  We present an investigation of the scaling relations between Supermassive
Black Hole (SMBH) masses (Mbh), and their host galaxies' K-band bulge (Lbul)
and total (Ltot) luminosities. The wide-field WIRCam imager at the
Canada-France-Hawaii-Telescope (CFHT) was used to obtain the deepest and
highest resolution near infrared images available for a sample of 35 galaxies
with securely measured Mbh, selected irrespective of Hubble type. For each
galaxy, we derive bulge and total magnitudes using a two-dimensional image
decomposition code that allows us to account, if necessary, for large- and
small-scale disks, cores, bars, nuclei, rings, envelopes and spiral arms. We
find that the present-day Mbh-Lbul and Mbh-Ltot relations have consistent
intrinsic scatter, suggesting that Mbh correlates equally well with bulge and
total luminosity of the host. Our analysis provides only mild evidence of a
decreased scatter if the fit is restricted to elliptical galaxies. The
log-slopes of the Mbh-Lbul and Mbh-Ltot relations are 0.75+/-0.10 and
0.92+/-0.14, respectively. However, while the slope of the Mbh-Lbul relation
depends on the detail of the image decomposition, the characterization of
Mbh-Ltot does not. Given the difficulties and ambiguities of decomposing galaxy
images into separate components, our results indicate that Ltot is more
suitable as a tracer of SMBH mass than Lbul, and that the Mbh-Ltot relation
should be used when studying the co-evolution of SMBHs and galaxies.
