  An extremely high-resolution (> 10^5) high-S/N (> 10^3) solar spectrum has
been used to measure 15 very weak first overtone (Delta v = 2) infrared OH
lines, resulting in a low solar abundance of A(O) ~ 8.6 when MARCS, 3D, and
spatially and temporally averaged 3D model atmospheres are used. A higher
abundance is obtained with Kurucz (A(O) ~ 8.7) and Holweger & Muller (A(O) ~
8.8) model atmospheres. The low solar oxygen abundance obtained in this work is
in good agreement with a recent 3D analysis of [OI], OI, OH fundamental (Delta
v = 1) vibration-rotation and OH pure rotation lines (Asplund et al. 2004). The
present result brings further support for a low solar metallicity, and although
using a low solar abundance with OPAL opacities ruins the agreement between the
calculated and the helioseismic measurement of the depth of the solar
convection zone, recent results from the OP project show that the opacities
near the base of the solar convection zone are larger than previously thought,
bringing further confidence for a low solar oxygen abundance.
