  We present XMM-Newton observations of the Chandra-detected nuclear X-ray
source in NGC 4561. The hard X-ray spectrum can be described by a model
composed of an absorbed power-law with Gamma= 2.5^{+0.4}_{-0.3}, and column
density N_H=1.9^{+0.1}_{-0.2} times 10^{22} atoms cm^{-2}. The absorption
corrected luminosity of the source is L(0.2 - 10.0 keV) = 2.5 times 10^{41}
ergs s^{-1}, with bolometric luminosity over 3 \times 10^{42} ergs s^{-1}.
Based on the spectrum and the luminosity, we identify the nuclear X-ray source
in NGC 4561 to be an AGN, with a black hole of mass M_BH > 20,000 solar masses.
The presence of a supermassive black hole at the center of this bulge-less
galaxy shows that black hole masses are not necessarily related to bulge
properties, contrary to the general belief. Observations such as these call
into question several theoretical models of BH--galaxy co-evolution that are
based on merger-driven BH growth; secular processes clearly play an important
role. Several emission lines are detected in the soft X-ray spectrum of the
source which can be well parametrized by an absorbed diffuse thermal plasma
with non-solar abundances of some heavy elements. Similar soft X-ray emission
is observed in spectra of Seyfert 2 galaxies and low luminosity AGNs,
suggesting an origin in the circumnuclear plasma.
