  In this paper a comprehensive analysis of VLT / X-Shooter observations of two
jet systems, namely ESO-H$\alpha$ 574 a K8 classical T Tauri star and Par-Lup
3-4 a very low mass (0.13~\Msun) M5 star, is presented. Both stars are known to
have near-edge on accretion disks. A summary of these first X-shooter
observations of jets was given in a 2011 letter. The new results outlined here
include flux tables of identified emission lines, information on the
morphology, kinematics and physical conditions of both jets and, updated
estimates of $\dot{M}_{out}$ / $\dot{M}_{acc}$. Asymmetries in the \eso flow
are investigated while the \para jet is much more symmetric. The density,
temperature, and therefore origin of the gas traced by the Balmer lines are
investigated from the Balmer decrements and results suggest an origin in a jet
for \eso while for \para the temperature and density are consistent with an
accretion flow. $\dot{M}_{acc}$ is estimated from the luminosity of various
accretion tracers. For both targets, new luminosity relationships and a
re-evaluation of the effect of reddening and grey extinction (due to the
edge-on disks) allows for substantial improvements on previous estimates of
$\dot{M}_{acc}$. It is found that log($\dot{M}_{acc}$) = -9.15 $\pm$ 0.45~\Msun
yr$^{-1}$ and -9.30 $\pm$ 0.27~\Msun yr$^{-1}$ for \eso and \para respectively.
Additionally, the physical conditions in the jets (electron density, electron
temperature, and ionisation) are probed using various line ratios and compared
with previous determinations from iron lines. The results are combined with the
luminosity of the [SII]$\lambda$6731 line to derive $\dot{M}_{out}$ through a
calculation of the gas emissivity based on a 5-level atom model.
