  The Seyfert 1 galaxy 1E1615+061 was observed to display a very steep and
intense soft X-ray spectrum during a HEAO-1 A2 observation in the 1978. Such an
exceptionally soft X-ray state has never been observed subsequently, but the
source has continued to exhibit a large (up to a factor 6) range of X-ray
intensity variability. The overall UV/X-ray spectrum of this source, observed
during a multiwavelength campaign in 1991-1992, can be well fit with a
self-consistent, low-m-dot accretion disk model. In this model, the soft X-rays
result were suggested to arise from reflection of the nuclear emission by
mildly ionized material in the inner regions of the disk. In this Paper we
report the results of an ASCA observation in 1995 August, which give a direct
confirmation of such a scenario. The spectrum may be modeled as a power-law
with a photon index of 1.8, together with absorption consistent with the
galactic line of sight value, substantial reflection from ionized material and
an iron fluorescent K-alpha emission line. The centroid energy (~6.6--6.8 keV)
implies a ionization stage >Fe XIX. The line profile is consistent with that
expected from a kinematically and gravitationally distorted line around a black
hole. These results provide the first direct evidence for the existence of
considerable amount of ionized material around the nucleus of a "broad" Seyfert
1 galaxy.
