systems. The QPO was confirmed by ASCA observations, which also suggest the presence of a soft component in the spectrum (below 2 keV), possibly due to emission from the accretion disk in the system (Yamaoka et al. 2000). [ Soft X-ray observations by [*Chandra*]{} did not confirm this (McClintock et al. 2000)]{}. The QPO frequency was reported to have shifted from 0.085 Hz to $\gsim 0.1$ Hz in subsequent observations (Yamaoka et al. 2000; Wood et al. 2000). Pointed XTE observations at the end of May do not reveal significant changes in the emission spectrum (P. Jonker, private communication).

XTE J1118+480 has also been the subject of an extensive multiwavelength observation campaign with HST, EUVE, UKIRT and RXTE. Thanks to the very low interstellar absorption to the source, the first EUVE spectrum of a BH-candidate X-ray Transient was obtained (Mauche et al. 2000). No periodic modulation was found in the EUVE data (Hynes et al. 2000b). An HST spectrum revealed a very broad ($>
10,000$ km s$^{-1}$) Ly$\alpha$ absorption feature, suggestive of a massive accretor (Haswell et al. 2000b). Haswell et al. (2000c) obtained a near-UV power density spectrum of XTE J1118+480 with a QPO and an overall shape in 