  New imaging of V605 Aql, was obtained in 2009 with HST/WFPC2, which had a
nova-like outburst in 1919, and is located at the center of the planetary
nebula (PN), Abell 58. This event has long been ascribed to a final helium
shell flash, but it has been suggested recently that it may instead have been
an ONe nova. The new images provide an 18 year baseline for the expansion of
the ejecta from the 1919 event. In addition, the central star has been directly
detected in the visible for the first time since 1923, when it faded from sight
due to obscuration by dust. The expansion of the ejecta has a velocity of ~200
km/s, and an angular expansion rate of ~10 mas/yr, consistent with a 1919
ejection. This implies a geometric distance of 4.6 kpc for V605 Aql, consistent
with previous estimates. The gas mass in the central knot of ejecta was
previously estimated to be 5 x 10^-5 M(Sun). It is estimated that warm dust
associated with this gas has a mass of ~10^-5 M(Sun). There is also evidence
for a significant amount, 10^-3 M(Sun), of cold (75 K) dust, which may be
associated with its PN. The knot ejected in 1919 is asymmetrical and is
approximately aligned with the asymmetry of the surrounding PN. Polarimetric
imaging was obtained to investigate whether the 2001 spectrum of V605 Aql was
obtained primarily in scattered light from dust in the central knot, but the
signal-to-noise in the data was insufficient to measure the level of
polarization.
