  It is not yet settled how the combination of secular processes and merging
gives rise to the bulges and pseudobulges of galaxies. The nearby ($D\sim$ 4.2
Mpc) disk galaxy M94 (NGC 4736) has the largest pseudobulge in the local
universe, and offers a unique opportunity for investigating the role of merging
in the formation of its pseudobulge. We present a first ever look at M94's
stellar halo, which we expect to contain a fossil record of M94's past mergers.
Using Subaru's Hyper Suprime-Cam, we resolve and identify red giant branch
(RGB) stars in M94's halo, finding two distinct populations. After correcting
for completeness through artificial star tests, we can measure the radial
profile of each RGB population. The metal-rich RGB stars show an unbroken
exponential profile to a radius of 30 kpc that is a clear continuation of M94's
outer disk. M94's metal poor stellar halo is detectable over a wider area and
clearly separates from its metal-rich disk. By integrating the halo density
profile, we infer a total accreted stellar mass of $\sim 2.8 \times 10^8
M_\odot$, with a median metallicity of [M/H] $=-$1.4. This indicates that M94's
most-massive past merger was with a galaxy similar to, or less massive than,
the Small Magellanic Cloud. Few nearby galaxies have had such a low-mass
dominant merger; therefore we suggest that M94's pseudobulge was not
significantly impacted by merging.
