2006/09/04 by Eric E. Mamajek · 2 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/508205
published as Astron.J.132:2198-2205,2006 · 23 pages, 3 figs., to appear in Nov. 2006 AJ
arxiv created 2006/09/04 · openalex publication_date 2006/10/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/30
The recent discoveries of nearby star clusters and associations within a few hundred pc of the Sun, as well as the order of magnitude difference in the formation rates of the embedded and open cluster populations, suggests that additional poor stellar groups are likely to be found at surprisingly close distances to the Sun. Here I describe a new nearby stellar aggregate found by virtue of the parallel proper motions, similar trigonometric parallaxes, and consistent color-magnitude distribution of its early-type members. The 120 Myr old group lies in Ophiuchus at d ≃ 170 pc, with its most massive member being the 4th magnitude post-main-sequence B8 II-III star μ Oph. The group may have escaped previous notice due to its nonnegligible extinction ( A V ≃ 0.9 mag). If the group was born with a normal initial mass function, and the nine B- and A-type systems represent a complete system of intermediate-mass stars, then the original population was probably of order ∼200 systems. The age and space motion of the new cluster are very similar to those of the Pleiades, the α Per cluster, and the AB Dor moving group, suggesting that these aggregates may have formed in the same star-forming complex some ∼10 8 yr ago.