Follow Us| BB Dor | ||||||||||||||||||
| BB Dor was observed with FUSE in a high state. We fit here four different models as shown: a WD, a disk, a WD+Disk at low inclination, and a WD+Disk at high inclination. The high inclination disk contributes much less flux than the WD, while the low inclination disk contributes much more flux than the WD. The sharp emission lines, all colored in blue, are most likely due to the reflection of day and/or sun light in the telescope. There are lines that appear clearly in the model but cannot be identified with reliability in the observed spectrum; these lines are marked on the figure (e.g. S iv 1006 & 1100). The S iv (1063 & 1073) and Si iii (1110) lines are much deeper in the observed spectrum than in the model, possibly a sign that there is additional absorption from material above the disk. The oxygen doublet is also in absorption and is not modeled. All the details of the spectral modeling, data analysis and processing of the data are given in Godon et al. 2008. | |||||||||||||||||
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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., Schlegel, E.M. 2008, ApJ, 687, 532 | ||||||||||||||||||||||||||||||||||||
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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., Schlegel, E.M. 2008, ApJ, 687, 532 | ||||||||||||||||||||||||||||||||||||
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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., Schlegel, E.M. 2008, ApJ, 687, 532 | ||||||||||||||||||||||||||||||||||||
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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., Schlegel, E.M. 2008, ApJ, 687, 532 | ||||||||||||||||||||||||||||||||||||
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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