Results: Eclipse UZ Fornax
In order to demonstrate the capabilities of S-CAM 2, we have created an animation showing an observation of an entire eclipse of UZ For. This was created by splicing together two integrations, with the join between them near the mid-point of the eclipse. Each step in the animation corresponds to 3 seconds of actual data.
The lightcurve in the top of the plot shows the evolution of the total source intensity across the complete spectral range. In order to illustrate the energy-sensitivity of the device, however, the 36 array pixels in the lower image are first assigned colours based on the V/R ratio obtained from two energy bands (ranging from blue to red on a spectral scale), and are then assigned intensities based on the total counts in that pixel over the 3 second time period.
A number of other cataclysmic variables have also been the subject of S-Cam 2 studies, including HU Aqr (Bridge et al 2002), Ep Dra (Bridge et al 2003) and IY Uma (Steeghs et al 2002), with more data still be to be analysed. Other studies have shown that S-Cam 2 is a powerful instrument for making direct measurements (without dispersive optics) of both quasar redshifts (de Bruijne et al 2002) and stellar temperatures (Reynolds et al 2003).
References (published S-Cam studies):
Perryman M.A.C., Cropper M., Ramsay G. et al 2001 MNRAS, 324, 899
Bridge C.M., Cropper M., Ramsay G. et al 2002 MNRAS, 336 1129
Bridge C.M., Cropper M., Ramsay G. et al 2003 MNRAS, 431 863
de Bruijne J.H.J., Reynolds A.P, Perryman M.A.C., 2002 A&A, 381, L57
Reynolds A.P., de Bruijne J.H.J, Perryman M.A.C., 2003 A&A, 400, 1209