We present Submillimeter Array (SMA) observations in the CO J = 3–2, SiO J = 5–4 and 8–7, and SO 98–87 lines, as well as Atacama Pathfinder EXperiment observations in the CO J = 6–5 line, of an extremely high-velocity and jet-like outflow in high-mass star-forming region HH 80–81. The outflow is known to contain two prominent molecular bullets, namely B1 and B2, discovered from our previous SMA CO J = 2–1 observations. While B1 is detected in all the CO, SiO, and SO lines, B2 is only detected in CO lines. The CO 3–2/2–1 line ratio in B1 is clearly greater than that in B2. We perform a large velocity gradient analysis of the CO lines and derive a temperature of 70–210 K for B1 and 20–50 K for B2. Taking into account the differences in the velocity, distance from the central source, excitation conditions, and chemistry between the two bullets, we suggest that the bullets are better explained by direct ejections from the innermost vicinity of the central high-mass protostar, and that we are more likely observing the molecular component of a primary wind rather than entrained or swept-up material from the ambient cloud. These findings further support our previous suggestions that the molecular bullets indicate an episodic, disk-mediated accretion in the high-mass star formation process.
