Near-infrared spectroscopy of Miranda

DOI: 
10.1051/0004-6361/201321988
Publication date: 
01/02/2014
Main author: 
Gourgeot F.
IAA authors: 
Alvarez-Candal A.
Authors: 
Gourgeot F., Dumas C., Merlin F., Vernazza P., Alvarez-Candal A.
Journal: 
Astronomy and Astrophysics
Publication type: 
Article
Volume: 
562
Pages: 
Number: 
A46
Abstract: 
Aims. We present new near-infrared spectra of the leading and trailing hemispheres of Uranus's icy satellite Miranda. This body is probably the most remarkable of all the satellites of Uranus, because it displays series of surface features such as faults, craters, and large-scale upwelling, a remnant of a geologically very active past. Methods. The observations were obtained with PHARO at Palomar and SpeX at the IRTF Observatory. We performed spectral modelings to further constrain the nature and the chemical and physical states of the compounds possibly present on the surface of Miranda. Results. Water ice signatures are clearly visible in the H and K bands, and it appears to be found in its crystalline state over most of the satellite's surface. Unlike what has been found for Uranus's outer moons, we did not find any significative differences in the abundances of ices covering the leading and trailing hemispheres of Miranda. The signature of carbon dioxide cannot be seen in our spectra, which could still account for the presence of ammonia hydrate, though in small amounts. © ESO, 2014.
Database: 
WOK
SCOPUS
ADS
URL: 
https://ui.adsabs.harvard.edu/#abs/2014A&A...562A..46G/abstract
ADS Bibcode: 
2014A&A...562A..46G
Keywords: 
Infrared: planetary systems; Planets and satellites: surfaces