[en] Results from the first large-scale survey in the CO(J = 1 → 0) line of the Vela-Carina-Centaurus region of the Southern Milky Way are reported. The observations, were spaced every beamwidth (0.125⁰) in the range 270⁰ ≤ I ≤ 300⁰ and -1⁰ ≤ b ≤ 1⁰, with latitude extensions to cover all Carina arm (I > 280⁰) emission beyond the absolute value of b = 1⁰. In a concurrent survey every half-degree in latitude and longitude was sampled in the range 270⁰ ≤ I ≤ 300⁰ and -5⁰ ≤ b ≤ 5⁰ at a spatial resolution of 0.5⁰. Both surveys had a spectral coverage of 330 km s^-1 with a resolution of 1.3 km s^-1. The Carina arm dominates the data. Its abrupt tangent at I ≅ 280⁰ and characteristic loop in the I,v diagram are unmistakable evidence for CO spiral structure. When the emission is integrated over velocity and latitude, the height of the setup seen in the tangent direction suggests that the arm-interarm contrast is at least 13 to 1. Spatial maps of the arm exhibit a projected narrowing in latitude of the CO layer with increasing kinematic distance. Comparison of the CO and HI data shows close agreement between these two species in a segment of the arm lying outside the solar circle (R₀ = 10 kpc); within R₀ the arm is more difficult to trace in HI than in CO