2000/07/27 by G. Gavazzi, Gavazzi, G., P. Franzetti +7
Environmental Science · Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Impact of Light on Environment and Health #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0007411
LaTex, 17 pages, 16 figures, accepted for publication in A&A
arxiv created 2000/07/27 · openalex publication_date 2000/07/27 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We present near-infrared H-band (1.65 micron) surface brightness profile decomposition for 1157 galaxies in five nearby clusters of galaxies: Coma, A1367, Virgo, A262 and Cancer, and in the bridge between Coma and A1367 in the "Great Wall". The optically selected (mp<=16.0) sample is representative of all Hubble types, from E to Irr+BCD, except dE and of significantly different environments, spanning from isolated regions to rich clusters of galaxies. We model the surface brightness profiles with a de Vaucouleurs r^(1/4) law (dV), with an exponential disk law (E), or with a combination of the two (B+D). From the fitted quantities we derive the H band effective surface brightness (mue) and radius (re) of each component, the asymptotic magnitude HT and the light concentration index C31. We find that: i) Less than 50% of the Elliptical galaxies have pure dV profiles. The majority of E to Sb galaxies is best represented by a B+D profile. All Scd to BCD galaxies have pure exponential profiles. ii) The type of decomposition is a strong function of the total H band luminosity (mass), independent of the Hubble classification: the fraction of pure exponential decompositions decreases with increasing luminosity, that of B+D increases with luminosity. Pure dV profiles are absent in the low luminosity range LH<10^(10) Lsolar and become dominant above 10^(11) Lsolar.