Multiplicity is a fundamental property that is set early during stellar lifetimes , and it is a stringent probe of the physics of star formation .
The distribution of close companions around young stars is still poorly constrained by observations .
We present an analysis of stellar multiplicity derived from APOGEE-2 spectra obtained in targeted observations of nearby star-forming regions .
This is the largest homogeneously observed sample of high-resolution spectra of young stars .
We developed an autonomous method to identify double lined spectroscopic binaries ( SB2s ) .
Out of 5007 sources spanning the mass range of \sim 0.05–1.5 M _ { \odot } , we find 399 binaries , including both RV variables and SB2s .
The mass ratio distribution of SB2s is consistent with a uniform for q < 0.95 with an excess of twins with q > 0.95 .
The period distribution is consistent with what has been observed in close binaries ( < 10 AU ) in the evolved populations .
Three systems are found to have q \sim 0.1 , with a companion located within the brown dwarf desert .
There are not any strong trends in the multiplicity fraction ( MF ) as a function of cluster age from 1 to 100 Myr .
There is a weak dependence on stellar density , with companions being most numerous at \Sigma _ { * } \sim 30 stars/pc ^ { -2 } , and decreasing in more diffuse regions .
Finally , disk-bearing sources are deficient in SB2s ( but not RV variables ) by a factor of \sim 2 ; this deficit is recovered by the systems without disks .
This may indicate a quick dispersal of disk material in short-period equal mass systems that is less effective in binaries with lower q .