Optical Spectroscopy of the Icy Dwarf Planet 136472 (2005 FY9)

Physics – Geophysics

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Scientific paper

We present optical spectra of 2005 FY9 taken with the Red Channel Spectrograph and the 6.5-m MMT telescope on 2006 March 4 UT (5000-9500 A; 6.38 A per pixel) and 2007 February 12 UT (6600-8500 A; 1.93 A per pixel). From a cross correlation experiment between the 2006 March 4 spectrum and a pure CH4-ice Hapke model, we found the CH4-ice bands in the MMT spectrum are blueshifted by 3.1 +\- 1.9 A relative to bands in a pure CH4-ice spectrum. We found the bands were blueshifted by 3.3 +/- 2.3 A in our 2006 March 5 spectrum (Tegler et al., 2007, AJ, 133, 526). The higher resolution spectrum of 2007 February 12 UT enabled us measure shifts of individual CH4-ice bands. We found the 7296 A, 7862 A, and 7993 A CH4-ice bands were blueshifted by 4.0 +/- 1.6 A, 4.0 +/- 3.0 A, and 4.2 +/- 3.7 A.
These small shifts are important because they suggest the presence of another ice component. Laboratory experiments show that CH4-ice bands in spectra of CH4 and N2 ice mixtures are blueshifted relative to the bands in spectra of pure CH4-ice (Quirico and Schmitt, 1997, Icarus, 127, 354). A likely candidate is N2-ice because its weak 2.15 micron band and blueshifted CH4 bands are seen in spectra of Triton and Pluto (Cruikshank et al., 1993, Science, 261, 742; Owen et al., 1993, Science, 261, 745).
Our spectra show no difference in CH4/N2 (within the uncertainties) between observations taken at two rotational phases; nor can we detect any difference at different depths into the surface.
We thank the NASA Planetary Astronomy and Planetary Geology and Geophysics Programs for financial support of this research.

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