• DOI:10.1051/0004-6361/201322758
• Corpus ID: 119278062

The IACOB project - I. Rotational velocities in northern Galactic O- and early B-type stars revisited. The impact of other sources of line-broadening

@article{SimonDiaz2014TheIP,
  title={The IACOB project - I. Rotational velocities in northern Galactic O- and early B-type stars revisited. The impact of other sources of line-broadening},
  author={Sergio Sim'on-D'iaz and Artemio Herrero},
  journal={Astronomy and Astrophysics},
  year={2014},
  volume={562}
}

• S. Sim'on-D'iaz, A. Herrero
• Published 14 November 2013
• Physics
• Astronomy and Astrophysics

Context. Stellar rotation is an important parameter in the evolution of massive stars. Accurate and reliable measurements of projected rotational velocities in large samples of OB stars are cruci al to confront the predictions of stellar evolutionary mode ls with observational constraints. Aims. We reassess previous determinations of projected rotational velocities (v sin i) in Galactic OB stars using a large, high quality spectroscopic dataset, and a strategy which account for other sources of broadening appart from rotation affecting the diagnostic lines Methods. We present a versatile and user friendly IDL tool — based on a combined Fourier Transform (FT)+ goodness of fit (GOF) methodology — for the line-broadening characterization in OB-type stars. We use this tool to (a) investigate the impact of macroturbulent and microturbulent broadenings on v sin i measurements, and (b) determine v sin i in a sample of∼ 200 Galactic OB-type stars, also characterizing the amount of macroturbulentbroadening (vm) affecting the line profiles. Results. We present observational evidence illustrating the strengths and limitations of the proposed FT+GOF methodology for the case of OB stars. We confirm previous statements (based on ind irect arguments or smaller samples) that the macroturbulent broadening is ubiquitous in the massive star domain. We compare the newly derived v sin i in the case of O stars and early-B Supergiants and Giants (where the effect of macroturbulence is found to be larger) with previous determinations not accounting for this extra line-broadening contribution, and show that those cases with v sin i≤ 120 km s −1 need to be systematically revised downwards by∼ 25 (± 20) km s −1 . We suggest that microturbulence may impose an upper limit below which v sin i and vm could be incorrectly derived by means of the proposed methodology as presently used, and discuss the implications of this statement on the study of relat ively narrow line massive stars. Conclusions. An investigation of impact of the revised v sin i distributions on the predictions by massive star evolution ary models is now warranted. Also, the reliability of v sin i measurements in the low v sin i regime, using a more precise description of the intrinsic profiles used for the line-broadening analysis, needs to be f urther investigated.