  We report results from 5-day VLBI observations of the well-known quasar 3C
279 at 1.3 mm (230 GHz) in 2011. The measured nonzero closure phases on
triangles including stations in Arizona, California and Hawaii indicate that
the source structure is spatially resolved. We find an unusual inner jet
direction at scales of $\sim$1 parsec extending along the northwest-southeast
direction (PA = $127^{\circ}\pm3^{\circ}$), as opposed to other (previously)
reported measurements on scales of a few parsecs showing inner jet direction
extending to the southwest. The 1.3 mm structure corresponds closely with that
observed in the central region of quasi-simultaneous super-resolution VLBA
images at 7 mm. The closure phase changed significantly on the last day when
compared with the rest of observations, indicating that the inner jet structure
may be variable on daily timescales. The observed new direction of the inner
jet shows inconsistency with the prediction of a class of jet precession
models. Our observations indicate a brightness temperature of $\sim
8\times10^{10}$ K in the 1.3 mm core, much lower than that at centimeter
wavelengths. Observations with better uv coverage and sensitivity in the coming
years will allow the discrimination between different structure models and will
provide direct images of the inner regions of the jet with 20--30 $\mu$as (5--7
light months) resolution.
