  The identification and characterisation of low-mass binaries is of importance
for a range of astrophysical investigations. Low-mass binaries in young
($\sim10 - 100 $ Myr) moving groups (YMGs) are of particular significance as
they provide unique opportunities to calibrate stellar models and evaluate the
ages and coevality of the groups themselves. Low-mass M-dwarfs have pre-main
sequence life times on the order of $\sim100$ Myr and therefore are continually
evolving along a mass-luminosity track throughout the YMG phase, providing
ideal laboratories for precise isochronal dating, if a model-independent
dynamical mass can be measured. AstraLux lucky imaging multiplicity surveys
have recently identified hundreds of new YMG low-mass binaries, where a
subsample of M-dwarf multiples have estimated orbital periods less than 50
years. We have conducted a radial velocity survey of a sample of 29 such
targets to complement the astrometric data. This will allow enhanced orbital
determinations and precise dynamical masses to be derived in a shorter
timeframe than possible with astrometric monitoring alone, and allow for a more
reliable isochronal analysis. Here we present radial velocity measurements for
our sample over several epochs. We report the detection of the three-component
spectroscopic multiple 2MASS J05301858-5358483, for which the C component is a
new discovery, and forms a tight pair with the B component. Originally
identified as a YMG member, we find that this system is a likely old field
interloper, whose high chromospheric activity level is caused by tidal spin-up
of the tight BC pair. Two other triple systems with a tight pair exist in the
sample, but for the rest of the targets we find that additional tidally
synchronized companions are highly unlikely, providing further evidence that
their high chromospheric activity levels are generally signatures of youth.
