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$\begin{figure} \par\includegraphics[width=16.9cm,clip]{9958.eps}\end{figure}$ Figure 1: This plot shows the relationship between the luminosities and the diameters of Shapley-Ames galaxies within 10 Mpc. Also shown as a solid line is the luminosity-diameter relation for the Virgo cluster according to Girardi et al. (1991). Figure 1A shows that nearby galaxies and those in the Virgo cluster follow the same power-law relationship. The deviant galaxy NGC 1569 is plotted as a plus sign. The Milky Way system is shown as a small circle. Figure 1B shows the Luminosity-Diameter relation for galaxies in clusters (red squares), in groups (green circles) and in the field (blue triangles). The Milky Way System is shown as a green circle. The figure shows a surprising absence of dependence of position in this diagram on environment. Figure 1C shows the Luminosity-Diameter relation for galaxies with $\theta < 0$ , which may be considered as undisturbed isolated objects (red squares). Galaxies with $\theta > 0$ , are plotted as blue triangles. These objects have Keplerian cyclical periods smaller than the Hubble time 1/H₀. The small blue circle represents the Milky Way System. The plot shows no evidence for a clear-cut relationship between the Karachentseve & Malakov tidal index and deviations from the mean luminosity-diameter relation. Finally Fig. 1D shows the luminosity-diameter relation for early-type (E+S0+S0/Sa) galaxies (red squares) and late type (Sc, Scd, Sd, Sm, Im) galaxies (blue triangles). Not unexpectedly this figure shows that at, a given luminosity, early-type galaxies are (on average) slightly more compact than are objects of later morphological types.
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