Rotation and activity in late-type members of the young cluster ASCC 123

Abstract

ABSTRACT ASCC 123 is a little-studied young and dispersed open cluster. Recently, we conducted the first research devoted to it. In this paper, we complement our previous work with Transiting Exoplanet Survey Satellite (TESS) photometry for the 55 likely members of the cluster. We pay special attention to seven of these high-probability members, all with FGK spectral types, for which we have high-resolution spectra from our preceding work. By studying the TESS light curves of the cluster members, we determine the rotational period and the amplitude of the rotational modulation for 29 objects. The analysis of the distribution of the periods allows us to estimate a gyrochronological age for ASCC 123 similar to that of the Pleiades, confirming the value obtained in our previous investigation. A young cluster age is also suggested by the distribution of variation amplitudes. In addition, for those stars with spectroscopic data, we calculate the inclination of their rotation axis. These values appear to follow a random distribution, as already observed in young clusters, with no indication of spin alignment. However, our sample is too small to confirm this on more solid statistical grounds. Finally, for these seven stars, we study the level of magnetic activity from the Hα and Ca ii H&K lines. Despite the small number of data points, we find a correlation of the Hα and Ca ii flux with Rossby number. The position of these stars in flux–flux diagrams follows the general trends observed in other active late-type stars.