Methanol Maser Parallaxes and Proper Motions

Xu, Ye; Reid, M. J.; Moscadelli, L.; Menten, K. M.; Zheng, Xingwu; Brunthaler, A.; Zhang, B.; Rygl, K. L. J.; Li, J. J.; Sanna, A.

doi:10.1017/s1743921312007326

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(1 citation statement)

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“…The precision of our distance determination to this eclipsing binary (total error of ∼ 4%) rivals those obtained from interferometric parallaxes of Galactic masers (e.g. Xu et al 2012, their Table 1) at comparable distances. In this paper we focus on a precise determination of physical parameters of the system, its distance and space kinematic properties and a discussion of evolutionary status.…”

Section: Introductionsupporting

confidence: 54%

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

Suchomska

Graczyk

Smolec

et al. 2015

Monthly Notices of the Royal Astronomical Society

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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 ± 1.38 and R 2 = 67.63 ± 1.40 R ⊙ and their masses are M 1 = 4.914 ± 0.021 and M 2 = 4.875± 0.021 M ⊙ . 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 ± 0.06 kpc (stat.) ± 0.05 (syst.) which places the star in the Sagittarius-Carina arm. The Galactic rotational velocity of the star is Θ s = 258 ± 26 km s −1 assuming Θ 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.

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Section: Introductionsupporting

confidence: 54%