Direct detections of white dwarfs in four WD+dM post-common envelope binaries within 20 pc

ABSTRACT Characterizing post-common envelope binaries (PCEBs) containing a white dwarf and a main-sequence companion is essential for improving theories of binary evolution. This paper presents the first direct spectroscopic confirmations of the white dwarf components in four PCEB systems within 20 pc of the Sun: G 203-47, GJ 207.1, LHS 1817, and Wolf 1130. To detect the white dwarfs we obtained near-UV spectroscopy from STIS on the Hubble Space Telescope, fitting with white dwarf models and M dwarf proxy spectra. We provide estimates of the white dwarf effective temperatures, which range from approximately 5300–6300 K. We compare these parameters to those determined from modelling with photometry alone, and find a 5–8 per cent discrepancy, due to emission features. Notably, 27 yr after its initial detection, we confirm the presence of a white dwarf in G 203-47, which is the ninth closest white dwarf to the Sun. Using Swift XRT data, we find that despite the 14.9-d orbital period of G 203-47, it is not tidally locked, possessing a rotation period likely exceeding 100 d, and making it a rare example of a long-period PCEB formed via a brief common envelope interaction. We update the local white dwarf space density to (5.2 $\pm \,$0.4) $\times$ 10$^{-3}$ pc$^{-3}$, and compare our results to models from the Binary Populations and Spectral Synthesis (bpass) framework, finding a good agreement with the predicted and observed numbers of PCEBs within 20 pc.