2011AJ....141...60M

We report H I 21 cm line observations of the asymptotic giant branch (AGB) star X Her obtained with the Robert C. Byrd Green Bank Telescope (GBT) and the Very Large Array. We have unambiguously detected H I emission associated with the circumstellar envelope of the star, with a mass totaling M_ H I _~ 2.1x10^–3 M_☉. The H I distribution exhibits a head-tail morphology, similar to those previously observed around the AGB stars Mira and RS Cnc. The tail is elongated along the direction of the star's space motion, with a total extent of ≳ 6'.0 (0.24 pc) in the plane of the sky. We also detect a systematic radial velocity gradient of ∼6.5 km/s across the H I envelope. These results are consistent with the H I emission tracing a turbulent wake that arises from the motion of a mass-losing star through the interstellar medium (ISM). GBT mapping of a 2°x2° region around X Her reveals that the star lies (in projection) near the periphery of a much larger H I cloud that also exhibits signatures of interaction with the ISM. The properties of the cloud are consistent with those of compact high-velocity clouds. Using ¹²CO J = 1-0 observations, we have placed an upper limit on its molecular gas content of N_H2< 1.3x10²⁰/cm2. Although the distance to the cloud is poorly constrained, the probability of a chance coincidence in position, velocity, and apparent position angle of space motion between X Her and the cloud is extremely small, suggesting a possible physical association. However, the large H I mass of the cloud ( ≳ 2.4 M_☉) and the blueshift of its mean velocity relative to X Her are inconsistent with an origin tied directly to ejection from the star.