  The stellar halos of large galaxies represent a vital probe of the processes
of galaxy evolution. They are the remnants of the initial bouts of star
formation during the collapse of the proto-galactic cloud, coupled with imprint
of ancient and on-going accretion events. Previously, we have reported the
tentative detection of a possible, faint, extended stellar halo in the Local
Group spiral, the Triangulum Galaxy (M33). However, the presence of
substructure surrounding M33 made interpretation of this feature difficult.
Here, we employ the final data set from the Pan-Andromeda Archaeological Survey
(PAndAS), combined with an improved calibration and a newly derived
contamination model for the region to revisit this claim. With an array of new
fitting algorithms, fully accounting for contamination and the substantial
substructure beyond the prominent stellar disk in M33, we reanalyse the
surrounds to separate the signal of the stellar halo and the outer halo
substructure. Using more robust search algorithms, we do not detect a large
scale smooth stellar halo and place a limit on the maximum surface brightness
of such a feature of ${\mu}_V$ = 35.5 mags per square arcsec, or a total halo
luminosity of $L < 10^6L_{\odot}$.
