Access to Astronomical Catalogues

← Click to display the menu
J/A+A/608/A100       CMD and mass distribution of Ba stars      (Escorza+, 2017)

Hertzsprung-Russell diagram and mass distribution of barium stars. Escorza A., Boffin H.M.J., Jorissen A., Van Eck S., Siess L., Van Winckel H., Karinkuzhi D., Shetye S., Pourbaix D. <Astron. Astrophys. 608, A100 (2017)> =2017A&A...608A.100E (SIMBAD/NED BibCode)
ADC_Keywords: Stars, barium; Stars, giant; HR diagrams; Stars, masses Keywords: Binaries: general - stars: late-type - stars: chemically peculiar Abstract: With the availability of parallaxes provided by the Tycho-Gaia Astrometric Solution, it is possible to construct the Hertzsprung-Russell diagram (HRD) of barium and related stars with unprecedented accuracy. A direct result from the derived HRD is that subgiant CH stars occupy the same region as barium dwarfs, contrary to what their designations imply. By comparing the position of barium stars in the HRD with STAREVOL evolutionary tracks, it is possible to evaluate their masses, provided the metallicity is known. We used an average metallicity [Fe/H]=-0.25 and derived the mass distribution of barium giants. The distribution peaks around 2.5M, with a tail at higher masses up to 4.5M. This peak is seen as well in the mass distribution of a sample of normal K and M giants used for comparison and is associated with stars located in the red clump. When we compare these mass distributions, we see a deficit of low-mass (1-2M) barium giants. This is probably because low-mass stars reach large radii at the tip of the red giant branch, which may have resulted in an early binary interaction. Among barium giants, the high-mass tail is however dominated by stars with a barium index (based on a visual inspection of the barium spectral line) less than unity, i.e., with a very moderate barium line strength. We believe that these stars are not genuine barium giants, but rather bright giants (or supergiants) where the barium lines are strengthened because of a positive luminosity effect. Moreover, contrary to previous claims, we do not see differences between the mass distributions of mild and strong barium giants. Description: This catalogue contains the effective temperatures and luminosities obtained for a sample of barium and related stars by an SED fitting method and using MARCS models with three different metallicities. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 262 437 Effective temperatures and luminosities obtained for a sample of barium and related stars
See also: I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) I/337 : Gaia DR1 (Gaia Collaboration, 2016) J/A+A/326/722 : HIPPARCOS Ba stars (Mennessier+ 1997) J/A+A/372/245 : Infrared properties of barium stars (Chen+, 2001) J/A+A/454/895 : Abundances of 26 barium stars. I. (Allen+, 2006) J/A+A/454/917 : Abundances of 26 barium stars. II. (Allen+, 2006) J/A+A/525/A63 : Abundances in Ba stars (Allen+, 2011) J/AZh/79/909 : Chemical abundances in barium stars (Boyarchuk+, 2002) J/AZh/80/704 : Studies of classical barium stars (Antipova+, 2003) J/MNRAS/459/4299 : Barium stars abundances and kinematics (de Castro+, 2016) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 14 A14 --- Name Name of the star 16- 27 F12.8 deg RAdeg Right ascension (J2000) 29- 40 F12.8 deg DEdeg Declination (J2000) 42- 46 A5 --- Type Star type 48- 55 F8.2 d Per ? Orbital period (1) 57- 61 F5.3 --- e ? Orbital eccentricity (1) 63- 67 F5.2 [Sun] [Fe/H] ? Metallicity with respect to solar 69- 90 A22 --- r_[Fe/H] Reference for [Fe/H] (2) 92- 96 F5.1 mas plx Parallax 98-100 F3.1 mas e_plx Error on the parallax 102-130 A29 --- r_plx Reference for the parallax (3) 132-135 I4 K b_T(0.0) Lower limit of Teff for grid with [Fe/H]=0.0 137-140 I4 K T(0.0) Effective temperature for grid with [Fe/H]=0.0 142-145 I4 K B_T(0.0) Upper limit of Teff for grid with [Fe/H]=0.0 147-154 F8.3 Lsun b_L(0.0) Lower limit of luminosity for grid with [Fe/H]=0.0 156-164 F9.3 Lsun L(0.0) Luminosity for grid with [Fe/H]=0.0 166-174 F9.3 Lsun B_L(0.0) Upper limit of luminosity for grid with [Fe/H]=0.0 176-179 I4 K b_T(-0.25) Lower limit of Teff for grid with [Fe/H]=-0.25 181-184 I4 K T(-0.25) Effective temperature for grid with [Fe/H]=-0.25 186-189 I4 K B_T(-0.25) Upper limit of Teff for grid with [Fe/H]=-0.25 191-198 F8.3 Lsun b_L(-0.25) Lower limit of luminosity for grid with [Fe/H]=-0.25 200-208 F9.3 Lsun L(-0.25) Luminosity for grid with [Fe/H]=-0.25 210-218 F9.3 Lsun B_L(-0.25) Upper limit of luminosity for grid with [Fe/H]=-0.25 220-223 I4 K b_T(-0.5) Lower limit of Teff for grid with [Fe/H]=-0.5 225-228 I4 K T(-0.5) Effective temperature for grid with [Fe/H]=-0.5 230-233 I4 K B_T(-0.5) Upper limit of Teff for grid with [Fe/H]=-0.5 235-242 F8.3 Lsun b_L(-0.5) Lower limit of luminosity for grid with [Fe/H]=-0.5 244-252 F9.3 Lsun L(-0.5) Luminosity for grid with [Fe/H]=-0.5 254-262 F9.3 Lsun B_L(-0.5) Upper limit of luminosity for grid with [Fe/H]=-0.5
Note (1): Orbital periods and eccentricities are determined by Jorissen et al. (1998A&A...332..877J) and Jorissen et al. (2017, in preparation) for the giants and by Escorza et al. (2017, in preparation) for the main sequence and subgiant stars. Note (2): Karinkuzhi for Karinkuzhi et al. (2017, in prep). Note (3): References as follows: Hipparcos (ESA, 1997) = HIP, 1997HIP...C......0E, Cat. I/239 Pourbaix & Jorissen (2000) = Pourbaix & Jorissen, 2000A&AS..145..161P TGAS (Lindegren et al., 2016) = TGAS, 2016A&A...595A...1G, Cat. I/337
Acknowledgements: Ana Escorza, ana.escorza(at)kuleuven.be
(End) Ana Escorza [KU Leuven], Patricia Vannier [CDS] 04-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact