1.65 micron (H-band) surface photometry of galaxies. VIII: the near-IR k-space at z=0

Details 1.65 micron (H-band) surface photometry of galaxies. VIII: the near-IR k-space at z=0 1.65 micron (H-band) surface photometry of galaxies. VIII: the near-IR k-space at z=0

2002-01-16

arxiv.org/abs/astro-ph/0201270v1

Mon.Not.Roy.Astron.Soc. 332 (2002) 422

Astronomy and Astrophysics

Astrophysics

11 pages, 1 Postscript table, 3 Postscript figures, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2002.05323.x

We present the distribution of a statistical sample of nearby galaxies in the k-space (k1 ~ log M, k2 ~ log Ie, k3 ~ log M/L). Our study is based on near-IR (H-band: lambda = 1.65 micron) observations, for the first time comprising early- and late-type systems. Our data confirm that the mean effective dynamical mass-to-light ratio M/L of the E+S0+S0a galaxies increases with increasing effective dynamical mass M, as expected from the existence of the Fundamental Plane relation. Conversely, spiral and Im/BCD galaxies show a broad distribution in M/L with no detected trend of M/L with M, the former galaxies having M/L values about twice larger than the latter, on average. For all the late-type galaxies, the M/L increases with decreasing effective surface intensity Ie, consistent with the existence of the Tully--Fisher relation. These results are discussed on the basis of the assumptions behind the construction of the k-space and their limitations. Our study is complementary to a previous investigation in the optical (B-band: lambda = 0.44 micron) and allows us to study wavelength-dependences of the galaxy distribution in the k-space. As a first result, we find that the galaxy distribution in the k1--k2 plane reproduces the transition from bulge-less to bulge-dominated systems in galaxies of increasing dynamical mass. Conversely, it appears that the M/L of late-types is higher (lower) than that of early-types with the same M in the near-IR (optical). The origins of this behaviour are discussed in terms of dust attenuation and star formation history.

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