then, the optical and X-ray flux have decreased significantly, indicating that the source may soon enter quiescence.

Continuum
---------

Figure \[fig:lowres\] shows the sum of the two DIS [*lowres*]{} spectra obtained on April 7, 2000, which is also representative of other spectra of the source obtained later on during our campaign. The strong, blue power-law continuum and the weak emission lines are typical of an SXT in outburst (see also Garcia et al. 2000). A power-law fit to the blue part of the spectrum yields a slope $p
\simeq +0.4 \pm 0.2$ (where the flux F$_\nu \propto \nu^p$), while a similar fit to the red part of the spectrum yields $p \simeq +0.33 \pm
0.15$. These values are consistent with the expectation $p=1/3$ for an optically-thick accretion disk (see, e.g., Frank, King & Raine 1992). Hynes et al. (2000b) find that the spectrum is flat using a wider wavelength range.

The broad, double-peaked H$\alpha$ emission line is the only one easily identified on the spectrum of Fig. \[fig:lowres\], but a closer examination reveals the presence of He[ii]{} $\lambda4686$, and of additional Balmer and He lines in the other spectra that we collected (see §3.2 below). We find only marginal evidence 