Follow Us| AM Cas | ||||||||||||||||||
| AM Cas was observed with FUSE in an intermediate state of brightness. The longer wavelengths of the spectrum are strongly affected by the worm. The spectrum was modeled with a WD+disk model assuming both E(B-V)=0 and E(B-V)=0.2. The distance to the system is possibly around 350 pc. The mass of the WD is unknown and so is the system inclination. We assessed Mwd and i here from the modeling (note the difference between model 1 and model 2 the Table). Details on the processing of the observed spectrum and the spectral analysis are given in Godon et al. 2009. The two models shown in the Figures do fit the longer wavelengths of the FUSE spectrum, but in the shorter wavelengths the observed flux is larger than in the models. The excess of flux could be due, for example, to broad emission from N iv (923) and S vi (933, 944) but as shown in the figures the observed features are not at the expected wavelengths and do not have the proper line profile, in addition excess of flux also occurs around 950 to 960 A, and the line notation is therefore only suggestive. Lines such as Si iii (1110) and Si iv (1120-1130) make large shallow depression which fit the disk-dominated model, indicative that Keplerian broadening is responsible for their appearence. The ISM absorption lines (molecular hydrogen) are colored blue in the Figures so as to not be confused with the other lines. | |||||||||||||||||
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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., Szkody, P., 2009, ApJ, 701, 1091 | ||||||||||||||||||||||||||||||||||||
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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., Szkody, P., 2009, ApJ, 701, 1091 | ||||||||||||||||||||||||||||||||||||
Notes on figures:The flux (vertical axis) is given in ergs/sec/cm2/A and the wavelength (horizontal axis) is given in Angstroem. For clarity the spectrum is shown on 3 panels: the upper panel from about 900 to 1000A, the middle panel from about 1000A to 1100A, and the lower panel from about 1100A to 1200A. Air glow emission is anoted above each panel with a "+" sign inside a circle. Strong emission lines reaching the upper part of the frame in each pael is marked just above the panel. The Hydrogen series is marked below the x-axis in the upper and middle panel and the hydrogen cut-off limit is clearly marked around 915A with an increasing density of tick marks. The He I (1168A) is marked below the lower panel. Oxygen I lines are shown with an arrow "OI -->" if many (ISM) OI lines are present, they are just annotated with verical tick marks in the lower portion of each panel. ISM molecular hydrogen lines are either individually annotated vertically (e.g. L10R1) or just marked with an arrow "MH -->" and vertical tick marks (usually in the upper part of each panel). Features resulting from fixed pattern noise introduced by FUSE detect ors are indicated with "FPN;.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. |
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