Pinpointing the position of the post-asymptotic giant branch star at the core of RAFGL 2688 using polarimetric imaging with NICMOS

We have used infrared polarimetric imaging with NICMOS to determine precise ly the position of the star that illuminates (and presumably generated) the bipolar, preplanetary reflection nebula RAFGL 2688 (the Egg Nebula). The p olarimetric data pinpoint the illuminating star, which is not detected dire ctly at wavelengths less than or equal to 2 mu m, at a position well within the dark lane that bisects the nebula, 0." 55 (similar to 550 AU) southwes t of the infrared peak that was previously detected at the southern tip of the northern polar lobe. The inferred position of the central star correspo nds to the geometric center of the tips of the four principle lobes of near -infrared H-2 emission; identifying the central star at this position also reveals the strong point symmetric structure of the nebula, as seen both in the intensity and polarization structure of the polar lobes. The polarimet ric and imaging data indicate that the infrared peak directly detected in t he NICMOS images is a self-luminous source and, therefore, is most likely a distant binary companion to the illuminating star. Although present theory predicts that bipolar structure in preplanetary and planetary nebulae is a consequence of binary star evolution, the separation between the component s of the RAFGL 2688 binary system, as deduced from these observations, is m uch too large for the presence of the infrared companion to have influenced the structure of the RAFGL 2688 nebula.