Canis Major OB1 stellar group contents revealed by Gaia. Issue 1 (1st October 2021)

• Record Type: Journal Article
• Authors: Santos-Silva, T; Perottoni, H D; Almeida-Fernandes, F; Gregorio-Hetem, J; Jatenco-Pereira, V; Mendes de Oliveira, C; Montmerle, T; Bica, E; Bonatto, C; Monteiro, H; Dias, W S; Barbosa, C E; Fernandes, B; Galli, P A B; Borges Fernandes, M; Kanaan, A; Ribeiro, T; Schoenell, W
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 508:Issue 1(2021)
• Page Start: 1033
• Page End: 1055
• Publication Date: 2021-10-01
• Subjects: star: early-type -- stars: formation -- stars: pre-main-sequence -- open clusters and associations: general; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab2409
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Canis Major OB1 (CMa OB1) is a Galactic stellar association with a very intriguing star-formation scenario. There are more than two dozen known star clusters in its line of sight, but it is not clear which ones are physically associated with CMa OB1. We use a clustering code that employs five-dimensional data from the Gaia DR2 catalogue to identify physical groups and obtain their astrometric parameters and, in addition, we use two different isochrone-fitting methods to estimate the ages of these groups. We find 15 stellar groups with distances between 570 and 1650 pc, including 10 previously known and five new open cluster candidates. Four groups, precisely the youngest ones (< 20 Myr), CMa05, CMa06, CMa07, and CMa08, are confirmed to be part of CMa OB1. We find that CMa08, a new cluster candidate, may be the progenitor cluster of runaway stars. CMa06 coincides with the well-studied CMa R1 star-forming region. While CMa06 is still forming stars, due to the remaining material of the molecular cloud associated with the Sh 2-262 nebula, CMa05, CMa07, and CMa08 seem to be in more evolved stages of evolution, with no recent star-forming activity. The properties of these CMa OB1 physical groups fit well in a monolithic scenario of star formation, with a common formation mechanism, and having suffered multiple episodes of star formation. This suggests that the hierarchical model alone, which explains the populations of other parts of the same association, is not sufficient to explain its whole formation history.