Distributions of H₂O and CO₂ ices on Ariel, Umbriel, Titania, and Oberon from IRTF/SpeX observations

Published in 2006: Icarus 184, 543-555.

W.M. Grundy^1,2, L.A. Young^1,3, J.R. Spencer³, R.E. Johnson⁴, E.F. Young^1,3, and M.W. Buie²

(1) Visiting/remote observer at the Infrared Telescope Facility, operated by the University of Hawaii under contract from NASA.

(2) Lowell Observatory, Flagstaff AZ.

(3) Southwest Research Institute, Boulder CO.

(4) University of Virginia Dept. of Engineering Physics, Charlottesville VA.

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Abstract

We present 0.8 to 2.4 micron spectral observations of uranian satellites, obtained at IRTF/SpeX on 17 nights during 2001-2005. The spectra reveal for the first time the presence of CO₂ ice on the surfaces of Umbriel and Titania, by means of 3 narrow absorption bands near 2 microns. Several additional, weaker CO₂ ice absorptions have also been detected. No CO₂ absorption is seen in Oberon spectra, and the strengths of the CO₂ ice bands decline with planetocentric distance from Ariel through Titania. We use the CO₂ absorptions to map the longitudinal distribution of CO₂ ice on Ariel, Umbriel, and Titania, showing that it is most abundant on their trailing hemispheres. We also examine H₂O ice absorptions in the spectra, finding deeper H₂O bands on the leading hemispheres of Ariel, Umbriel, and Titania, but the opposite pattern on Oberon. Potential mechanisms to produce the observed longitudinal and planetocentric distributions of the two ices are considered.

Figure 1

Fig. 1. Example spectra of uranian satellites, normalized at J band and offset upward with zero levels indicated by tick marks on the ordinate axis. Gaps around 1.4 and 1.85 microns coincide with high atmospheric opacity. The Ariel spectrum is an average of all spectra with subsolar longitudes between 210 and 330 degrees. The Umbriel spectrum is from 2005/09/18 UT and the Titania and Oberon spectra are both from 2005/10/13 UT. Data for these spectra are available via links below.

Figure 4

Fig. 4. Variation of total integrated area of the three strongest CO₂ ice bands near 2 microns. Sine fits are plotted as dashed curves. Both the integrated areas and their longitudinal variation decline with planetocentric distance. No CO₂ absorption was detected in the Oberon spectra.

• Ariel trailing hemisphere average spectrum.
• Umbriel trailing hemisphere spectrum.
• Titania trailing hemisphere spectrum.
• Oberon trailing hemisphere spectrum.
• ADS refereed citations to this work.