  We analyse \'Echelle spectra of $\theta^1$ Ori F obtained by us on six nights
unevenly distributed along six years; we identify several hundred spectral
lines and measure, for the first time, the star's heliocentric radial velocity.
We also collect and discuss previously published photometry of $\theta^1$ OriF .
  We find that $\theta^1$ Ori F is a Chemically Peculiar (CP) star with
overabundant silicon and phosphorus, and possibly other elements as well. From
the singly ionised Fe, Cr and Ti lines we estimate its spectral type to be
between B7 and B8. The radial velocity of $\theta^1$ Ori F is possibly
marginally variable, with an average of $24 \pm 4.2$ kms, (standard deviation),
in good agreement with the mean radial velocity of the Orion Nebula Cluster
members, and about 5 kms smaller than the average of the other Trapezium
components. We cast doubt on the coeval nature of this star relative to the
other Trapezium components, and present arguments that almost certainly exclude
its membership to the Orion Trapezium. $\theta^1$ Ori F turns out to be
enigmatic in several respects, and is probably an important link for
understanding the evolutionary stage at which the CP phenomenon sets on.
