  Solar oxygen abundance measurements based on the O I near-infrared triplet
have been a much-debated subject for several decades since non-local
thermodynamic equilibrium (NLTE) calculations with 3D radiation-hydrodynamics
model atmospheres introduced a large change to the 1D LTE modelling. In this
work, we aim to test solar line formation across the solar disk using new
observations obtained with the SST/CRISP instrument. The observed dataset is
based on a spectroscopic mosaic stretching from disk center to the solar limb.
By comparing the state-of-the-art 3D NLTE models with the data, we find that
the 3D NLTE models provide an excellent description of line formation across
the disk. We obtain an abundance value of $A(\mathrm{O}) = (8.73 \pm 0.03)$
dex, with a very small angular dispersion across the disk. We conclude that
spectroscopic mosaics are excellent probes for geometric and physical
properties of hydrodynamics models and non-LTE line formation.
