Volume 570, October 2014
|Number of page(s)||13|
|Section||Catalogs and data|
|Published online||31 October 2014|
White dwarf-main sequence binaries from LAMOST: the DR1 catalogue⋆
Key Laboratory of Optical Astronomy, National Astronomical Observatories,
Chinese Academy of Sciences,
e-mail: firstname.lastname@example.org; email@example.com
2 University of Chinese Academy of Sciences, 100049 Beijing, PR China
3 Kavli Institute for Astronomy and Astrophysics, Peking University, 100871 Beijing, PR China
4 Peking University, 100871 Beijing, PR China
5 University of Science and Technology of China, 230026 Hefei, PR China
6 Nanjing Institute of Astronomical Optics & Technology, National Astronomical Observatories, Chinese Academy of Sciences, 210042 Nanjing, PR China
Accepted: 31 July 2014
Context. White dwarf-main sequence (WDMS) binaries are used to study several different important open problems in modern astrophysics.
Aims. The Sloan Digital Sky Survey (SDSS) identified the largest catalogue of WDMS binaries currently known. However, this sample is seriously affected by selection effects and the population of systems containing cool white dwarfs and early-type companions is under-represented. Here we search for WDMS binaries within the spectroscopic data release 1 of the Large sky Area Multi-Object fiber Spectroscopic Telescope (LAMOST) survey. LAMOST and SDSS follow different target selection algorithms. Hence, LAMOST WDMS binaries may be drawn from a different parent population and thus help in overcoming the selection effects incorporated by SDSS on the current observed population.
Methods. We develop a fast and efficient routine based on the wavelet transform to identify LAMOST WDMS binaries containing a DA white dwarf and a M dwarf companion, and apply a decomposition/fitting routine to their LAMOST spectra to estimate their distances and measure their stellar parameters, namely the white dwarf effective temperatures, surface gravities and masses, and the secondary star spectral types.
Results. We identify 121 LAMOST WDMS binaries, 80 of which are new discoveries, and estimate the sample to be ~90 per cent complete. The LAMOST and SDSS WDMS binaries are found to be statistically different. However, this result is not due to the different target selection criteria of both surveys, but likely a simple consequence of the different observing conditions. Thus, the LAMOST population is found at considerably shorter distances (~50–450 pc) and is dominated by systems containing early-type companions and hot white dwarfs.
Conclusions. Even though WDMS binaries containing cool white dwarfs are also missed by the LAMOST survey, the LAMOST WDMS binary sample dominated by systems containing early-type companions is an important addition to the current known spectroscopic catalogue. Future LAMOST observations however are required to increase the small number of LAMOST WDMS binaries.
Key words: binaries: spectroscopic / stars: low-mass / white dwarfs / methods: data analysis
Full Tables 1–3 and the spectra are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/570/A107
© ESO, 2014
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