White dwarf-main sequence binaries from LAMOST: the DR1 catalogue

TL;DR

This paper presents a new catalogue of 121 white dwarf-main sequence binaries from LAMOST, including 80 new discoveries, and analyzes their properties to address selection biases in previous surveys.

Contribution

The study introduces an efficient wavelet-based method to identify WDMS binaries in LAMOST data and provides a comparative analysis with SDSS samples.

Findings

LAMOST WDMS binaries are statistically different from SDSS ones.

The LAMOST sample is closer, at 50-450 pc, and contains more systems with early-type companions and hot white dwarfs.

Approximately 90% of the LAMOST WDMS binary population has been identified.

Abstract

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 LAMOST (Large sky Area Multi-Object fiber Spectroscopic Telescope) 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 \sim90 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 (\sim50-450 pc) and is dominated by systems containing early-type companions and hot white dwarfs. (abridged)