Context : Dynamically undisrupted , young populations of stars are crucial in studying 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 search for associations containing young stars ( SACY ) sample , 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 and triple-lined spectroscopic systems ( SB2/SB3s ) , in addition to this we computed radial velocity ( RV ) values for our subsample of SACY targets using several epochs of fiber-fed extended range optical spectrograph ( FEROS ) and ultraviolet and visual echelle spectrograph ( UVES ) data .
These values were used to revise the membership of each association that was 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 seven 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 close star-forming regions ( \approx 1-2 Myr ) and the field ( F _ { \mathrm { m } } \leq 10 % ) .
These are seen 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 } ] , respectively .

Conclusions : Our results are consistent with the picture of universal star formation , when compared to the field and close star-forming regions ( SFRs ) .
We comment on the implications of the relationship between increasing multiplicity fraction with the primary mass within the close companion range in relation to star formation .