Below, we show those data as position-velocity-diagrams (PVD), where the origin of the especial coordinate is set on the position of the brightest star and the velocity is derived from the rest-wavelength of the a feature and the radial velocity of the star.
As first step, we perform a visual inspection in the SAOImage DS9 program. Figure \ref{974356} shows an example of the data shown as a position-velocity-diagram (PVD). The vertical axis is the spatial coordinate and the horizontal access is wavelength, where we transform the wavelength into the radial velocity centered on the rest-wavelength of an FEL. Since the stellar continuum contributes signal at all wavelengths, the dispersed spectra run from the left to the right. Jets are very weak in the continuum, but can be resolved in the FELs along the slit direction. We will only be able to find outflows that happen to align with the direction of the slit. In a PVD, resolved FEL emission would cause a bulge i2n the vicinity of the rest wavelength in the emission line. If both the blue- and the redshifted jet are detected, we should see signal at a positive velocities on one side of the star and at a negative velocity on the other. For stars where the tentative signal is identified and we find a radial velocity measurement in the literature, we correct for the radial velocity of the star. We take the radial velocities from \citet{2012ApJ...745..119N} for UY Aur and from \citet{2006AstL...32..759G} for DF Tau.