Europlanet Science Congress 2022
Palacio de Congresos de Granada, Spain
18 – 23 September 2022
Europlanet Science Congress 2022
Palacio de Congresos de Granada, Spain
18 September – 23 September 2022

SB5

SB
Tools for characterizing planetary and small bodies surfaces, atmospheres, and dust particles (Imagery, photometry, spectroscopy, spectrophotopolarimetry) 

Electromagnetic scattering phenomena play a key role in determining the properties of Solar System objects based on observations using different techniques and in a variety of wavelengths ranging from the ultraviolet to the radio. This session will promote a general advancement in the exploitation of observational and experimental techniques to characterize complex particulate media. We particularly welcome discussions of future perspectives in the utilization of observational and experimental techniques to characterize small bodies surfaces in the context of new missions like Comet Interceptor, and also the planetary aerosols and dust in the solar system.

Abstracts are solicited on progress in observational, numerical, and laboratory methods to extract relevant information from imagery, photometry, polarimetry and spectroscopy in solid phase, reference laboratory databases, photometric and polarimetric modeling, software and web service applications.

Conveners: Oleksandra Ivanova, Frédéric Schmidt | Co-conveners: Stefano Bagnulo, Ludmilla Kolokolova, Johannes Markkanen, Olga Muñoz, Olivier Poch, A.Chantal Levasseur-Regourd, Stéphane Erard, Antti Penttilä, Maria Gritsevich
Orals
| Fri, 23 Sep, 10:00–13:30 (CEST), 15:30–17:00 (CEST)|Room Andalucia 2
Posters
| Attendance Thu, 22 Sep, 18:45–20:15 (CEST) | Display Wed, 21 Sep, 14:00–Fri, 23 Sep, 16:00|Poster area Level 2

Session assets

Discussion on Slack

Orals: Fri, 23 Sep | Room Andalucia 2

Chairpersons: Olivier Poch, Ludmilla Kolokolova
Laboratory measurement
10:00–10:20
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EPSC2022-512
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solicited
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MI
Antoine Pommerol, Lucas Patty, Stefano Spadaccia, Lukas Affolter, Patricio Becerra, Holly Capelo, Romain Cerubini, Camila Cesar, Tatiana Drozhzhova, Clément Feller, Kristina Kipfer, Linus Stoeckli, Adomas Valantinas, Zuriñe Yoldi, and Nicolas Thomas

The planetary Ice Laboratory has been developed at the University of Bern to measure various reflectance properties of analogues for small bodies and planetary surfaces with a special focus on icy surfaces. Its core facilities are a set of devices to produce well-characterized and reproducible analogue samples and a set of instruments designed to measure the reflectance properties of the samples over different spectral ranges, different geometrical configurations, either in total light or sorted by polarisation state.

We use the laboratory to work on a range of scientific questions, mostly related to current Solar System missions and the interpretation of remote-sensing data but also occasionally on telescopic observations of Solar System objects as well as distant exoplanets and planet-forming circum-stellar discs. The experimental datasets collected are then provided to public databases for use by the community.

Some of our most recent investigations include:

- Visible and near-infrared reflectance spectra of analogues for the icy moons of the outer Solar System. We have collected new data with salty ice samples (Fig. 1), before and after irradiation by electrons, which can be compared with reflectance data measured by previous missions. The dataset will also help with the preparation of the JUICE and Europa Clipper missions.

- Simulations of cometary activity, in the framework of the CoPhyLab project led by TU Braunschweig, with IWF Graz, MPS and DLR as partners. We develop quantitative methods to derive the ice-to-dust ratio from reflectance data in order to study the sublimation of dust ice mixtures prepared as cometary analogues. The results help interpreting the data from previous missions such as Rosetta and preparing future missions such as Comet Interceptor.

- Spectral reflectance properties of different types of icy and dry Martian analogues, most notably in relation with the quantitative analysis of images returned by the CaSSIS imager of Exomars TGO. These measurements are performed in a simulation chamber equipped to simulate the Martian conditions of composition, temperature and pressure and we look at the samples with an imager equipped with the spare bandpass filters from CaSSIS (Fig. 2).

- The linear polarisation properties of pure and mixed minerals as analogues for the surfaces of asteroids with implications for the interpretation of measured phase curves in terms of composition. (see also Spadaccia et al., this conference).

- Assessment of the potential of circular spectropolarimetry as a biosignature in reflected light for Solar System objects and exoplanets.

- Measurements of artificial samples for comparison with numerical simulations.

With this presentation, we will provide an overview of the main objectives of the overall project, detail the methodology used, and present some of the results from the most recent studies mentioned here.