Very low frequency and low frequency radio receivers will monitor stable transmitters before, during, and after the eclipse. Changes in received signal strength and propagation conditions can be used to probe eclipse driven changes in the ionosphere caused by reduced solar ionization. In parallel, GNSS data from personal phones and, where available, dedicated receivers will be collected to investigate possible changes in signal strength, positioning residuals, and ionospheric delay proxies. These measurements will be designed as a citizen science activity, allowing the public to contribute geographically distributed data. The observing site and activities will be announced publicly. Outreach will include safe solar viewing, solar projection demonstrations, sunspot observations, distribution of eclipse glasses, and explanations of the science behind the experiments [2,5]. In this way, the campaign will combine eclipse science, public participation, and training for future total eclipse observations. References:[1] Schmieder, B., Baratashvili, T., Poedts, S., Lani, A., Wang, H., Foing, B., Sansari, S., Zeegers, S., Pascual, J., Nahum, R., Nagainis, K., Gomez de Castro, A. I., and Heras, A.: Total Eclipse on August 12, 2026: observations in Spain and prediction with COCONUT, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-1542, https://doi.org/10.5194/egusphere-egu26-1542, 2026.[2] European Space Agency, “Solar Total Eclipse 1999,” ESA Science & Technology, 1999. Available: https://sci.esa.int/web/observational-astronomy/-/38064-total-eclipse-99[3] B. H. Foing, L. Duvet, L. Ligot, J. Oliveira, T. Beaufort, J. E. Wiik, B. Altieri, N. Henrich, S. Cravatte, and E. Maurice, “Results from the 3 November 1994 Solar Eclipse: Density and Temperature Variations in Streamers and Coronal Holes,” in The Tenth Cambridge Workshop on Cool Stars, Stellar Systems and the Sun, ASP Conference Series, vol. 154, R. A. Donahue and J. A. Bookbinder, Eds. San Francisco, CA: Astronomical Society of the Pacific, 1998, p. 1035.[4] B. H. Foing, L. Duvet, K. Muglach, J. E. Wiik, T. Beaufort, and E. Maurice, “Polar plumes and streamers from 1994 and 1998 eclipses,” in Solar Jets and Coronal Plumes, ESA SP-421, 1998, p. 273.[5] European Space Agency, “Solar Eclipse Index,” ESA Multimedia, 1 July 1999. Available: https://www.esa.int/ESA_Multimedia/Videos/1999/07/Solar_Eclipse_Index

Distinguishing galaxies as either fast or slow rotators plays a vital role in understanding the processes behind galaxy formation and evolution. Standard techniques, which are based on the λR spin parameter obtained from stellar kinematics, frequently face difficulties in classifying fast and slow rotators accurately. These challenges arise particularly in cases where galaxies have complex interaction histories or exhibit significant morphological diversity. In this paper, we evaluate the performance of a Convolutional Neural Network (CNN) in classifying galaxy rotation kinematics based on stellar kinematic maps from the SAMI survey. Our results show that the optimal CNN architecture achieves an accuracy and precision of approximately 91% and 95%, respectively, on the test dataset. Subsequently, we apply our trained model to classify previously unknown rotator galaxies for which traditional statistical tools have been unable to determine whether they exhibit fast or slow rotation, such as certain irregular galaxies or those in dense clusters. We also used Integrated Gradients (IGs) to reveal the crucial kinematic features that influenced the CNN’s classifications. This research highlights the power of CNNs to improve our comprehension of galaxy dynamics and emphasizes their potential to contribute to upcoming large-scale Integral Field Spectrograph (IFS) surveys.

6500+ exoplanets have been detected using various techniques. This prompted the emergence of many recent works on the taxonomy, or classification, of exoplanets. However, there is still no basic, fundamental definition of 'What is a planet?'. IAU has forwarded a definition in 2006, which however, raised more questions than it solved. The first task here is to establish if there are limits on the size/mass of planets. The lower mass limit may be assumed as of Mimas (0.03 EU) - approximately minimum mass required to attain a nearly spherical hydrostatic equilibrium shape. The upper mass limit may be easier - there is a natural lower limit to what constitutes a star: 0.08 SU. But then there are brown dwarfs: IAU has defined brown dwarfs as objects exceeding the deuterium burning limit ( 13 JU), and giant exoplanets generally have masses of 0.3 to 60 JU. The resolution requires assembling the basic physical parameters that define planets quantitatively. Mass and radius are the two fundamental properties, and we propose to use a third correlated parameter: the moment of inertia. Based on this, we create the parametric Fundamental Planetary Plane where the two parameters are correlated with the third. The fundamental planetary plane (FPP) with turn-off point diagrams is constructed for visual representation. We propose an alternate potential description of a planet definition as 'A celestial spherical object, bound to a star or unbound, that lies on the fundamental planetary plane, within a mass range between 0.02 EU to 13 JU'. This definition is intended to complement existing taxonomies by providing a quantitative, structure-based criterion applicable to both Solar System planets, exoplanets and free-floating planets. These turn-off point diagrams serve as an alternative to the Hertzsprung-Russell (HR) diagram, but for planets.

The extreme lighting conditions on the Moon present significant challenges to the astronaut visual system. This study uses virtual reality (VR) technology to build a high-fidelity lunar lighting model and combines eye-tracking technology to explore visual adaptation mechanisms under dynamic lighting conditions. Thirty healthy participants completed geometric shape recognition tasks under four different lighting change speeds (1/5/10/15 s), resulting in 480 valid trials, which provided data on behavioral performance, eye movement characteristics, and subjective perception. The results indicate that rapid lighting changes increase astronauts' visual load, leading to reduced recognition efficiency and accuracy, requiring more time to perceive the environment. In contrast, slower lighting changes alleviate visual load, improving information recognition accuracy and response speed. The slower the lighting change speed, the better the performance in information recognition tasks. Thus, slow lighting changes can help astronauts process information and execute tasks more effectively. This paper provides insights for human-computer interaction design and astronaut task settings in lunar environments.

This study examines the mineral composition of volcanic samples similar to lunar materials, focusing on olivine and pyroxene. Using hyperspectral imaging (HSI) from 400 to 1000 nm, we created data cubes to analyze the reflectance characteristics of samples from Vulcano, a volcanically active island in the Aeolian archipelago, north of Sicily, Italy, categorizing them into nine regions of interest (ROIs) and analyzing spectral data for each. We applied various unsupervised clustering algorithms, including K-Means, hierarchical clustering, Gaussian mixture models (GMMs), and spectral clustering, to classify the spectral profiles. Principal component analysis (PCA) revealed distinct spectral signatures associated with specific minerals, facilitating precise identification. The clustering performance varied by region, with K-Means achieving the highest silhouette score of 0.47, whereas GMMs performed poorly with a score of only 0.25. Non-negative matrix factorization (NMF) aided in identifying similarities among clusters across different methods and reference spectra for olivine and pyroxene. Hierarchical clustering emerged as the most reliable technique, achieving a 94% similarity with the olivine spectrum in one sample, whereas GMMs exhibited notable variability. Overall, the analysis indicated that both the hierarchical and K-Means methods yielded lower errors in total measurements, with K-Means demonstrating superior performance in estimated dispersion and clustering. Additionally, GMMs showed a higher root mean square error (RMSE) compared to the other models. The RMSE analysis confirmed K-Means as the most consistent algorithm across all samples, suggesting a predominance of olivine in the Vulcano region relative to pyroxene. This predominance is likely linked to historical formation conditions similar to volcanic processes on the Moon, where olivine-rich compositions are common in ancient lava flows and impact-melt rocks. These findings provide a deeper context for mineral distribution and formation processes in volcanic landscapes.

This study investigates the impact of mixed-reality (MR) interface background colors on cognitive performance and subjective workload in a simulated space emergency scenario. Thirty-five participants performed a modified Space Stroop task under five different MR background colors: red, green, blue, yellow, and white, with response times, task accuracy, and perceived cognitive load assessed. The results revealed significant differences in response times, with participants demonstrating the best performance under the yellow background, exhibiting faster response times and higher accuracy compared to the other colors. While no significant correlation was found between response times and accuracy, yellow backgrounds appeared to offer a cognitive advantage, likely due to improved visibility and reduced cognitive load. Subjective workload assessments using the NASA Task Load Index (NASATLX) indicated that participants experienced lower cognitive demand and frustration with the yellow interface. These findings suggest that yellow MR backgrounds may optimize performance and emotional stability during high-stress tasks, such as emergency repairs in space. Further analysis revealed no significant learning or fatigue effects, strengthening the conclusion that background color was the primary driver of performance differences. The study highlights the potential for yellow MR backgrounds to enhance astronaut efficiency and decision-making during space missions, providing a foundation for future interface design recommendations. Future research should explore individual differences in color perception and test these results in real-world space environments to further validate the findings.

In response to the growing importance of space exploration, the objectives of the COSPAR Panel on Exploration (PEX) are to provide high quality, independent science input to support the development of a global space exploration program, to promote space sciences as a key element of this program, to contribute to maximize its scientific return via enhanced international cooperation, and to take action to safeguard the scientific assets of solar system bodies. This paper summarizes the presentations of the two panel sessions at the COSPAR assembly 2024 and identifies the most intensely discussed recent topics of interest or concern for space exploration. These topics include environment stewardship of celestial bodies, space debris, resource utilization, the Moon, Mars, and other celestial bodies that we want to explore with planetary protection measures, preservation of dark and quiet skies, potential atmospheric pollution, space as an independent goal of sustainable development, human spaceflight, agile and affordable space programs, and the early preparation of a new edition of the COSPAR exploration roadmap.

The Atacama Desert and the Puna (an ecoregion of the Central Andes that mainly straddles three South American countries, Argentina, Bolivia and Chile, with altitudes ranging from 3500 to 4800 meters above sea level [masl] see. Figure 1) have extreme terrestrial environmental characteristics that make these two geographic locations potential analogs of the conditions that Mars may have experienced during its geological history [1,2].Figure 1 : Geographical landmark / Bottom left, Zoom in on the campaign area with sampling points present (Copyright : Google Earth)The University of Atacama (UDA) located in Copiapo (27º37S / 70º33W) in Chile, aims to conduct multidisciplinary studies to better characterize the extreme environment of the Puna de Atacama. This project is based, in particular, on the forthcoming implementation of a high-altitude laboratory located at 3800 masl in the vicinity of the Salar de Maricunga (26º92S / 69º08W) [3]. The construction of this high-altitude laboratory should enable the scientific exploration of the region to be strengthened. Moreover, in order to benefit from expertise in the field of planetary analogs, the UDA has approached the EuroMoonMars program [4], which has more than ten years of experience in organizing analog field campaigns. This partnership in the making has taken shape with the setting-up of a first joint expedition at the end of February/beginning of March 2021. This expedition was organized by the Cryosphere and Water laboratory of the UDA (LICA) and has also been supported remotely by members of the EuroMoonMars program. During this high-altitude 10-days campaign (between 3800 and 6500 masl) the geographical extend included the Salar de Maricunga (26º92S / 69º08W), the Tres Cruces (27º07S / 68º79W), the Laguna Verde (28º88S / 68º47W) and finally the Ojos del Salado areas (27º11S / 68º54W) (see. Figure 1), whose potential as a Martian analog has been highlighted in recent publications [5]. To the initial objectives related to environmental sciences, scientific, technical, logistical and medical protocols specific to planetary science and space exploration were added, as the first steps towards for the organization of more complex campaigns involving EuroMoonMars people in the field. According to the multidisciplinary perspective of characterizing the environment of the Puna de Atacama and in addition to geophysical work, soil, water and biological material sampling was carried out along an altitudinal gradient (see. Figure 1). This study aims to review the preliminary results of these samples, notably via the geochemical analysis of the soils (carried out using Inductively Couple Plasma spectrometry (ICP) and X-fluorescence spectroscopy) contextualized in the perspective of considering the Puna de Atacama as a Martian analog. Acknowledgments: The authors would like to thank the people involved in the success of this project, which aims to both promote and protect the incredible natural heritage of the Puna de Atacama region. References: [1] Navarro-González, R. et al. (2003) Science, 302(5647), 1018-1021. [2] Schmidt, S. K. et al. Antonie van Leeuwenhoek, 111(8), 1389-1401. [3] Tavernier, A. et al. (2021) 52nd LPSC conference 15-19 March, 2021. LPI Contribution No. 2548, id.2253.[4] Foing, B. et al. (2020) p. EPSC2020-14. [5] Kereszturi, Á. et al. (2020) Astrobiology, 20(6),677-683.

In May 2021, a group of students and young professionals from EuroMoonMars will construct a lunar-analogue habitat inside a lava tube in Iceland, known as CHILL-ICE.As a preparation for semi-permanent humanned missions to the lunar surface, analogue field tests on Earth will greatly improve the chance of a mission success. Looking at prospective habitat locations in or on the lunar surface, lava tubes may present an excellent opportunity in terms of safety and efficiency. These locally occurring features provide a rigid structure with a solid ground, and therefore offer protection from radiation, temperature variations, regolith, and micrometeorite impacts [1]. Furthermore, the unaltered rocks and minerals inside lunar lava tube systems will grant a unique insight into the origin of the Moon, and with that, the Earth [2].Lava TubesLava tubes on Earth are most commonly found in areas with deep-mantle volcanic activity, such as ‘hot spots’: places where mantle plumes arrive at the surface (Hawaii, Iceland, Canary Islands). Geochemically speaking, the basaltic rocks present at these locations on Earth are quite comparable to their lunar counterparts in major element compositions. As most of the larger lava tubes on Earth are located on oceanic islands, they are highly suited to explore the psychological factors of being remotely distanced from the rest of the Earth. Colder regions, such as on Iceland or at the high peaks of Mauna Loa on Hawaii, are preferred for analogue habitats due to less biochemical weathering of the environment. The high latitude of Iceland further aids the lunar-day simulation aspect of an analogue habitat, as there can be over 20 hours of sunlight in the summer, and only 4 hours of sunlight in the winter. The EuroMoonMars and future EXTAR teams are therefore planning to set up a lunar-analogue habitat inside a lava tube on Iceland. Earlier campaignsIn September 2018, a reconnaissance campaign was organized to scout multiple lava fields across Iceland for their suitability to host a lunar analog habitat [3]. The most promising site found was the Surtshellir-Stefanshellir cave system in the Hallmundarhraun lava flow in the Western part of Iceland, see Figure 1. At the easternmost part of the Stefanshellir lava tube, there is a large open gallery with a relatively flat surface within the tube. This would be an optimal location for the construction of a lava tube habitat.Figure 1: Location of the Stefanshellir cave system. Top left image shows the location in Iceland, top right shows the Hallmundarhraun lava field (in light yellow). Bottom right shows an overlay of the Stefanshellir cave system as drawn by J.R. Reich jr., in 1975, over aerial footage. Upcoming scout missionThis year a follow-up scout mission to the lava tube systems of Hallmundarhraun is planned for the 28th of June until the 4th of July 2020. The main goal is to investigate the lava tube and its direct surroundings into a much greater detail. Inside Stefanshellir, the aim is to make at least two 180-degree 3D movies for a virtual walkthrough tour, take precise measurements of the dimensions of the gallery, and 360 degrees pictures for a model. On the surface, the focus lies on making aerial maps to scout for visible signs of the subsurface lava tubes [4] and setting up communications and solar observational antennae.Besides investigations regarding the lunar analog mission, geological fieldwork to the lava field will be performed to create a clearer reconstruction between Stefanshellir and other lava tubes within Hallmundarhraun. Directly located to the east of Stefanshellir, lies Surtshellir, a maze-like cave that is unlikely to have formed in one event. Another lava tube is located directly to the west, called Hulduhellir, or “secret cave” [5], as it has no openings to the surface and is known only through ground penetrating radar and magnetometric studies. There are in total another seven lava tubes in the lava flow confirmed and discovered thus far, but it is likely that there are other, still pristine and unopened lava tubes yet to be found. Simulation missionThe final lunar analog habitat will be constructed end of May 2021. Besides earlier campaign objectives, the simulation mission will focus on the feasibility of setting up a lunar tube habitat in-sim. This means that the habitat should be deployable by four astronauts in a tight and possibly dark environment within ten hours. Other instruments will be deployed out of simulation, this would compare to the deployment of instruments via robotic missions in earlier stages of lunar habitation. Figure 2 provides a rough overview sketch of some crucial instruments used in the simulation mission.Figure 2: Rough sketch of the planned base for the CHILL-ICE campaign in May 2021. The subsurface habitat’s shape is still to be determined and will not (yet) include any large life support systems, such as greenhouses or water replenishment systems. On the surface, several instruments will be deployed out-of-simulation; comparable to robotic deployment in lunar missions. Even with a lightweight, partially inflatable, habitat, this is expected to take up the largest part of the first mission. From the ten days set out for the campaign, only two and a half day will be spent in simulation; the rest of time will be to conduct further research to the terrain and its origin, other ISRU objectives, drone mapping, communication protocols, solar observations, (aerial) gravimetric, LIDAR, and magnetometric studies, and of course training in setting up the habitat locally in an efficient and safe manner.We would like to thank Space Iceland, 4th Planet Logistics, Prof. Bernard Foing, EuroMoonMars, and ILEWG for their great support during our campaign.[1] M.V. Heemskerk et al., LPSC50, #1693, (2019)[2] C.L. York et al., LPI Joint Workshop on New Technologies for Lunar Resource Assessment, (1992)[3] M.V. Heemskerk et al., EGU2019-17503-1, (2019)[4] P. Lee et al., LPSC50, #3118, (2019)[5] C. Wood et al., Expedition Report Hallmundarhraun 2003 Iceland, (2004)

This study presents a comprehensive evaluation of various classification algorithms used for the detection of exoplanets using labeled time series data from the Kepler mission. The study investigates the performance of six commonly employed algorithms, namely Random Forest, Support Vector Machine, Logistic Regression, K-Nearest Neighbors, Naive Bayes, and Decision Tree. The evaluation process involves analyzing a dataset that consists of time series measurements of star brightness, accompanied by labels indicating the presence or absence of exoplanets. To assess the effectiveness of each algorithm in accurately identifying exoplanets, performance metrics such as accuracy, precision, recall, and F1 score are employed. The results demonstrate that the Random Forest algorithm achieves the highest accuracy of 94.2%, followed closely by the Support Vector Machine with 93.8 percent accuracy. The Logistic Regression algorithm achieves an accuracy of 91.5 percent, while the K-Nearest Neighbors, Naive Bayes, and Decision Tree algorithms achieve accuracies of 89.6%, 87.3%, and 85.9% respectively. Furthermore, the precision, recall, and F1 score metrics provide insights into the strengths and weaknesses of each classifier. The Random Forest algorithm exhibits a precision of 0.92, recall of 0.95, and F1 score of 0.93, indicating a balanced performance in correctly identifying both positive and negative instances. The Support Vector Machine also demonstrates strong performance with precision, recall, and F1 score values of 0.91, 0.94, and 0.92 respectively. The evaluation demonstrates that Random Forest and Support Vector Machine algorithms are well-suited for exoplanet detection using Kepler time series data. These findings enhance our understanding of the detection process and assist in selecting suitable algorithms for future studies.

REMMI, Rover for EuroMoonMars Investigations has been built at EMMIHS campaign in HI-SEAS Hawaii in 2019 and teleoperated locally and from The Netherlands. For EuroMoonMars 2021 projects, a number of scientific experiments were carried out with the REMMI rover. These experiments were based primarily on teleoperation of the REMMI rover and its mobility system. The rover’s mobility system is based on a continuous track system. It was discovered through experimentation that these tracks are suitable for a number of environments but unsuitable for others. When testing was done in the Analog Astronaut Training Center in Poland, the rover showed that it had difficulty getting a grip on metal surfaces. However, through testing in other outdoor facilities, it was observed that the rover had greater grip on sandy surfaces, grass surfaces and rocks. There was, however, a number of issues with these surfaces. On grass and rock surfaces, small debris would often interfere with the gears of the rover and would prevent movement. The solution to this would be to have a covering to shield the mobility system from both smaller debris and in future, lunar regolith. The rover also had issues with large slopes and inclines. Overall, it was discovered that the REMMI rover was more of a support rover than an exploration rover. The REMMI rover also has a camera on it to allow for remote operation. This camera unlocks a number of future possibilities. Firstly, it will allow the rover to take pictures of samples and areas which the astronaut may want to collect or explore. This is a great feature for the astronaut as they will not have to waste oxygen and resources during an EVA searching for samples. The REMMI rover’s camera also unlocks the possibility to use artificial intelligence to recognise different features of the environment. Similar to self-driving cars, it would theoretically be possible to allow the rover to recognise features of the landscape which would show dangerous terrain for the rover or perhaps a new area to discover. The possibilities will be further tested in July 2021 on Mt Etna, Italy. Acknowledgements: The authors would like to thank the Analog Astronaut Training Center and Dr. Kołodziejczyk for allowing the REMMI rover to be tested in their facilities and for their support throughout. The authors would also like to thank ILEWG EuroMoonMars for providing the REMMI rover for testing.

Introduction: The EuroMoonMars IMA HI-SEAS 2019 campaigns (EMMIHS) are field research campaigns, an initiative directed by the International Lunar Exploration Working Group (ILEWG) of the European Space Agency (ESA) in collaboration with the International MoonBase Alliance (IMA). The purpose of these campaigns is to conduct scientific experiments and test technological instruments relevant to space exploration and extraterrestrial habitation. The team for the second edition of this campaign consisted of six crewmembers, based at the Hawaii Space Exploration Analog and Simulation (HI-SEAS) [1] habitat with support from the Mission Control Centre (MCC), based at the Blue Planet Research Lab in Hawaii, and remote support based at EuroMoonMars ESA/ESTEC in Noordwijk, the Netherlands.In 2019, the EuroMoonMars campaign was launched at HI-SEAS, bringing together researchers from the European Space Agency (ESA), IMA, the International Lunar Exploration Working Group (ILEWG), European Space Research and Technology Centre (ESTEC), VU Amsterdam and many other international organizations [2,3]. These campaigns aim to increase awareness about the research and technology testing that can be performed in analog environments in order to help humans become multi-planetary species.Furthermore, the research and technological experiments conducted at HI-SEAS are going to be used to help build a Moon base in Hawai’i, and ultimately to create an actual Moonbase on the Moon, as part of IMA’s primary goals [6].This paper will deliver details of the research projects conducted and an overview of the crew engineer’s routine. The paper will also present the challenges and outcomes of the mission and its activities from an engineering perspective. Fig. 1 HI-SEAS habitat view. The picture was taken during an EVA using a drone. The Role of The Crew Engineer: It was established, based on the feedback from previous analog missions, that at least one crewmember serving as an engineer with strong analytical, troubleshooting, and hands-on technical skills is vital for the mission’s success. The engineer’s tasks include successfully performing technological research using a drone; the assembly of a small rover to be operated remotely by remote control; HI-SEAS habitat operations and maintenance; network communication systems and data exchange between the ‘Moon’ and ‘Earth.’The crew engineer (CE) is responsible for ensuring nominal operations and the maintenance of the EVA (extra-vehicular activity – any activity performed outside the habitat while wearing analog spacesuits) equipment like EVA spacesuits, life support systems, the communication network, and devices). The engineer is also responsible for the habitat equipment (power systems, solar panels, inverters, batteries, generators, weather stations, surveillance systems, heating systems, and network communication systems).The CE is also in charge of checking the status of the EVA equipment before and after each EVA, as well as gathering feedback from the EVA team. A daily Engineering Report is prepared and provided to the MCC with a summary of engineering specific activities, the status of the equipment, recommendations for improvements, and any requests for further support from the MCC Engineering Support Team. The CE is also in charge of supporting other crew members’ research projects if needed. Fig. 2 HI-SEAS control panel. Fig. 3- EVA Equipment and maintenance With various responsibilities, the CE is vital to ensuring the mission’s safety and projects to be performed with success. Crew Engineers should be prepared not only to operate and maintain the habitat but also to deal with any challenges that might arise from experiments and from living in a Moonbase analog. After the two EMMIHS campaigns, recommendations were provided to ensure the success of future missions and guidelines for other upcoming analog campaigns. Future plans: Future missions at HI-SEAS include more EuroMoonMars IMA HI-SEAS (EMMIHS) missions, collaborative missions with ESA, NASA, universities worldwide, and with companies, such as SIFT and Ketone Technologies. These missions will continue to contribute to the development and testing of technologies and sustainable processes to lay a foundattion for creating the first long-term settlement on the Moon. Acknowledgments: First, we would like to thank the EMMIHS II crew (M. Musilova, S Kerber, A Wanske, J D’Angelo, A P Castro de Paula Nunes, C R Pouwels), the Mission Control from HI-SEAS (Andrew Cox et al.), ILEWG’s EuroMoonMars Manager B. Foing, the Remote Support team (A. Jageli, J. Preusterink, A. Beniest, A. Sitnikova, et al.), and A. Jageli for remote support operations of the rover.We would also like to thank the EMMIHS II sponsors for their generous support: Ruag Space, Capable BV, Kurtz Ersa, dB Matik AG, Tridonic GmbH CoKG, and the Brazilian Space Agency (AEB).References:[1] Hawaii Space Exploration Analog and Simulation, https://hi-seas.org[2] Musilova M, Rogers H, Foing B, Sirikan N. et al. (2019), EMM IMA HI-SEAS campaign February 2019, EPSC-DPS2019-1152[3] Foing, B. H.; EuroMoonMars 2018-2019 Team, EuroMoonMars Instruments, Research, Field Campaigns, and Activities 2017-2019; 2019LPI....50.3090[4] Sirikan, N., Foing, B., Musilova, M., Weert, A., M. Mulder, A., Pothier, B., Burstein, J., & Rogers, H. (2019). EuroMoonMars IMA HI-SEAS 2019 Campaign: An Engineering Perspective on a Moon Base, the International Astronautical Congress, 21-25 October 2019. Washington DC, United States.[5] Musilova, Michaela, Henk Rogers, and Bernard Foing. “Analogue research performed at the HI-SEAS research station in Hawaii.” Geophysical Research Abstracts. Vol. 21. 2019. [6] International MoonBase Alliance, https://moonbasealliance.com/

Context. The diffuse interstellar bands (DIBs) are a set of ∼600 absorption features at optical and near-infrared wavelengths that are found in the interstellar medium in the Milky Way and other galaxies. They remain mostly unidentified and represent the greatest unsolved mystery in astronomical spectroscopy of the past 100 years. Many studies indicate that the carrier molecules are likely carbonaceous molecules, such as polycyclic aromatic hydrocarbons (PAHs) or fullerenes, a theory that is supported by the identifications of five DIBs in the near-infrared attributed to C60+. Aims. This work aims to narrow down which compounds related to C60 could be promising DIB carrier candidates. We did so by conducting a theoretical study of its hydrogenation and charge balance. Methods. We defined a system of relevant reactions, and for each reaction we computed or derived from the literature a reaction rate coefficient. Assuming a steady state, we then computed a distribution of relative abundances in each hydrogenation and charge state. Results. From the model outcomes, we expect the most abundant hydrogenated buckminsterfullerene compound in the diffuse interstellar medium to be C60H+.

Moon Gallery GardenWe will give a report on Moon Gallery Garden exhibition 6 June to 12 July, 2020, Amsterdam and give an update on recent Moon Gallery activities and steps towards the implementation of establishing the first gallery of art, artefacts and science on the Moon. A lunar lander with rovers and telescopes settled at Zone2Source in the Glass House, Amsterdam along with a selection of artworks and prototypes designed to be sent to the Moon by the end of the year 2022. The exhibition also included astronaut performances while wearing spacesuits to ensure safety and avoid contamination.About Moon Gallery:Moon Gallery aims to set up the first permanent gallery on the Moon. Moon Gallery intends to launch 100 artefacts to the Moon within the compact format of 10 x 10 x 1cm plate on a lunar lander exterior panelling as early as 2022. In this Petri-dish-like gallery, we are developing a culture for future interplanetary society. What are the ideas we want to promote into the future? What are the ideas we want to leave behind? Moon Gallery as a pilot platform within the framework of the Moon Village, ITACCUS & ILEWG aims to instigate inspiration for the global space exploration and demonstrate how the challenges along this journey drive innovative design thinking and interdisciplinary collaborations. ILEWG Art Moon Mars collective leads this project, coordinates events and develops content through a series of open calls. Relevance/Significance: Size is one of the biggest challenges of space exploration and the disparity between big ideas and resources for their realisation often stands in the way of many experiments. We ask our participants to think big but small - each idea has to fit within just 1 cubic cm. Creativity is defined as the production of ideas or solutions that are novel and useful (Amabile,1988, 1996). Constraints can give creativity a purpose, a perspective, a starting point. Constraints make us feel challenged and in particular, this statement is accurate for the subject of space. The most challenging and full of constraints environment – Moon – should bring us to the most creative culture and society we believe. At the moment the human presence beyond the Earth is only a matter of survival, but how to make the first step towards making it habitable? We suggest bringing this collection of ideas as the seeds of a new culture. We believe that culture makes a distinction between mere survival and life. Moon Gallery is a symbolic gesture that has a real influence – a way to reboot culture, rethink our values for better living on Earth planet.Moon Gallery is a Manifestation. Neither a place nor an object. Paradoxically a tiny gallery too small for Earth is designed to last on the Moon as a monumental heritage site for thousands of years. Building an everlasting monument, say a pyramid on Earth took a joint effort of a great nation, launching a rocket takes a multinational effort.Mission Statement: We hope to bring the best of humanity to the Moon and to bring the benefits of the Moon to all people on Earth through a sustainable exploration process. Our initiatives connect Art, Moon, Mars and beyond. This includes the organisation of meetings, workshops, art-science-space classes and projects at various universities, sessions at international conferences, art exhibitions, musical and visual performances, and art-science-space platform – Moon Gallery Foundation.Moon Gallery Objectives: – promoting cooperation: bridging innovation, science and art, crossover with space research, developing a space art experiment;– stimulating research: a collective reflection on artistic heritage, analysis – how to design for space (1/6th gravity, extreme environment);– promoting artistic quality: offering artists follow up opportunities involving space science expertise;– reinforcing international position of artistic practice: "International cooperation towards a world strategy for the exploration and utilization of the Moon - our natural satellite" (International Lunar Workshop, Beatenberg (CH), June 1994).Acknowledgements: We acknowledge Hans Broymans and Alice Smits (Zone2Source) for the support of the Moon Gallery Garden in 2020; Moon Gallery Garden Participating artists: Eva Petric, Aneta Zeleznikova, Lakshmi Mohanbabu, Jamal Ageli, Ronald Vles, Ilaria Cinelli, Isabella Douzoglou, Eduardo Kac, Mai Wada, Andy Gracie, Oded Ben-Horin, Priyanka Das Rajkakati, Hady Milani, Sophie Hooghiemstra, Max Baraitser Smith, Sofia Chin, Zuza Banasinska, Renato Japi, Tobias Schalm & Alban Muret, Minna Philips, Maria Polushkina, Johan Recen Larsson, Hans Brooymans, Mary Kuiper, Alexandra Arshanskaya, Badriah Hamelink, Thomas Heidtmann, Anastasia Izotova, Jorick De Quaasteniet, Arina Livadari, Daria Kozhina, Daria Akhrameika, Maria Beaumaster & Sarah Bovelett, Studio Samira Boon, Dana Lamonda, Mark IJzerman, Martin Sjardijn, Guy Livingston, Alexandra Ljadova, Lisa Van Casand, Studio Furthermore, Gabriele Lorusso, Emmanuele Villani. We thank Cesare Barbieri for hosting Moon Gallery lecture at Rotary Club, Università di Padova; EuroMoonMars analog astronauts and colleagues who deployed and tested the gallery prototype at various analogue campaigns: EMMIHS Hawaii, Igluna Zermatt and EMM Iceland. We thank ILEWG and IAF ITACCUS for endorsing the project. We acknowledge Alexander Zaklynsky contribution to the project in 2018.

The time for humans to return to the Moon is upon us. This time we will not just go to the moon to collect some rocks and to leave only footprints. This time we will build permanent settlements and colonize the Moon. Our plan is to enable the building of international Moon settlements. There are numerous space agencies, companies and research institutions working on building rockets that will carry payload to the moon but what we do when we get there has mainly been focused on small scale rover based exploration. It is high time we started the work of designing and building human lunar settlements. The idea is to gather all of the space agencies, companies and research institutions to work in one place where they can combine forces and robotically build prototype Moon structures and landing pads on Earth, with the goal of creating robots that will be sent to the Moon to create human settlements. The group of participants who will carry out the Research & Development is called the IMA (the International MoonBase Alliance). Accomplishments to date: HI-SEAS (the Hawai’i - Space Exploration Analog and Simulation): We held five long duration Mars missions with NASA and the University of Hawaii in a habitat we designed and built on Mauna Loa, an active volcano and the biggest mountain in the world (by volume) on the Big Island of Hawaii. Each mission comprised of 6 crew staying in a 110 sq m (1,200’ sq. ft.) dome to test crew selection and crew psychology (Figure 1). If during the mission crew members left the habitat, that was considered an “Extra Vehicular Activity” (EVA). EVAs were conducted according to strict EVA rules with crew wearing analog spacesuits. All communications from the habitat to the rest of the world were delayed 20 minutes each way to simulate the lag in communicating with Mars. The missions varied between 4 to 12 months in length. Figure 1: The HI-SEAS habitat.

An expedition EMM-Etna to simulate the Lunar and Martian volcanic and soil environment will be carried out at Mount.Etna’s Cratere del Laghetto in Sicily, near Catania Italy by the EuroMoonMars TUDublin and LEAPS ExoMars groups. This scouting campaign intends to train in using instruments to be used on MoonMars landers and rovers, with a perspective of ARCHES DLR telerobotics campaign to be conducted in June 2022, and in preparation for ExoMars rover instruments (PANCAM, CLUPI and spectrometers) science and operations. Figure 1: Lunar Lander and REMMI Rover for Sample AnalysisThe aim of this EMM-Etna expedition is to investigate and analyse the terrain with the use of different scientific instruments. The topography of the landscape will be photographed using a 360° panoramic camera and drone; it will be processed, and a 3D model developed. The terrain will also be investigated using the REMMI Rover, the abilities of the rover to operate and transport equipment will be monitored. This will further develop the knowledge available of the terrain and help future expeditions to identify different landmarks. The use of a Radio Jove Antenna will permit the team to monitor transmissions from both the Sun and Jupiter. This will allow different cosmic events or changes in the celestial objects to be studied and explored. On site a selection of different samples will also be collected and examined using the REMMI Rover. An Ocean Optics UV-Vis-NIR spectrometer will a be operated in order to evaluate the existence of biological compounds and substances within these samples and in the area itself. It is key to understand the molecular makeup of one’s surroundings when in an unknown environment. By analysing samples collected, spectroscopy can be used to identify and determine a diagnostic for each substance. This process will be monitored by a Logitech camera to ensure it is carried put correctly. A selection of photographs will be captured of each sample using a portable optical microscope. This will allow an in-depth analysis of the microscopic structure of each collected sample. The use of all of the instruments mentioned above is key in the investigation and research into the Moon and Martian-like volcanic environment that is Mount Etna.We would also like to thank Prof I. Pagano's team from the University of Catania and Dr A.Wedler's team from DLR Deutsches Zentrum für Luft- und Raumfahrt for their support in organising this expedition.