Abstract
We have compared the frequency distribution of the dynamical observedquantity log (V z 2 r p), for a sample of 46 pairs of elliptical galaxies, to the distribution of this quantity obtained from numerical simulations of pairs of galaxies. From such an analysis, where we have considered the structure of the galaxies and its influence in the orbital evolution of the system, we have obtained the characteristic mass and the mass-luminosity ratio for the sample. Our results show that the hypothesis of point-mass in elliptical orbits is, for this sample, an approximation as good as the model that takes into account the structure of the galaxies. The statistical method used here gives an estimate of a more reliable mass, it minimizes the contamination of spurious pairs and it considers adequately the contribution of the physical pairs. We have obtained a characteristic mass to the 46 elliptical pairs of 1.68 × 1012 ± 7.01 ×1011 M⊙ with M/L = 17.6 ± 7.3 (H 0 = 60 km s-1Mpc-1).
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Junqueira, S., Chan, R. Mass of Galaxies in Pairs. Astrophysics and Space Science 279, 271–280 (2002). https://doi.org/10.1023/A:1015179911087
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DOI: https://doi.org/10.1023/A:1015179911087