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Context: Recent works with improved model atmospheres, line formation, atomicand molecular data, and detailed treatment of blends, have resulted in asignificant downward revision of the solar oxygen abundance.  Aims: Considering the importance of the Sun as an astrophysical standard andthe current conflict of standard solar models using the new solar abundanceswith helioseismological observations we have performed a new study of the solaroxygen abundance based on the forbidden [OI] line at 5577.34 A, not previouslyconsidered.  Methods: High-resolution (R > 500 000), high signal-to-noise (S/N > 1000)solar spectra of the [O I] 5577.34 A line have been analyzed employing boththree-dimensional (3D) and a variety of 1D (spatially and temporally averaged3D, Holweger & Muller, MARCS and Kurucz models with and without convectiveovershooting) model atmospheres.  Results: The oxygen abundance obtained from the [OI] 5577.3 A forbidden lineis almost insensitive to the input model atmosphere and has a mean value ofA(O) = 8.71 +/- 0.02 (\sigma from using the different model atmospheres). Thetotal error (0.07 dex) is dominated by uncertainties in the log gf value (0.03dex), apparent line variation (0.04 dex) and uncertainties in the continuum andline positions (0.05 dex).  Conclusions: The here derived oxygen abundance is close to the 3D-basedestimates from the two other [OI] lines at 6300 and 6363 A, the permitted OIlines and vibrational and rotational OH transitions in the infrared. Our studythus supports a low solar oxygen abundance (A(O) ~ 8.7), independent of theadopted model atmosphere.

Another forbidden solar oxygen abundance: the [O I] 5577 A line