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High-precision Orbital and Physical Parameters of Double-lined Spectroscopic Binary Stars—HD78418, HD123999, HD160922, HD200077, and HD210027

Konacki, Maciej and Muterspaugh, Matthew W. and Kulkarni, Shrinivas R. and Hełminiak, Krzysztof (2010) High-precision Orbital and Physical Parameters of Double-lined Spectroscopic Binary Stars—HD78418, HD123999, HD160922, HD200077, and HD210027. Astrophysical Journal, 719 (2). pp. 1293-1314. ISSN 0004-637X.

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We present high-precision radial velocities (RVs) of double-lined spectroscopic binary stars HD78418, HD123999, HD160922, HD200077, and HD210027. They were obtained based on the high-resolution echelle spectra collected with the Keck I/HIRES, Shane/CAT/Hamspec, and TNG/Sarge telescopes/spectrographs over the years 2003-2008 as part of the TATOOINE search for circumbinary planets. The RVs were computed using our novel iodine cell technique for double-line binary stars, which relies on tomographically disentangled spectra of the components of the binaries. The precision of the RVs is of the order of 1-10 m s^(–1), and to properly model such measurements one needs to account for the light-time effect within the binary's orbit, relativistic effects, and RV variations due to tidal distortions of the components of the binaries. With such proper modeling, our RVs combined with the archival visibility measurements from the Palomar Testbed Interferometer (PTI) allow us to derive very precise spectroscopic/astrometric orbital and physical parameters of the binaries. In particular, we derive the masses, the absolute K- and H-band magnitudes, and the parallaxes. The masses together with the absolute magnitudes in the K and H bands enable us to estimate the ages of the binaries. These RVs allow us to obtain some of the most accurate mass determinations of binary stars. The fractional accuracy in msin i only, and hence based on the RVs alone, ranges from 0.02% to 0.42%. When combined with the PTI astrometry, the fractional accuracy in the masses in the three best cases ranges from 0.06% to 0.5%. Among them, the masses of HD210027 components rival in precision the mass determination of the components of the relativistic double pulsar system PSR J0737 – 3039. In the near future, for double-lined eclipsing binary stars we expect to derive masses with a fractional accuracy of the order of up to ~0.001% with our technique. This level of precision is an order of magnitude higher than of the most accurate mass determination for a body outside the solar system—the double neutron star system PSR B1913+16.

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Kulkarni, Shrinivas R.0000-0001-5390-8563
Additional Information:© 2010 American Astronomical Society. Received 2009 October 23; accepted 2010 June 16; published 2010 July 28. We thank the California and Carnegie Exoplanet Search team, and Geoff Marcy in particular, for allowing us access to their precision velocimetry tools at Lick Observatory. This work benefits from the efforts of the PTI collaboration members who have each contributed to the development of an extremely reliable observational instrument. We thank PTI’s night assistant Kevin Rykoski for his efforts to maintain PTI in excellent condition and operating PTI. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. M.W.M. acknowledges support from the Townes Fellowship Program. M.K. is supported by the Foundation for Polish Science through a FOCUS grant and fellowship and by the Polish Ministry of Science and Higher Education through grant N203 005 32/ 0449. Part of the algorithms used in this analysis were developed during the SIM Double Blind Test, under JPL contract 1336910. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. The observations on the TNG/Sarge have been funded by the Optical Infrared Coordination network (OPTICON), a major international collaboration supported by the Research Infrastructures Programme of the European Commissions Sixth Framework Programme. This publication makes use of data products from the TwoMicronAll Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research was supported in part by the National Science Foundation under grant No. PHY05-51164. Facilities: Keck:I (HIRES), TNG (Sarg), Shane (Hamspec), PO:PTI
Funding AgencyGrant Number
UC Berkeley Space Sciences Laboratory Townes Postdoctoral FellowshipUNSPECIFIED
Foundation for Polish ScienceUNSPECIFIED
Ministry of Science and Higher Education (Poland)N203 005 32/0449
Subject Keywords:binaries: spectroscopic; stars: fundamental parameters; stars: individual (HD78418, HD123999, HD160922, HD200077, and HD210027); techniques: radial velocities
Issue or Number:2
Classification Code:PACS: 95.75.-z; 97.10.Wn; 95.30.Ky; 97.10.Vm; 97.80.Fk; 97.10.Nf
Record Number:CaltechAUTHORS:20100901-164355636
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Official Citation:Maciej Konacki et al 2010 ApJ 719 1293 doi: 10.1088/0004-637X/719/2/1293
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:19761
Deposited By: Jason Perez
Deposited On:03 Sep 2010 17:45
Last Modified:03 Oct 2019 02:01

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