Detecting faint secondaries of spectroscopic binaries: HD 101177B and 149414A

Details Detecting faint secondaries of spectroscopic binaries: HD 101177B and 149414A Detecting faint secondaries of spectroscopic binaries: HD 101177B and 149414A

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.284..341m&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 284, Issue 2, pp. 341-347.

Astronomy and Astrophysics

Astronomy

13

Binaries: Spectroscopic - Stars: Individual: Hd 101177B - Stars: Individual: Hd 149414A

Scientific paper

We have observed HD 101177B and 149414A, two known single-lined binaries, and directly measured the radial velocities of their secondaries, enabling us to derive the mass ratios of the two systems. Using high signal-to-noise ratio spectra obtained mostly with the William Herschel Telescope, and a new algorithm to analyse composite spectra, TODCOR, we show that the mass ratios of HD 101177B and 149414A are 0.48+/-0.03 and 0.57+/-0.02, respectively. These are two of the lowest mass ratios ever measured around normal G or K dwarf stars. These two systems demonstrate the potential of the present approach, which can turn many of the known single-lined binaries into double-lined systems. Such work has important implications for the study of the mass-ratio distribution of many samples of binaries.

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