  In a previous paper (McGroarty & Ray 2004, 420, 975) we examined the
environment of a number of evolved low-mass young stars, i.e. Classical T Tauri
Stars, to see if they are capable of driving parsec-scale outflows. These stars
- CW Tau, DG Tau, DO Tau, HV Tau C and RW Aur - were previously known to drive
only "micro-jets" or small-scale outflows of < 1' or 0.04 pc at the distance of
the Taurus-Auriga Cloud. We found that they drive outflows of 0.5pc - 1pc,
based on the morphology and alignment of newly discovered and previously known
HH objects with these sources and their "micro-jets". Here, we use a
cross-correlation method to determine the proper motions of the HH objects in
these five outflows (HH 220, HH 229, HH 702, HH 705 and HH 826 - HH 835) which
in turn allows us to confirm their driving sources. Moreover, the tangential
velocities of HH objects at large distances from their origin are currently
poorly known so these proper motions will allow us to determine how velocities
evolve with distance from their source. We find tangential velocities of
typically 200 kms^-1 for the more distant objects in these outflows.
Surprisingly, we find similar tangential velocities for the "micro-jets" that
are currently being ejected from these sources. This leads us to suggest that
either the outflow velocity was much higher 10^3 years ago when the more
distant objects were ejected and that these objects have decelerated to their
current velocity or that the outflow velocity at the source has remained
approximately constant and the more distant objects have not undergone
significant deceleration due to interactions with the ambient medium. Numerical
simulations are needed before we can decide between these scenarios.
