  The active galaxy NGC 1275 lies at the center of the Perseus cluster of
galaxies, being an archetypal BH-galaxy system that is supposed to fit well
with the M_BH-host scaling relations obtained for quiescent galaxies. Since it
harbours an obscured AGN, only recently our group has been able to estimate its
black hole mass. Here our aim is to pinpoint NGC 1275 on the less dispersed
scaling relations, namely the M_BH-sigma_star and M_BH-L_bul planes. Starting
from our previous work Ricci et al. 2017b, we estimate that NGC 1275 falls well
outside the intrinsic dispersion of the M_BH-sigma_star plane being ~1.2 dex
(in black hole mass) displaced with respect to the scaling relations. We then
perform a 2D morphological decomposition analysis on Spitzer/IRAC images at 3.6
mic and find that, beyond the bright compact nucleus that dominates the central
emission, NGC 1275 follows a de Vaucouleurs profile with no sign of significant
star formation nor clear merger remnants. Nonetheless, its displacement on the
M_BH-L_(3.6,bul) plane with respect to the scaling relation is as high as
observed in the M_BH-sigma_star.
