THE ORIGIN OF THE OPTICAL-EMISSION LINES IN THE NARROW-LINE SEYFERT-1GALAXY RE-J1034+396

We present high-resolution optical spectroscopy of the narrow-line Sey fert 1 galaxy and ultrasoft X-ray source RE J1034+396. We examine the profiles of the Hot, HP and [O III] lines, and find evidence for an in termediate-velocity (FWHM similar to 1000 km s(-1)) line-emitting regi on which produces significant amounts of both the permitted and forbid den line fluxes. This intermediate region probably has a scalesize of order Ipc, and its emission dominates the Balmer line profiles, causin g the net FWHM to be relatively low. There is also an underlying broad er component to the Balmer lines which has FWHM similar to 2500 km s(- 1), and which almost certainly originates from the normal broad-line r egion. Since narrow Balmer lines are now a common, if not ubiquitous, feature of ultrasoft X-ray AGN, this result implies a causal link betw een the slope of the soft X-ray spectrum and the physical conditions i n the broad- and intermediate-line region. Our observations show that AGN models with abnormally low-mass central black holes, or broad-line clouds at abnormally large radii from the black hole, are not a requi rement to explain RE J1034+396.