Rotational velocities of A-type stars ?;?? I. Measurement of v sini in the southern hemisphere

By F. Royer, S. Grenier, M. Baylac, A. Gómez, J. Zorec. 2001

167 citations recorded by the source corpus.

Within the scope of a Key Programme determining fundamental parameters of stars observed by HIPPARCOS, spectra of 525 B8 to F2-type stars brighter than V = 8 have been collected at ESO. Fourier transforms of several line proles in the range 4200{4500 A are used to derive v sini from the frequency of the rst zero. Statistical analysis of the sample indicates that measurement error is a function of v sini and this relative error of the rotational velocity is found to be about 6% on average. The results obtained are compared with data from the literature. There is a systematic shift from standard values from Slettebak et al. (1975), which are 10 to 12% lower than our ndings. Comparisons with other independent v sini values tend to prove that those from Slettebak et al. are underestimated. This eect is attributed to the presence of binaries in the standard sample of Slettebak et al., and to the model atmosphere they used.

Subfields: Astronomy and Astrophysics, Computational Mechanics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1d6b11a378821841ecb5d35659345e311bf386dc

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In Astronomy and Astrophysics

1. J. Winn
2. J. Southworth
3. G. Torres
4. Lars A. Buchhave
5. F. Royer
6. Debra A. Fischer
7. J. Carter
8. J. Zorec

In Computational Mechanics

1. Debra A. Fischer
2. F. Royer
3. A. Paris
4. Lars A. Buchhave
5. G. Torres
6. I. D. Paris
7. J. Zorec

In Instrumentation

1. J. Winn
2. G. Torres
3. Lars A. Buchhave
4. J. Zorec
5. F. Royer
6. S. Simón-Díaz
7. M. Holman
8. J. Carter

Citations in the corpus

• A Medium Resolution Near-Infrared Spectral Atlas of O and Early-B Stars (2005, unknown): “A0 V 191 a From Royer et al. (2002a, 2002b).”
• Rotational Velocities of B Stars (2002, background): “On the other hand, Royer et al. (2002) have derived a new set of standards for B8–F2 stars usingHipparcos parallaxes, new model atmospheres, and measured rotational velocities derived with Fourier transforms.”
• IMPROVED SPECTROSCOPIC PARAMETERS FOR TRANSITING PLANET HOSTS (2012, methodology): “Part of this may be related to differences in the continuumfitting algorithms used in the two techniques (see, e.g., Behr 2003; Royer et al. 2002a,b; Glazunova et al. 2008; Improved spectroscopic parameters 5 Fig.”
• Rotational velocities of A-type stars. III. Velocity distributions (2006, methodology): “We preferred then to base our study on two homogeneous data sets: the v sin i obtained using the Fourier transform method (FT) by Royer et al. (2002a,b, hereafter Papers I and II, or I ∪ II) and the v sin i determined by Abt & Morrell (1995, hereafter called AM) and Abt et al. (2002, hereafter calle”
• Fourier method of determining the rotational velocities in OB stars (2007, methodology): “There are numerous papers illustrating its use in determining v sin i in later type stars (Smith 1976; Gray 1980; Royer et al. 2002a,b; Reiners & Schmitt 2003); however, there is no comprehensive study applying this technique to early-type stars except the one by Ebbets (1979), who analyzed a…”
• A possible black hole in the γ-ray microquasar LS 5039 (2005, methodology): “Alternatively, we attempted a refined determination following the Fourier technique described by Gray (1992); for a recent application see Royer et al. (2002).”