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The near-IR M bh – L and M bh – n relations

We present near-infrared (near-IR) surface photometry (2D proﬁling) for a sample of 29 nearby galaxies for which supermassive black hole (SMBH) masses are constrained. The data are derived from the UKIDSS-LAS representing a signiﬁcant improvement in image quality and depth over previous studies based on Two Micron All Sky Survey data. We derive the spheroid luminosity and spheroid S´ersic index for each galaxy with GALFIT 3 and use these data to construct SMBH mass–bulge luminosity ( M bh – L ) and SMBH–S´ersic index ( M bh – n ) relations. The best-ﬁtting K -band relation for elliptical and disc galaxies is log ( M bh /M (cid:2) ) = − 0.36( ± 0.03)( M K + 18) + 6.17( ± 0.16), with an intrinsic scatter of 0.4 + 0 . 09 − 0 . 06 dex, whilst for elliptical galaxies we ﬁnd log ( M bh /M (cid:2) ) = − 0.42( ± 0.06)( M K + 22) + 7.5( ± 0.15), with an intrinsic scatter of 0.31 + 0 . 087 − 0 . 047 dex. Our revised M bh – L relation agrees closely with the previous near-IR constraint by Graham. 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, 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.