TY - JOUR
T1 - Characterization of carbon dioxide on Ganymede and Europa supported by experiments
T2 - Effects of temperature, porosity, and mixing with water
AU - Schiltz, L.
AU - Escribano, B.
AU - Muñoz Caro, G. M.
AU - Cazaux, S.
AU - Del Burgo Olivares, C.
AU - Carrascosa, H.
AU - Boshuizen, I.
AU - González Díaz, C.
AU - Chen, Y. J.
AU - More Authors, null
PY - 2024
Y1 - 2024
N2 - Context. The surfaces of icy moons are primarily composed of water ice that can be mixed with other compounds, such as carbon dioxide. The carbon dioxide (CO2) stretching fundamental band observed on Europa and Ganymede appears to be a combination of several bands that are shifting location from one moon to another. Aims. We investigate the cause of the observed shift in the CO2 stretching absorption band experimentally. We also explore the spectral behaviour of CO2 ice by varying the temperature and concentration. Methods. We analyzed pure CO2 ice and ice mixtures deposited at 10 K under ultra-high vacuum conditions using Fourier-transform infrared (FTIR) spectroscopy and temperature programmed desorption (TPD) experiments. Laboratory ice spectra were compared to JWST observation of Europa's and Ganymede's leading hemispheres. The simulated IR spectra were calculated using density functional theory (DFT) methods, exploring the effect of porosity in CO2 ice. Results. Pure CO2 and CO2-water ice show distinct spectral changes and desorption behaviours at different temperatures, revealing intricate CO2 and H2O interactions. The number of discernible peaks increases from two in pure CO2 to three in CO2-water mixtures. Conclusions. The different CO2 bands were assigned to ν3,1 (2351 cm-1, 4.25 μm) caused by CO2 dangling bonds (CO2 found in pores or cracks) and ν3,2 (2345 cm-1, 4.26 μm) due to CO2 segregated in water ice, whereas ν3,3 (2341 cm-1, 4.27 μm) is due to CO2 molecules embedded in water ice. The JWST NIRSpec CO2 spectra for Ganymede and for Europa can be fitted with two Gaussians attributed to ν3,1 and ν3,3. For Europa, ν3,1 is located at lower wavelengths due to a lower temperature. The Ganymede data reveal latitudinal variations in CO2 bands, with ν3,3 dominating in the pole and ν3,1 prevalent in other regions. This shows that CO2 is embedded in water ice at the poles and it is present in pores or cracks in other regions. Ganymede longitudinal spectra reveal an increase of the CO2 ν3,1 band throughout the day, possibly due to ice cracks or pores caused by large temperature fluctuations.
AB - Context. The surfaces of icy moons are primarily composed of water ice that can be mixed with other compounds, such as carbon dioxide. The carbon dioxide (CO2) stretching fundamental band observed on Europa and Ganymede appears to be a combination of several bands that are shifting location from one moon to another. Aims. We investigate the cause of the observed shift in the CO2 stretching absorption band experimentally. We also explore the spectral behaviour of CO2 ice by varying the temperature and concentration. Methods. We analyzed pure CO2 ice and ice mixtures deposited at 10 K under ultra-high vacuum conditions using Fourier-transform infrared (FTIR) spectroscopy and temperature programmed desorption (TPD) experiments. Laboratory ice spectra were compared to JWST observation of Europa's and Ganymede's leading hemispheres. The simulated IR spectra were calculated using density functional theory (DFT) methods, exploring the effect of porosity in CO2 ice. Results. Pure CO2 and CO2-water ice show distinct spectral changes and desorption behaviours at different temperatures, revealing intricate CO2 and H2O interactions. The number of discernible peaks increases from two in pure CO2 to three in CO2-water mixtures. Conclusions. The different CO2 bands were assigned to ν3,1 (2351 cm-1, 4.25 μm) caused by CO2 dangling bonds (CO2 found in pores or cracks) and ν3,2 (2345 cm-1, 4.26 μm) due to CO2 segregated in water ice, whereas ν3,3 (2341 cm-1, 4.27 μm) is due to CO2 molecules embedded in water ice. The JWST NIRSpec CO2 spectra for Ganymede and for Europa can be fitted with two Gaussians attributed to ν3,1 and ν3,3. For Europa, ν3,1 is located at lower wavelengths due to a lower temperature. The Ganymede data reveal latitudinal variations in CO2 bands, with ν3,3 dominating in the pole and ν3,1 prevalent in other regions. This shows that CO2 is embedded in water ice at the poles and it is present in pores or cracks in other regions. Ganymede longitudinal spectra reveal an increase of the CO2 ν3,1 band throughout the day, possibly due to ice cracks or pores caused by large temperature fluctuations.
KW - Infrared: planetary systems
KW - Methods: laboratory: solid state
KW - Methods: numerical
KW - Methods: observational
KW - Planets and satellites: composition
UR - http://www.scopus.com/inward/record.url?scp=85201716546&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202449846
DO - 10.1051/0004-6361/202449846
M3 - Article
AN - SCOPUS:85201716546
SN - 0004-6361
VL - 688
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A155
ER -