  Although supermassive black holes (SMBHs) reside in the heart of virtually
every massive galaxy, it remains debated whether dwarf galaxies also commonly
host SMBHs. Because low-mass galaxies may retain a memory of the assembly
history of their black holes, probing the black hole occupation fraction of
local dwarf galaxies might offer insights into the growth and seeding
mechanisms of the first black holes. In this work, we exploit the Western half
of the eROSITA all-sky survey (covering $20,000~\rm{deg^2}$) and compile a
catalog of accreting SMBHs in local ($D<200$~Mpc) dwarf galaxies. After
cleaning our sample from cosmic X-ray background sources, X-ray binaries, and
ultraluminous X-ray sources, we identify 74 AGN-dwarf galaxy pairs. Using this
large and uniform sample, we derive a luminosity function of dwarf galaxy AGN,
fitting it with a power law function and obtaining ${\rm d}N/{\rm d}L_{\rm X} =
(15.9\pm2.2)\times L_{\rm X}^{-1.63\pm0.05}$. Measuring the offset between the
centroid of dwarf galaxies and the X-ray sources, we find that about $50\%$ of
the AGN are likely off-nuclear, in agreement with theoretical predictions. We
also compare the black hole-to-stellar mass relation of the AGN in our sample
with the local and high-redshift relations, finding that our sources better
adhere to the former. This suggests that local AGN across different mass scales
underwent a similar growth history. Finally, we compare our sources with
semi-analytical models: while our sample is too shallow to distinguish between
different seeding models, it favors a growth mechanism linked to the
star-formation rate of the host galaxy.
