• DOI:10.1093/mnras/stv951
• Corpus ID: 59397309

The Araucaria Project: accurate stellar parameters and distance to evolved eclipsing binary ASAS J180057-2333.8 in Sagittarius Arm

@article{Suchomska2015TheAP,
  title={The Araucaria Project: accurate stellar parameters and distance to evolved eclipsing binary ASAS J180057-2333.8 in Sagittarius Arm},
  author={Ksenia Suchomska and Dariusz Graczyk and Radosław Smolec and Grzegorz Pietrzy'nski and Wolfgang Gieren and K. Stcepie'n and Piotr Konorski and Bogumił Pilecki and Sandro Villanova and Ian B. Thompson and Marek G'orski and Paulina Karczmarek and Piotr Wielg'orski and Richard I. Anderson},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2015},
  volume={451},
  pages={651-659}
}

• K. Suchomska, D. Graczyk, +11 authors R. I. Anderson
• Published 4 May 2015
• Physics
• Monthly Notices of the Royal Astronomical Society

We have analyzed the double-lined eclipsing binary system ASAS J180057-2333.8 from the All Sky Automated Survey (ASAS) catalogue . We measure absolute physical and orbital parameters for this system based on archival $V$-band and $I$-band ASAS photometry, as well as on high-resolution spectroscopic data obtained with ESO 3.6m/HARPS and CORALIE spectrographs. The physical and orbital parameters of the system were derived with an accuracy of about 0.5 - 3%. The system is a very rare configuration of two bright well-detached giants of spectral types K1 and K4 and luminosity class II. The radii of the stars are $R_1$ = 52.12 $\pm$ 1.38 and $R_2$ = 67.63 $\pm$ 1.40 R$_\odot$ and their masses are $M_1$ = 4.914 $\pm$ 0.021 and $M_2$ = 4.875$\pm$ 0.021 M$_\odot$ . The exquisite accuracy of 0.5% obtained for the masses of the components is one of the best mass determinations for giants. We derived a precise distance to the system of 2.14 $\pm$ 0.06 kpc (stat.) $\pm$ 0.05 (syst.) which places the star in the Sagittarius-Carina arm. The Galactic rotational velocity of the star is $\Theta_s=258 \pm 26$ km s$^{-1}$ assuming $\Theta_0=238$ km s$^{-1}$. A comparison with PARSEC isochrones places the system at the early phase of core helium burning with an age of slightly larger than 100 million years. The effect of overshooting on stellar evolutionary tracks was explored using the MESA star code.