  Most galaxies with a well-structured bulge host a supermassive black hole
(SMBH) in their centre. Stellar kinematics models applied to adaptive optics
(AO) assisted integral field unit observations are well-suited to measure the
SMBH mass ($M_{BH}$) and also the total mass-to-light ratio [$(M/L)_{TOT}$] and
possible anisotropies in the stellar velocity distribution in the central
region of galaxies. In this work, we used new AO assisted Near-Infrared
Integral Field Spectrometer (NIFS) observations and also photometric data from
the Hubble Space Telescope Legacy Archive of the galaxy NGC 4546 in order to
determine its SMBH mass. To do this, we applied the Jeans Anisotropic Modelling
(JAM) method to fit the average second velocity moment in the line of sight
$(\overline{v^2_{los}})$ of the stellar structure. In addition, we also
obtained $(M/L)_{TOT}$ and the classical anisotropy parameter
$\beta_z$=1--($\sigma_z$/$\sigma_R$)$^2$ for this object within a field of view
of 200$\times$200 pc$^2$. Maps of the stellar radial velocity and of the
velocity dispersion were built for this galaxy using the penalized pixel
fitting ({\sc ppxf}) technique. We applied the Multi Gaussian Expansion
procedure to fit the stellar brightness distribution. Using JAM, the
best-fitting model for $\overline{v^2_{los}}$ of the stellar structure was
obtained with $(M/L)_{TOT}$ = 4.34$\pm$0.07 (Johnson's R band), $M_{BH}$ =
(2.56$\pm$0.16)$\times$10$^8$ M$_\odot$ and $\beta_z$ = --0.015$\pm$0.03
(3$\sigma$ confidence level). With these results, we found that NGC 4546
follows the $M_{BH}$ $\times$ $\sigma$ relation. We also measured the central
velocity dispersion within a radius of 1 arcsec of this object as $\sigma_c$ =
241$\pm$2 km s$^{-1}$.
