Rotation periods for stars of the TW Hydrae association: the evidence for two spatially and rotationally distinct pre-main-sequence populations

We have conducted a photometric study of late-type members of the TW Hydrae association (TWA) and measured the rotation periods for 16 stars in 12 systems. For TWA stars listed by Webb et al. and Sterzik et al. (TWA 1-13; led by TW Hya = TWA 1) we find a median period of 4.7 d. However, for stars that we measured in the TWA 14-19 group identified by Zuckerman et al., we find a median period of only 0.7 d. The period distributions of the two groups cannot be reconciled at the 3sigma significance level. Using photometric arguments supported by the Hipparcos distance to HD 102458 ( = TWA 19A), we find that TWA 14-19 reside at an average distance of d approximate to 90 pc, spatially at the near boundary of the Lower Centaurus-Crux (LCC) subgroup of the Ophiuchus-Scorpius-Centaurus OB-star association. Proper motions for HD 102458, TWA 14, 18 and 19B link these stars to the LCC subgroup. From Hertzsprung-Russell diagram placement, we derive an age of approximate to 17 Myr for the HD 102458 system that may be the representative age for the TWA 14-19 group. Merging various lines of evidence, we conclude that these stars form a spatially and rotationally distinct population of older pre-main-sequence (PMS) stars, rather than being an extension of the TWA beyond those stars associated with TW Hya that have an age of similar to10 Myr and reside at d approximate to 55 pc. Instead, TWA 14-19 likely represent the population of low-mass stars still physically associated with the LCC subgroup.