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PG 2131+066 is a composite-spectrum binary with a hot pulsating PG 1159-typepre-white dwarf and an early M-type main sequence star. Analysis of Whole EarthTelescope observations of the pulsating pre-white dwarf component provided anasteroseismological determination of its mass, luminosity, and effectivetemperature. These determinations allowed Kawaler et al. (1995) to determinethe distance to this star. In this paper, we refine the asteroseismologicaldistance determination, and confirm the distance by an independent measurementto the system via the spectroscopic parallax of the M star. PG 2131+066 wasobserved by the HST using the original PC in September 1993. Exposures withfilters F785LP and F555W both showed the companion at a distance of 0.3 arcseconds. Photometry of the images provides an apparent magnitude for the mainsequence companion of v=18.97+/-0.15, from which we find a distance of 560(+200 -134) pc. We also recalculated the asteroseismological distance to thepre-white dwarf using updated models and new spectroscopic constraints from UVspectra. The new seismological distance is 668 (+78 -83) pc, in satisfactoryagreement with the distance of the secondary star. These results suggest thatthis is indeed a physical binary, and that seismological distance determinationmay be the best way to determine the distance to the pulsating hot pre-whitedwarf stars.Comment: 13 pages, 4 figures, to appear in The Astrophysical Journal, Dec.10,  200

PG 2131+066: A Test of Pre–White Dwarf Asteroseismology