CVARO-UVSCAT Object Page

NSV 10934

Target Information
RA:	18:40:52.45
Dec:	-83:43:09.7
Type:	DN
Subtype:	SU
Period [hr]:	1.74
Inclination [deg]:	0
E(B-V):	0

NSV 10934 was observed with FUSE twice consecutively, and we combined the two individual spectra. At the time of the observations NSV 10934 was in a low state about a month after an outburst. The low S/N (especially in the lower wavelengths) is due to the fact that the data from the 2bSiC, 2bLiF and 1aSiC channels were unusable and a large portion of the 1bLiF channel was lost to the infamous worm. Because of this there is a gap around 1085A and the spectrum is not modeled. Details on the processing of the observed spectrum can be found in Godon et al (2009). The only spectral features that we identify and which belong to the source are the braod emission from C iii (977 & 1175) and the O vi doublet. The other spectral features that are identified are the ISM molecular hydrogen absorption lines. All the other other spectral lines marked on the figure are only suggestive.

Bibliography

FUSE Data

Data:	G9251201
Obs Date:	2006-06-28 14:08:26
Exposure Time [sec]:	10844
State:	LOW
Download FUSE data (ascii table)

Data:	G9251202
Obs Date:	2006-06-30 17:46:04
Exposure Time [sec]:	14177
State:	LOW
Download FUSE data (ascii table)

Data:	combined
Obs Date:	2006-06-28 14:08:26
Exposure Time [sec]:	25021
State:	LOW
Download FUSE data (ascii table)

Synthetic Spectrum

Model:	NONE
Inclination [deg]:	0
E(B-V):	0
Log(g) [cgs]:
T [K]:	0
VRot [km/s]:	0
C [solar]:
Si [solar]:
S [solar]:
N [solar]:
d [pc]:	0
Log(Mdot) [Msun/year]:

Click to see larger version of the plot

These data and models were published in the paper:

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.