EDP Sciences
Free Access
Issue
A&A
Volume 561, January 2014
Article Number A126
Number of page(s) 4
Section Catalogs and data
DOI https://doi.org/10.1051/0004-6361/201220762
Published online 21 January 2014

© ESO, 2014

1. Introduction

Over the past two decades, observations have been carried out at the Geneva Observatory, Switzerland, and the Federal University of Rio Grande do Norte, Brazil, to accurately measure projected rotational velocities (v sin i) of evolved stars, with the aim of studying the evolution of stellar rotation with stellar age.

The technique used is to combine a high-resolution spectrometer with the cross-correlation technique, which yields accurate, high S/N cross-correlation line profiles from relatively low S/N spectra. From these profiles, accurate radial velocities and, once calibrated, projected rotational velocities (v sin i) with an accuracy better than 1 km s-1 can be derived, allowing measurements of v sin i for large samples of relatively faint stars with telescopes of moderate aperture.

Table 2

Double-lined spectroscopic binary systems SB2 with evolved component.

Table 3

Evolved stars with no CORAVEL dip.

Most of the observations presented here were made with the CORAVEL cross-correlation spectrometers (Baranne et al. 1979). In addition, De Medeiros et al. (2006) measured rotational velocities, v sin i, for 100 metal-poor stars with the digital version of the cross-correlation procedure, using spectra obtained with the FEROS (Kaufer & Pasquini 1998) and CORALIE (Baranne et al. 1996) spectrometers.

As part of this programme, De Medeiros & Mayor (1999) measured v sin i for 1541 stars of luminosity classes IV, III, and II, De Medeiros et al. (2002b) presented v sin i for 232 Ib supergiant stars, and De Medeiros et al. (2004) also measured v sin i for 78 double-lined binaries with an evolved component. These high-quality data have inspired several studies, enabling reliable investigations of stellar rotational characteristics in different regions of the H−R diagram (Carlberg et al.2011; Cortés et al.2009; Melo et al.2001), the relationship between rotation and different stellar properties (Monaco et al. 2011; Raghavan et al. 2010; López-Santiago et al. 2010; Grunhut et al. 2010; Massarotti et al. 2008; De Medeiros et al. 2002a; Cutispoto et al. 2002), constraints on theoretical models (Eggenberger et al. 2010; Brun & Palacios 2009) and in many studies on extra-solar planets (e.g. Watson et al. 2010; Döllinger et al. 2009).

The present work brings complementary results for our observational efforts, with the measurements of projected rotational velocity v sin i for southern subgiant, giant, bright giant, and Ib supergiant stars of spectral types F, G, and K, listed in the Bright Star Catalog (Hoffleit & Jaschek 1982; Hoffleit et al. 1983). Although the primary aim of this investigation is to study the rotational behaviour of evolved stars, our observational procedure also produced a large set of radial velocity measurements, representing an important tool for answering several questions in stellar astrophysics, including the search for planets around evolved stars.

This paper is arranged as follows. Section 2 presents the definition of the sample, the observational procedure used throughout this survey, and the calibration of rotational velocities, with a discussion of their probable errors. The list of individual v sin i measurements and mean radial velocities are presented in Sect. 3.

2. The observational programme

The present sample consists of a total of 1702 mainly southern F, G, and K stars of luminosity classes IV, III, II, and Ib listed in the Bright Star Catalog. Most of these stars were observed in different programmes carried out at the Geneva Observatory, the majority devoted to studying stellar binarity (Duquennoy et al. 1991; De Medeiros & Mayor 1999; De Medeiros et al. 2002b, 2004) or to precise measurements of radial velocity in programmes on Galactic structure (Andersen et al. 1985; Prevot et al. 1985; Maurice et al. 1987; Nordström et al. 2004a).

As in previous papers (De Medeiros & Mayor 1999; De Medeiros et al. 2002b, 2004), the observations reported here were made using the two CORAVEL spectrometers (Baranne et al. 1979) mounted on the 1.54-m Danish telescope at ESO, La Silla (Chile), and the 1-m Swiss telescope at Haute-Provence Observatory, Saint Michel (France). Radial velocities were derived by direct cross-correlation of the stellar spectra with a binary (0, 1) physical template, constructed from the spectrum of the K2 III star Arcturus and mounted inside the spectrometers. The radial-velocity system applied is that defined by Udry et al. (1999). Typical integration times were 5 min, and data was reducted using standard procedures (Duquennoy 1987; Duquennoy et al. 1991; De Medeiros & Mayor 1999). For a complete discussion of the observational procedure, calibration, and error analysis, readers are referred to Duquennoy (1987), Duquennoy et al. (1991), and De Medeiros & Mayor (1999).

Here, we just recall a few salient points. In all cases, the radial velocity uncertainty is derived from an instrumental error added in quadrature to photon and scintillation noise, which are estimated using the computed parameters of the cross-correlation profiles (Baranne et al. 1979). Different studies of large data samples (Duquennoy et al. 1991; Udry et al. 1997; De Medeiros & Mayor 1999) show that the typical uncertainty for CORAVEL radial velocity is about 0.3 km s-1 for slowly rotating stars, generally with v sin i< 20 km s-1. For faster rotators, the uncertainty is somewhat greater.

Rotational velocities (v sin i) were obtained through an appropriate calibration of the widths of cross-correlation profiles, as described by De Medeiros & Mayor (1999). The original v sin i calibration by Benz & Mayor (1984) is also valid for subgiant and giant stars of luminosity classes IV and III, but for class II and Ib bright giants and supergiants, the increase in macroturbulence with spectral type required a new calibration of the width of the cross-correlation profile into v sin i as measured from a Fourier transform of line profiles from Gray & Toner (1986, 1987). Whereas Benz & Mayor (1984) obtained for the parameter associated with the CORAVEL cross-correlation profiles σ0 the value of 6.88 km s-1 for stars of luminosity classes V to III, the new calibration shows that for the luminosity classes II and Ib the value of σ0 is 7.158 km s-1 and 7.978 km s-1, respectively.

The computed v sin i has a typical uncertainty of around 1.0 km s-1 for subgiant and giant stars with v sin i ≪ 30 km s-1, whereas for bright giants and Ib supergiants, we conservatively assume an uncertainty of 2.0 km s-1, since it is impossible to define precise limits between rotation and macroturbulence. For faster rotators, those with v sin i higher than 30 km s-1, De Medeiros & Mayor (1999) estimate an uncertainty of about 10%, regardless of luminosity class.

3. Contents

The main results of this catalogue are listed in Table 1, which presents CORAVEL rotational and mean radial velocities for 1589 evolved FGK stars of luminosity classes IV, III, II, and Ib, ordered by HD number, for single stars and single-lined spectroscopic binaries. Columns are as follows: 1. HD number; 2. spectral type; 3. (B − V) color index; 4–5. mean radial velocity RV and its uncertainty ϵ, on N number of CORAVEL observations. In this case, the uncertainty is given by max (, ), where ϵ1 is the typical error for one single radial velocity measurement; 6. radial velocity dispersion (rms) σ; 7. E/T, the ratio of observed to expected rms dispersion for observations, when N ≥ 2; 8. P(χ2), the probability that the radial velocity of the star is constant; 9. N, number of observations for each star; 10. time span ΔT of observations; 11–12. rotational velocity Vsini and its uncertainty ϵrot; 13. remarks. The remarks SBO and SB indicate, respectively, single-lined spectroscopic binaries for which orbital parameters are available in the literature, and stars displaying single-lined spectroscopic binary behaviour. Nevertheless, for a few stars classified as SB, the RV variability may reflect another cause, e.g. pulsation.

A number of the programme stars, identified in Table 1, were already included in the papers by Andersen et al. (1985), Prevot et al. (1985), and Maurice et al. (1987), with radial velocities referred to in the 1985 standard system of Udry et al. (1999), while the velocities listed here are referred to in the revised zero-point of Udry et al. (1999). The colour-dependent differences from the earlier velocities are small, about 0.11, 0.31, and 0.45 km s-1 for F-, G-, and K-type stars, respectively, but can be noticed in precise work.

Table 2 lists 79 SB2 and SB3 binary systems also observed by CORAVEL, many of which were detected here for the first time, while Table 3 presents the evolved F-type stars for which no correlation dip was obtained with CORAVEL. These are undoubtedly fast rotators.

The individual radial velocity measurements for single and SBO stars, as well as for SB not included in follow-up programmes, are available at the Centre de Données Astronomiques de Strasbourg (CDS).

Acknowledgments

We gratefully acknowledge the support of the CORAVEL observers in this survey, particularly Gilbert Burki, Bernard Pernier, Pierre North, Jean-Claude Mermilliod and Gerard Jasniewicz. We also thank Emile Ischi and Bernard Tartarat for technical maintenance of the CORAVELs and B. L. Canto Martins, I. C. Leão and J. D. do Nascimento for assistance in preparing tables and data controls. S. Alves acknowledges a graduate fellowship and a PNPD fellowship from the CAPES Brazilian agency. This study used the SIMBAD database, operated at the CDS in Strasbourg, France, and it was supported by continuous grants from the Swiss National Science Foundation. Research activities of the Observational Stellar Board of the Federal University of Rio Grande do Norte are supported by the Brazilian agencies CNPq, FAPERN, and the INCT INEspaço. The observations at the Danish 1.54 m telescope from ESO, La Silla, Chile, was supported by grants from ESO and Danish observing time, and financially by the Danish Natural Science Research Council through the Danish Board for Astronomical Research.

References

All Tables

Table 2

Double-lined spectroscopic binary systems SB2 with evolved component.

Table 3

Evolved stars with no CORAVEL dip.

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