  The presence of young massive stars in the Galactic Centre (GC) raises
questions about star formation near the black hole Sagittarius A* (Sgr A*).
Additionally, the initial mass function (IMF) in this region appears different
from the standard Salpeter/Kroupa law. Extreme extinction and crowding limit
our understanding of the stellar population, with spectroscopic data available
only for selected bright sources. We aim to improve knowledge about the
distribution and IMF of young, massive stars near Sgr A*. Using intermediate
band (IB) photometry, we identify candidates for massive young stars through
Bayesian inference, a neural network, and a gradient-boosted trees algorithm.
We obtained spectral energy distributions for 6590 stars, 1181 of which have
been previously classified spectroscopically. We identify 351 stars classified
as early types by all three methods, including 155 newly identified candidates.
The radial density profiles for late and early-type stars fit broken power
laws, with a break radius of 9.2 +- 0.6'' for early-type stars. Late-type stars
show a core-like distribution around Sgr A*, while early-type stars' density
increases steeply towards the black hole. We infer a top-heavy IMF of young
stars near Sgr A* (R < 9''), with a power-law of 1.6 +- 0.1. At greater
distances, a standard Salpeter/Kroupa IMF fits the data. IB photometry also
constrains the metallicities of late-type stars, estimating metallicities for
over 600 stars. The IMF variation with radial distance suggests different star
formation mechanisms, with a top-heavy IMF near Sgr A* consistent with disc
star formation.
