http://arxiv.org/abs/2011.13330
We present our final orbit for the late-type spectroscopic binary HD 1. Employed are 553 spectra from 13 years of observations with our robotic STELLA facility and its high-resolution echelle spectrograph SES. Its long-term radial-velocity stability is $\approx$50m/s . A single radial velocity of HD 1 reached a rms residual of 63m/s, close to the expected precision. Spectral lines of HD 1 are rotationally broadened with $v\sin i$ of 9.1$\pm$0.1 km/s . The overall spectrum appears single-lined and yielded an orbit with an eccentricity of 0.5056$\pm$0.0005 and a semi-amplitude of 4.44km/s . We constrain and refine the orbital period based on the SES data alone to 2318.70$\pm$0.32d, compared to 2317.8$\pm$1.1d when including the older data set published by DAO and Cambridge/Coravel. Owing to the higher precision of the SES data, we base the orbit calculation only on the STELLA/SES velocities in order not to degrade its solution. We redetermine astrophysical parameters for HD 1 from spectrum synthesis and, together with the new {\it Gaia} DR-2 parallax, suggest a higher luminosity than published previously. We conclude that HD 1 is a slightly metal-deficient K0 III-II giant 217 times more luminous than the Sun. The secondary remains invisible at optical wavelengths. We present evidence for the existence of a third component.
K. Strassmeier and M. Weber
Mon, 30 Nov 20
52/117
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