2000A&A...353..917L

In this paper we analyze the line-strength indices in the Lick-system measured by Longhetti et al. (1998A&AS..130..251L, 1998A&AS..130..267L) for a sample of 51 early-type galaxies located in low density environments (LDE) and showing signatures of fine structures and/or interactions. The sample contains 21 shell-galaxies and 30 members of interacting pairs. Firstly we perform a preliminary comparison between three different sources of calibrations of the line strength indices, namely Buzzoni et al. (1992AJ....103.1814B, 1994AJ....107..513B), Worthey (1992ApJ...398...69W), Worthey et al. (1994ApJS...94..687W) and Idiart et al. (1995AJ....109.2218I), derived from stars with different effective temperature, gravity, and metallicity. Looking at the three indices in common, i.e. Mg2, Fe5270, and Hβ, the calibrations by Buzzoni et al. (1992AJ....103.1814B, 1994AJ....107..513B), Worthey (1992ApJ...398...69W) and Worthey et al. (1994ApJS...94..687W) lead to mutually consistent results. The calibration of Hβ by Idiart et al. (1995AJ....109.2218I) can be compared with the previous ones only for a limited range of ages, in which good agreement is found. Mg2 and Mgb indices predicted by the Idiart's et al. (1995AJ....109.2218I) fitting functions result to be systematically lower than those obtained from using Worthey (1992ApJ...398...69W) calibrations. Secondly, we discuss the properties of the galaxies in our sample by comparing them both with theoretical Single Stellar Populations (SSPs) and the normal galaxies of the Gonzalez (1993, Ph.D. thesis: G93) sample. The analysis is performed by means of several diagnostic planes. In the σ, Mg2, Fe5270 and Fe5335 space, normal, shell- and pair-galaxies have a different behavior. First of all, normal and pair-galaxies follow the universal σ vs. Mg2 relation, whereas shell-galaxies lie above it; secondly the Fe versus Mg2 relation of normal, shell- and pair-galaxies is flatter than the theoretical expectation. This fact hints for enhancement of α-elements with respect to solar partition in galaxies with strong Fe indices and/or high velocity dispersion, mass and luminosity in turn. In the σ vs. Hβ plane normal galaxies seem to follow a nice relation suggesting that objects with shallow gravitational potential have strong Hβ values (youth signature?), whereas shell- and pair-galaxies scatter all over the plane. A group of galaxies with deep gravitational potential and strong Hβ is found. Is this a signature of recent star formation? In the Hβ vs. [MgFe] plane, which is perhaps best suited to infer the age of the stellar populations, the peculiar galaxies in our sample show nearly the same distribution of the normal galaxies in the G93 sample. There is however a number of peculiar galaxies with much stronger Hβ. Does this mean that the scatter in the Hβ vs. [MgFe] plane, of normal, shell- and pair-galaxies has a common origin, perhaps a secondary episode of star formation? We suggest that, owing to their apparent youth, shell- and pair-galaxies should have experienced at least one interaction event after their formation. The explanation comes natural for shell- and pair-galaxies where the signatures of interactions are evident. It is more intrigued in normal galaxies (perhaps other causes may concur). Noteworthy, the distribution in the Hβ vs. [MgFe] plane of normal, shell- and pair-galaxies is confined within a narrow strip that runs significantly steeper than the path followed by aging SSPs. This feature is explained as due to metal enrichment always accompanying star formation. Shell-galaxies encompass the whole range of ages inferred from the Hβ vs. [MgFe] plane, indicating that among them recent and old interaction/acquisition events are equally probable. If shells are formed at the same time at which the rejuvenating event took place, shells ought to be long lasting phenomena.