Bibcode
Nigoche-Netro, A.; Aguerri, J. A. L.; Lagos, P.; Ruelas-Mayorga, A.; Sánchez, L. J.; Machado, A.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 516, id.A96
Fecha de publicación:
6
2010
Revista
Número de citas
29
Número de citas referidas
27
Descripción
Aims: Previous studies have found that the coefficients and
intrinsic dispersions of both the Kormendy relation and the Fundamental
Plane depend on the magnitude range within which the galaxies are
contained. We study whether this type of behaviour is also present for
the Faber-Jackson relation. Methods: We take a sample of
early-type galaxies from the Sloan Digital Sky Survey (SDSS-DR7, ~90 000
galaxies) spanning a range of approximately 7 mag in both g and r
filters and analyse the behaviour of the Faber-Jackson relation
parameters as functions of the magnitude range. We calculate the
parameters in two ways: i) we consider the faintest (brightest) galaxies
in each sample and we progressively increase the width of the magnitude
interval by inclusion of the brighter (fainter) galaxies
(increasing-magnitude-intervals); and ii) we consider narrow-magnitude
intervals of the same width (ΔM = 1.0 mag) over the whole
magnitude range available (narrow-magnitude-intervals). Results:
Our main results are that: i) in both increasing and
narrow-magnitude-intervals the Faber-Jackson relation parameters change
systematically, ii) non-parametric tests show that the fluctuations in
the values of the slope of the Faber-Jackson relation are not products
of chance variations. Conclusions: We conclude that the values of
the Faber-Jackson relation parameters depend on the width of the
magnitude range and the luminosity of galaxies within the magnitude
range. This dependence is caused, to a great extent by the selection
effects and because the geometrical shape of the distribution of
galaxies on the M - log(σ0) plane depends on
luminosity. We therefore emphasize that if the luminosity of galaxies or
the width of the magnitude range or both are not taken into
consideration when comparing the structural relations of galaxy samples
for different wavelengths, environments, redshifts and luminosities, any
differences found may be misinterpreted.
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