DO THE BROAD EMISSION-LINES IN ARP 102B ARISE IN A RELATIVISTIC DISK

It is been proposed by Chen, Halpern, and Fillippenko that the asymmetric, double-peaked, emission-line profiles observed in Arp 102B arise in a relativistic disk. We present new data showing that at least at some epochs the long-wavelength side of the line profile is higher than the short-wavelength side, contrary to what is expected from a relativistic disk in which the approaching side of the disk is brighter because of Doppler boosting. Moreover, the two peaks do not vary together in flux as expected if the emission-line variability is attributable to changes in the flux from the central continuum source. We conclude that an axisymmetric relativistic disk cannot explain the salient features of the line profiles in Arp 102B.