$440>K_2$ (km s$^{-1}$) $>260$ for $0.01<q<1$.

The observed velocity FWHM ($v_{\rm fwhm}$) of the lines provides an upper limit to the minimum emitting Keplerian disk radius: $$R_{\rm in}\lsim 1.3\cdot 10^{10}\ (M_1/M_\odot)\left(\sin i/v_{\rm
fwhm}\right)^2\ {\rm cm},$$ where $v_{\rm fwhm}$ is expressed in units of 1000 km s$^{-1}$. The absorption features from the optically-thick disk (see §4.1 and Table. \[tab:lines\]) have FWHM $\gsim 3000$ km s$^{-1}$ implying $R_{\rm in}\lsim 10^9$ cm. Haswell et al. (2000b) detect broad Ly$\alpha$ absorption with $v_{\rm fwhm} \sim 10^4$ km s$^{-1}$ which gives a stricter $R_{\rm in}\lsim 10^8$ cm or $R_{\rm in} \lsim 500$ in Schwarzschild units. Spectral models of the X-ray low/hard state of BH candidates tend to predict larger values of $R_{\rm in} (\gsim
1000$ in Schwarzschild units) at which the transition from a thin disk to a hot advection-dominated flow occurs (see, e.g., Esin et al. 1998). The EUV flux of XTE J1118+480 could also imply a smaller transition radius (see §4.2).

Doppler mapping
---------------

Figure \[fig:swave\] shows the evolution of the He[ii]{} $\lambda
4686$ line profile over an approximately continuous 2.9 hr period on April 20, 2000. A partial S-wave pattern moves from the red to the blue side of the He[ii]{} $\lambda 