The VLT-FLAMES survey of massive stars: atmospheric parameters and rotational velocity distributions for B-type stars in the Magellanic Clouds

TL;DR

This study provides homogeneous measurements of atmospheric parameters and rotational velocities for ~400 massive B-type stars in the Magellanic Clouds, revealing insights into stellar evolution, rotation, and potential GRB progenitors.

Contribution

It offers the first comprehensive, homogeneous dataset of atmospheric parameters and rotational velocities for massive stars in the Magellanic Clouds, and compares these with Galactic stars to inform stellar evolution models.

Findings

SMC stars rotate faster than Galactic stars at 3sigma confidence.

Rotational velocity distributions are modeled as Gaussians peaking at 175km/s (SMC) and 100km/s (LMC).

Fast rotation in 10-25Msun stars supports their potential as GRB progenitors.

Abstract

We provide atmospheric parameters and rotational velocities of a large sample (~400) of O- and early B-type stars, analysed in a homogeneous and consistent manner, for use in constraining theoretical models. Comparison of the rotational velocities with evolutionary tracks suggest that the end of core hydrogen burning occurs later than currently predicted. We also show that the large number of the luminous blue supergiants observed in the fields are unlikely to have directly evolved from main-sequence massive O-type stars as neither their low rotational velocities or position on the H-R diagram are predicted. We suggest that blue-loops or mass-transfer binary systems may populate the blue supergiant regime. By comparing the rotational velocity distributions of the Magellanic Cloud stars to a similar Galactic sample we find that (at 3sigma confidence level) massive stars (above 8Msun) in the SMC rotate faster than those in the solar neighbourhood. However there appears to be no significant difference between the rotational velocity distributions in the Galaxy and the LMC. We find that the vsini distributions in the SMC and LMC can modelled with an intrinsic rotational velocity distribution which is a Gaussian peaking at 175km/s (SMC) and 100km/s (LMC). We find that in NGC346 in the SMC, the 10-25Msun main-sequence stars appear to rotate faster than their higher mass counterparts. Recently Yoon et al. (2006) have determined rates of GRBs by modelling rapidly rotating massive star progenitors. Our measured rotational velocity distribution for the 10-25Msun stars is peaked at slightly higher velocities than they assume, supporting the idea that GRBs could come from rapid rotators with initial masses as low as 14Msun at low metallicities. (abridged).