Investigating the possible connection between lambda Bootis stars and intermediate Population II type stars

TL;DR

This study compares lambda Bootis stars with intermediate Population II stars, analyzing their elemental abundances and kinematic properties to explore potential intrinsic links or distinctions between these stellar groups.

Contribution

It provides the first detailed abundance and kinematic comparison between lambda Bootis and intermediate Population II stars, clarifying their similarities and differences.

Findings

No kinematic distinction between intermediate Population II and F-weak stars.

Lambda Bootis stars are chemically distinct from intermediate Population II stars.

Intermediate Population II and F-weak stars are essentially the same group.

Abstract

The lambda Bootis (LB) stars are located at the upper main sequence of the H-R diagram and exhibit a peculiar abundance pattern. The light elements (C, N, O, and S) present solar abundances whereas all other elements are moderately to strongly underabundant. It has not yet been determined whether that abundance pattern is intrinsic, or is restricted to the stellar surface. If we follow the hypothesis that the LB stars are intrinsically metal-weak, then there should be a connection with the intermediate Population II and F-weak objects. Such a possible affinity has not been previously investigated. We present detailed elemental abundances, including those of the light elements carbon and oxygen, for 38 bright intermediate Population II and F-weak objects. In addition, we investigate the kinematic characteristics of the groups. From photometric, spectroscopic, and kinematic data, there is no distinction between the intermediate Population II and F-weak type stars. We therefore conclude that the two groups are identical. However, it is possible to distinguish the LB stars from the intermediate Population II stars on the basis of elemental abundances, though not in terms of their kinematics. The LB stars seem to be distinct from the intermediate Population II group. Further asteroseismologic investigations and analyses of spectroscopic binary systems are needed to strengthen this conclusion.