  The development of knowledge of how the coronal origin of the solar wind
affects its in situ properties is one of the keys to understanding the
relationship between the Sun and the heliosphere. In this paper, we analyse
ACE/SWICS and WIND/3DP data spanning >12 years, and test properties of solar
wind suprathermal electron distributions for the presence of signatures of the
coronal temperature at their origin which may remain at 1AU. In particular we
re-examine a previous suggestion that these properties correlate with the
oxygen charge state ratio O7+/O6+; an established proxy for coronal electron
temperature. We find only a very weak but variable correlation between measures
of suprathermal electron energy content and O7+/O6+. The weak nature of the
correlation leads us to conclude, in contrast to earlier results, that an
initial relationship with core electron temperature has the possibility to
exist in the corona, but that in most cases no strong signatures remain in the
suprathermal electron distributions at 1AU. It can not yet be confirmed whether
this is due to the effects of coronal conditions on the establishment of this
relationship, or to the altering of the electron distributions by processing
during transport in the solar wind en route to 1AU. Contrasting results for the
halo and strahl population favours the latter interpretation. Confirmation of
this will be possible using Solar Orbiter data (cruise and nominal mission
phase) to test whether the weakness of the relationship persists over a range
of heliocentric distances. If the correlation is found to strengthen when
closer to the Sun, then this would indicate an initial relationship which is
being degraded, perhaps by wave-particle interactions, en route to the observer
