Distance to G14.33-0.64 in the Sagittarius Spiral Arm: H2O Maser Trigonometric Parallax with VERA
Mayumi Sato, Tomoya Hirota, Mark J. Reid, Mareki Honma, Hideyuki, Kobayashi, Kenzaburo Iwadate, Takeshi Miyaji, Katsunori M. Shibata

TL;DR
This study precisely measures the distance to the star-forming region G14.33-0.64 using VLBI parallax, revealing the Sagittarius arm is closer than previously thought and refining our understanding of Galactic structure.
Contribution
First direct parallax measurement of G14.33-0.64, clarifying its position in the Sagittarius arm and improving Galactic spiral arm models.
Findings
Distance to G14.33-0.64 is 1.12 kpc, less than half the kinematic estimate.
Sagittarius arm is closer (~1 kpc) than previously assumed (~2-3 kpc).
G14.33-0.64 shows no significant peculiar motion, aligning with Galactic rotation.
Abstract
We report on trigonometric parallax measurements for the Galactic star forming region G14.33-0.64 toward the Sagittarius spiral arm. We conducted multi-epoch phase-referencing observations of an H2O maser source in G14.33-0.64 with the Japanese VLBI array VERA. We successfully detected a parallax of 0.893+/-0.101 mas, corresponding to a source distance of 1.12+/-0.13 kpc, which is less than half of the kinematic distance for G14.33-0.64. Our new distance measurement demonstrates that the Sagittarius arm lies at a closer distance of ~1 kpc, instead of previously assumed ~2-3 kpc from kinematic distances. The previously suggested deviation of the Sagittarius arm toward the Galactic center from the symmetrically fitted model (Taylor & Cordes 1993) is likely due to large errors of kinematic distances at low galactic longitudes. G14.33-0.64 most likely traces the near side of the Sagittarius…
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