  The Paschen beta (1.2822 micron) emission line found in the near-infrared
spectra of T-Tauri stars (TTSs) is believed to trace the accretion of material
onto the central star. We present spectroscopic data which suggests that this
may not always be the case. The technique of spectro-astrometry is used by us
to measure positional displacements in the Pab emission from four T-Tauri
stars, namely DG Tau, V536 Aql, LkHalpha 321 and RW Aur. We also observed the
optical forbidden emission from these sources. Forbidden emission lines are
formed in the outflows that accompany the evolution of protostars and so are
ideal to use as a comparison to confirm that the measured offsets in the Pab
emission are indeed due to outflowing material. Models based on the
magnetospheric accretion theory have been the most successful to date in
explaining the origin of atomic hydrogen emission lines. Yet we see that the
line profiles of the sources showing displacement in their Pab emission all
have features that the magnetospheric accretion model has so far failed to
explain, such as broad full width half maxima, large wings and an absence of
red shifted absorption features. The failure of the models to explain the
presence of large extended wings in the line profiles is particularly
interesting in the context of this study as in all cases it is in the extended
wings that we measure offsets in position with respect to the source.
