We report measurements of parallaxes and proper motions of ten high-mass star-forming regions in the Sagittarius spiral arm of the Milky Way as part of the BeSSeL Survey with the VLBA. Combining these results with eight others from the literature, we investigated the structure and kinematics of the arm between Galactocentric azimuths ß ˜ -2° and 65°. We found that the spiral pitch angle is 7°.3 ± 1°.5; the arm's half-width, defined as the rms deviation from the fitted spiral, is ˜0.2 kpc; and the nearest portion of the Sagittarius arm is 1.4 ± 0.2 kpc from the Sun. Unlike for adjacent spiral arms, we found no evidence for significant peculiar motions of sources in the Sagittarius arm opposite to Galactic rotation. Tables 1 and 2 and Appendix A are available in electronic form at http://www.aanda.org
