This low S/N FUSE spectrum of EY Cyg was obtained in quiescence and is modeled with a WD spectrum. The increase of flux in the short wavelengths (<950A) is an artifact in one of the FUSE channels due to inaccurate background subtraction (very low S/N), the N iv (923) lines have been marked but are not detected and do not match any observed feature. All the sharp emission lines of H, O, He) are due to geo- and helio-coronal emission (light reflected in the telescope). There could be some broad emission from O vi (1032) and, though less likely, from O vi (1038). We have marked some of the ISM absorption lines where they match some absorption features in the observed spectrum such as some hydrogen molecular lines and C ii (1036). With some low (but non-zero) reliability we identify some absorption lines matching the theoretical spectrum as follows: S iv (1073), Si iv (1128) and Si iii (1142-1145). All the other lines that are marked on the figure are not identified and are there mostly for comparison and identification with the theoretical spectrum. The FUSE spectrum of this system was processed and modeled in Godon et al. (2008). This object exhibits the N/C composition anomaly indicative of CNO processing.

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FUSE Data

Synthetic Spectrum

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These data and models were published in the paper:

Godon, P., Sion, E.M., Barrett, P.E., Hubeny, I., Linnell, A.P., Szkody, P. 2008, ApJ, 679, 1447

Notes on figures:

When a model is shown, the portions of the observed spectrum that have been masked before the spectral fit are in blue, while the rest of the observed spectrum is in red. The model fit is shown the solide line in black (or possibly white). If the model is a composite made of a disk model and a white dwarf model, then these are shown with the dashed- and dotted lines (respectively). Some models include the effect of quasi-molecular HI absorption features, these are labelled "Q-mol" in the spectrum.