We report results of the measurement of the trigonometric parallax of an H2O maser source in IRAS 22555+6213 with the VLBI Exploration of Radio Astrometry (VERA). The annual parallax was determined to be 0.2780.019 mas, corresponding to a distance of 3.66+0:30 -0:26 kpc. Our results conrm that IRAS 22555+6213 is located in the Perseus arm. We computed the peculiar motion of IRAS 22555+6213 to be (Usrc; Vsrc;Wsrc) = (0 ± 1,-32 ± 1, 9 ± 1) km s􀀀1, where Usrc, Vsrc, and Wsrc are directed toward the Galactic center, in the direction of Galactic rotation and toward the Galactic north pole, respectively. IRAS 22555+6213, NGC7538 and Cepheus A lie along the same line of sight, and are within 2 on the sky. Their parallax distances, with which we derived their absolute position in the Milky Way, show that IRAS 22555+6213 and NGC7538 are associated with the Perseus arm, while Cepheus A is located in the Local arm. We compared the kinematic distances of IRAS 22555+6213 derived with at and non- at rota- tion curve with its parallax distance and found the kinematic distance derived from the non- at rotation assumption (—32 km s-1 lag) to be consistent with the parallax distance.

ABSTRACT
1. INTRODUCTION
2. OBSERVATIONS
3. RESULTS & DISCUSSIONS
REFERENCES

• James O. Chibueze(East Asian ALMA Regional Center, National Astronomical Observatory of Japan/Department of Physics and Astronomy, Faculty of Physical Sciences, University of Nigeria, Carver Building)
• Hirofumi Sakanoue(Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University)
• Toshihiro Omodaka(Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University)
• Toshihiro Handa(Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University)
• Takumi Nagayama(Mizusawa VLBI Observatory, National Astronomical Observatory of Japan)
• Tatsuya Kamezaki(Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University)
• Ross Burns(Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University)