overall stability of asteroids in co-orbital motion with Venus has been studied multiple times (e.g. Mikkola & Innanen 1992; Tabachnik & Evans 2000; Scholl, Marzari & Tricarico 2005; Morais & Morbidelli 2006). Results from these studies indicate that any hypothetical primordial population of Venusian co-orbitals could not possibly have survived until the present time and that any current population of co-orbital objects must be transient in nature. Asteroids in co-orbital motion with Venus undergo multiple captures/ejections in/from the 1:1 mean motion resonance and the average duration of one of these events (capture to ejection) is 32,000 yr (Morais & Morbidelli 2006). During these episodes they may become quasi-satellites or librate on horseshoe orbits or tadpole orbits (Scholl et al. 2005).

Here we present the results for the nominal orbit in Table \[elements\]. In addition to these calculations using the nominal orbital elements and for Model 3 (see below), we have performed 100 control simulations using sets of orbital elements derived from the nominal ones using the uncertainties in Table \[elements\], at 3-$\sigma$. These control integrations take into account the uncertainties in observation and orbital determination. As listed in Table \[elements\], the errors are very small and the results for the 