UV spectrum of Enceladus |
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| Authors: | Mark Zastrow John T Clarke Amanda R Hendrix Keith S Noll |
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| Institution: | 1. Center for Space Physics, Boston University, 725 Commonwealth Ave., Boston, MA 02215, United States;2. Jet Propulsion Laboratory, California Institute of Technology, Mail Stop 230-250, Pasadena, CA 91109, United States;3. Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, United States |
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| Abstract: | We present a far ultraviolet (FUV) spectrum of Saturn’s moon Enceladus from the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST). We have put upper limits on emission from C, N, and O lines in Enceladus’ atmosphere and column densities for the C lines assuming solar resonance scattering. We find these upper limits to be relatively low—on the order of tens to thousands of Rayleighs and with C column densities on the order of 108–1015 cm?2, depending on the assumed source size. We also present a segment of a reflectance spectrum in the FUV from ～1900–2130 Å. This region was sensitive to the different ice mixtures in the model spectra reported by Hendrix et al. (Hendrix, A.R., Hansen, C.J., Holsclaw, G.M. 2010]. Icarus, 206, 608). We find the spectrum brightens quickly longward of ～1900 Å, constraining the absorption band observed by Hendrix et al. from ～170 to 190 nm. We find our data is consistent with the suggestion of Hendrix et al. of the presence of ammonia ice (or ammonia hydrate) to darken that region, and also possibly tholins to darken the mid-UV, as reported by Verbiscer et al. (Verbiscer, A.J., French, R.G., McGhee, C.A. 2005]. Icarus, 173, 66). |
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