@article{oai:ir.kagoshima-u.ac.jp:00006098, author = {Asaki, Yoshiharu and 朝木, 義晴 and Deguchi, Shuji and 出口, 修至 and Imai, Hiroshi and 今井, 裕 and Hachisuka, Kazuya and 蜂須賀, 一也 and Miyoshi, Makoto and 三好, 真 and Honma, Mareki and 本間, 希樹}, issue = {1}, journal = {The Astronomical Journal}, month = {}, note = {We have conducted Very Long Baseline Array phase-referencing monitoring of H2O masers around the red supergiant, S Persei, for six years.We have fitted maser motions to a simple expanding-shell model with a common annual parallax and stellar proper motion, and obtained the annual parallax as 0.413 ± 0.017 mas and the stellar proper motion as (-0.49 ± 0.23 mas yr^-1, -1.19 ± 0.20 mas yr^-1) in right ascension and declination, respectively. The obtained annual parallax corresponds to the trigonometric distance of 2.42[+0.11 -0.09] kpc. Assuming a Galactocentric distance of the Sun of 8.5 kpc, the circular rotational velocity of the local standard of rest at a distance of the Sun of 220 km s^-1, and a flat Galactic rotation curve, S Persei is suggested to have a non-circular motion deviating from the Galactic circular rotation for 15 km s^-1, which is mainly dominated by the anti-rotation direction component of 12.9 ± 2.9 km s^-1. This red supergiant is thought to belong to the OB association, Per OB1, so that this non-circular motion is representative of a motion of the OB association in the MilkyWay. This non-circular motion is somewhat larger than that explained by the standard density-wave theory for a spiral galaxy and is attributed to either a cluster shuffling of the OB association, or to non-linear interactions between non-stationary spiral arms and multi-phase interstellar media. The latter comes from a new view of a spiral arm formation in the Milky Way suggested by recent large N-body/smoothed particle hydrodynamics numerical simulations.}, pages = {267--277}, title = {DISTANCE AND PROPER MOTION MEASUREMENT OF THE RED SUPERGIANT, S PERSEI, WITH VLBI H2O MASER ASTROMETRY}, volume = {721}, year = {2010} }