References - TC43IV
The first heavy-metal hot subdwarf composite binary SB 744
By: Peter Nemeth, Joris Vos, Francisco Molina and Alexander Bastian
In: Astronomy & Astrophysics - 2021 - Accepted - arXiv:2107.03270
(Astroserver project reference: TC43IV)
poster The spectral energy distribution of SB 744 together with the best-fit model. The observed fluxes are shown as open circles while the calculated fluxes are shown as crosses. The best fit binary model (black) is shown along with the cool (green) and hot (blue) component.

A radial velocity follow-up of the long-period sdOB+G1V type spectroscopic binary SB 744 revealed strong lines of fluorine and lead in the optical spectrum of the sdOB star and subsolar metallicity in the G1V companion. With high-quality observations and Gaia astrometric data, we aim at measuring the chemical composition and Galactic kinematics of the system to put it in context with known populations of hot subdwarfs. Such binary systems have high potential, as they give insights into the late stages of binary evolution as well as into the mysterious formation of stripped core helium-burning stars.

We have analyzed the optical spectra with homogeneous atmospheric models to derive surface parameters of the binary members from a direct wavelength space decomposition and independently measured the atmospheric properties of the cool companion. The two independent methods reached consistent results, which, amended with constraints from spectral energy distributions provided a subdwarf mass. The Gaia astrometry allowed us to derive the Galactic kinematics of the system.

SB 744 turned out to be an old, Population II system, that has gone through dramatic events. The hot subdwarf star belongs to the heavy-metal subclass of sdOB stars and we report super-solar abundances of lead, based on Pb III/IV lines. The He abundance of the hot subdwarf is the lowest among the known heavy-metal sdOB stars. The presence of fluorine implies that SB 744 was once a hierarchical triple system and the inner binary has merged in the near past. As an alternative scenario, single-star evolution through late core helium flash and atmospheric mixing can also produce the observed fluorine abundances. The atmospheric metal over-abundances currently observed are perhaps the results of a combination of mixing processes during formation and radiative support.

Selected region of the best-fit Tlusty/XTgrid model of SB 744. Strong lines of F and Pb are marked and labelled in the figure. The decomposition over the entire VLT/UVES spectral range is also available.

Science contact

  • Dr Peter Nemeth
  • Astronomical Institute of the Czech Academy of Sciences
  • Fričova 298, CZ-25165, Ondřejov, Czech Republic
  • Phone:
  • Email: peter.nemethno

Related links

Partner institutes