A White Dwarf–Main-sequence Binary Unveiled by Time-domain Observations from LAMOST and TESS
Ling-Lin Zheng, Wei‐Min Gu, Mouyuan Sun, Zhi-Xiang Zhang, Tuan Yi, Jianfeng Wu, Junfeng Wang, Jin-Bo Fu, Senyu Qi, Fan Yang, Song Wang, Liang Wang, Zhongrui Bai, Haotong Zhang, Chunqian Li, Jianrong Shi, Weikai Zong, Yu Bai, Jifeng Liu
Abstract
Abstract We report a single-lined white dwarf–main-sequence binary system, LAMOST J172900.17+652952.8, which is discovered by the Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST)’s medium-resolution time-domain surveys. The radial-velocity semi-amplitude and orbital period of the optical visible star are measured by using follow-up observations with the Palomar 200 inch telescope and light curves from the Transiting Exoplanet Survey Satellite (TESS). Thus the mass function of the invisible candidate white dwarf is derived, f ( M 2 ) = 0.120 ± 0.003 M ⊙ . The mass of the visible star is measured based on a spectral energy distribution fitting, M 1 = <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>0.81</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.06</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.07</mml:mn> </mml:mrow> </mml:msubsup> <mml:mspace width="0.25em"/> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> </mml:math> . Hence, the mass of its invisible companion is M 2 ≳ 0.63 M ⊙ . The companion ought to be a compact object rather than a main-sequence star owing to the mass ratio q = M 2 / M 1 ≳ 0.78 and the single-lined spectra. The compact object is likely to be a white dwarf if the inclination angle is not small, i ≳ 40°. By using the Galaxy Evolution Explorer (GALEX) near-UV flux, the effective temperature of the white dwarf candidate is constrained as <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mi>T</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>eff</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>WD</mml:mi> </mml:mrow> </mml:msubsup> </mml:math> ≲ 12,000–13,500 K. It is difficult to detect white dwarfs which are outshone by their bright companions via single-epoch optical spectroscopic surveys. Therefore, optical time-domain surveys can play an important role in unveiling invisible white dwarfs and other compact objects in binaries.