The near-IR $M_{bh}$ - L and $M_{bh}$ - n relations
  We present near-IR surface photometry (2D-profiling) for a sample of 29
nearby galaxies for which super-massive black hole (SMBH) masses are
constrained. The data is derived from the UKIDSS-LASS survey representing a
significant improvement in image quality and depth over previous studies based
on 2MASS data. We derive the spheroid luminosity and spheroid S\'ersic index
for each galaxy with GALFIT3 and use these data to construct SMBH mass -bulge
luminosity ($M_{\rm bh}$--$L$) and SMBH - S\'ersic index ($M_{\rm bh}$--$n$)
relations. The best fit K-band relation for elliptical and disk galaxies is
$\log(M_{\rm bh}/M_{\odot})= -0.36(\pm 0.03) (M_{\rm K} + 18) + 6.17(\pm 0.16)$
with an intrinsic scatter of 0.4$^{+0.09}_{-0.06}$dex whilst for elliptical
galaxies we find $\log(M_{\rm bh}/M_{\odot})= -0.42(\pm 0.06) (M_{\rm K} + 22)
+ 7.5(\pm 0.15)$ with an intrinsic scatter of 0.31$^{+0.087}_{-0.047}$dex. Our
revised $M_{\rm bh}$--$L$ relation agrees closely with the previous near-IR
constraint by \citet{tex:G07}. The lack of improvement in the intrinsic scatter
in moving to higher quality near-IR data suggests that the SMBH relations are
not currently limited by the quality of the imaging data but is either
intrinsic or a result of uncertainty in the precise number of required
components required in the profiling process. Contrary to expectation (see
\citealt{tex:GD07a}) a relation between SMBH mass and the S\'ersic index was
not found at near-IR wavelengths. This latter outcome is believed to be
explained by the generic inconsistencies between 1D and 2D galaxy profiling
which are currently under further investigation.
