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As part our investigation into the Galactic rotation curve, we carried outVery Long Baseline Interferometry (VLBI) observations towards the star-formingregion IRAS 01123+6430 using VLBI Exploration of Radio Astrometry (VERA) tomeasure its annual parallax and proper motion. The annual parallax was measuredto be 0.151+/-0.042 mas, which corresponds to a distance ofD=6.61^{+2.55}_{-1.44} kpc, and the obtained proper motion components were({\mu}_{\alpha}cos{\delta}, {\mu}_{\delta})=(-1.44+/-0.15, -0.27+/-0.16) masyr^{-1} in equatorial coordinates. Assuming Galactic constants of (R_0,{\Theta}_0)=(8.05+/-0.45 kpc, 238+/-14 km s^{-1}), the Galactocentric distanceand rotation velocity were measured to be (R, {\Theta})=(13.04+/-2.24 kpc,239+/-22 km s^{-1}), which are consistent with a flat Galactic rotation curve.The newly estimated distance provides a more accurate bolometric luminosity ofthe central young stellar object, L_Bol=(3.11+/-2.86)\times 10^3 L_solar, whichcorresponds to a spectral type of B1-B2. The analysis of 12CO(J=1-0) surveydata obtained with the Five College Radio Astronomical Observatory (FCRAO) 14 mtelescope shows that the molecular cloud associated with IRAS 01123+6430consists of arc-like and linear components, which well matches a structurepredicted by numerical simulation of the cloud-cloud collision (CCC)phenomenon. The coexistence of arc-like and linear components implies that therelative velocity of initial two clouds was as slow as 3-5 km s^{-1}, whichmeets the expected criteria of massive star formation where the core mass iseffectively increased in the presence of low relative velocity (~3-5 kms^{-1}), as suggested by Takahira et al.(2014).

Outer rotation curve of the Galaxy with VERA IV: Astrometry of IRAS 01123+6430 and the possibility of cloud-cloud collision