Proper motions of OB stars in the far Carina Arm

TL;DR

This study analyzes the proper motions of over 4000 OB stars in the far Carina Arm, revealing complex kinematic patterns, a moving group, and ejection hot spots linked to specific star clusters, enhancing understanding of Galactic structure and star ejection processes.

Contribution

It provides the first detailed proper motion analysis of OB stars in the far Carina Arm, identifying kinematic perturbations, a moving group, and ejection hot spots associated with specific clusters.

Findings

Proper motion pattern shows a saw-tooth modulation with ~1 mas/yr amplitude.

Identified a moving group of over 50 OB stars behind the main arm.

Estimated at least 10 ext{--}20\% of OB stars are runaways, with ejection linked to NGC 3603 and Westerlund 2.

Abstract

In large scale maps of the Galactic disc, the Carina Arm stands out as a clear spiral feature, hosting prominent star clusters and associations rich in massive stars. We study the proper motions of 4199 O and early B most likely in the far Carina Arm, at distances mainly in excess of 4 kpc from the Sun, within the sky region, $282^{\circ} < \ell < 294^{\circ}$ and $-3^{\circ} < b < +1^{\circ}$ (Galactic coordinates). The sample is constructed by extending an existing blue-selected catalogue, and cross-matching with Gaia EDR3 astrometry. The observed pattern of proper motions is modulated into a saw-tooth pattern, with full amplitude approaching 1 mas yr$^{-1}$, recurring roughly every 2--3 degrees of longitude (200--300 pc at the median OB-star distance of 5.8 kpc). Kinematic perturbation of underlying circular rotation is most likely present. The data also reveal a moving group containing $>50$ OB stars at $\ell \sim 286^{\circ}$, $b \sim -1^{\circ}.4$ behind the main run of the far arm. An analysis of relative proper motions is performed that yields an incidence of runaway O stars of at least 10\% (potentially $>20$\% when full space motions become available). To map where runaways have run away from, we set up simulations for the region that assume linear trajectories and test for trajectory impact parameter in order to identify likely ejection hot spots. We find the method currently gives good results for times of flight of up to $\sim$4 Myr. It shows convincingly that only NGC 3603 and Westerlund 2 have ejected OB stars in significant numbers. Indeed, both clusters have experienced intense spells of ejection between 0.6--0.9 and 0.5--0.8 Myr ago, respectively.