  Context: Dynamically undisrupted, young populations of stars are crucial to
study the role of multiplicity in relation to star formation. Loose nearby
associations provide us with a great sample of close ($<$150 pc) Pre-Main
Sequence (PMS) stars across the very important age range ($\approx$5-70 Myr) to
conduct such research.
  Aims: We characterize the short period multiplicity fraction of the SACY
(Search for Associations Containing Young stars) accounting for any
identifiable bias in our techniques and present the role of multiplicity
fractions of the SACY sample in the context of star formation.
  Methods: Using the cross-correlation technique we identified double-lined
spectroscopic systems (SB2), in addition to this we computed Radial Velocity
(RV) values for our subsample of SACY targets using several epochs of FEROS and
UVES data. These values were used to revise the membership of each association
then combined with archival data to determine significant RV variations across
different data epochs characteristic of multiplicity; single-lined multiple
systems (SB1).
  Results: We identified 7 new multiple systems (SB1s: 5, SB2s: 2). We find no
significant difference between the short period multiplicity fraction
($F_\mathrm{m}$) of the SACY sample and that of nearby star forming regions
($\approx$1-2 Myr) and the field ($F_\mathrm{m}\leq$10%) both as a function of
age and as a function of primary mass, $M_1$, in the ranges $P$ [1:200 day] and
$M_2$ [0.08 $M_{\odot}$-$ M_1$].
  Conclusions: Our results are consistent with the picture of universal star
formation, when compared to the field and nearby star forming regions (SFRs).
We comment on the implications of the relationship between increasing
multiplicity fraction with primary mass, within the close companion range, in
relation to star formation.

Solar and Stellar Astrophysics