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The main results of a new analysis of the spheroidal (I) and disk (II) components of 98 lenticular and spiral galaxies are :
(i)on the average, the magnitude difference between spheroid and total luminosity, ΔmI = BT(I) - BT, varies smoothly along the Hubble sequence from early lenticulars to late-type spirals (Fig. 1);
(ii)the trend of ΔmI confirms the concept of the lenticular class as intermediate between E and S classes, not as a parallel sequence;
(iii)the large scatter at any given type, σ(ΔmI) ≃ 0.7 mag, is still dominated by measuring and decomposition errors.
(iv)The effective surface brightness of the spheroid, μce(I), corrected for galactic extinction AB, decreases by ~2 mag from early to late types, but with a large range (~ 3 mag) at T = const. (Fig. 2a).
(v)The effective surface brightness of the disks, corrected for galactic extinction and inclination, μce(II) = μe(II)- AB + 3 log R2s, is almost independent of type, with <μce(II)> ≃ 23.5 for spirals. This implies a corrected central surface brightness μc(0) = μce −1.82 ≃ 21.7, in good agreement with the Freeman rule, but with a large scatter. However, the disks of lenticulars (T< 0) tend to be ~ 0.5 mag fainter than the disks of spirals (Fig. 2b).
(vi)The linear effective radii of the spheroidal components are largest, <re (I)> ≳ 1 kpc, among the early type spirals, in agreement with the Hubble classification criterion. The spheroid of lenticulars and late-type spirals tend to be smaller, <re(I)> ≃ 0.5 kpc, but with a large scatter (Fig. 3a). There is no indication of systematic difference between ordinary (SA) and barred (SB) spirals.
(vii)The linear effective radii of the disk components are largest <re (I)> ≳ 5 kpc, among intermediate type spirals. The disks of lenticular and late type spirals tend to be smaller (Fig. 3b).
(viii)The mean absolute magnitudes of the disk and spheroidal components depend on type (Fig. 4). On the average the disks are brighter (MII ≃ −19.5) among types Sb-Sbc, spheroids (MI ⋍ −19) among types L+ to Sa, but, again, with a large scatter. Disks and spheroids are about equally bright (MI ⋍ MII ⋍ − 19) at stage SO/a (T = 0).
We present measurements of stellar kinematics for seven early-type galaxies in HCG 67, HCG 74 and HCG 79. These data are aimed at studying the relation between the environment and the dynamics, structure and stellar content of early-type galaxies. In the present three groups, the kinematic features we observed cannot be associated unambiguously to physical interactions. Visible morphological peculiarities do not appear correlated with kinematical perturbations.
1) Photometry from de Vaucouleurs 1958 shows a bulge obeying the r1/4 law up to less than 5 pc from the center with an effective radius re = 17′5. In the region from 0.01 to 0.2 re, equal luminosity curves are well approximated by similar ellipses of axial ratio 0.68. The reduced spatial density υ* and the reduced gravitationnal potential φ* (i.e. for a mass to luminosity ratio f equal to 1) can then be easily computed (Monnet and Simien 1977).
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