We present results from a large , high-spatial-resolution near-infrared imaging search for stellar and sub-stellar companions in the Taurus-Auriga star-forming region .
The sample covers 64 stars with masses between those of the most massive Taurus members at \sim 3 M _ { \odot } and low-mass stars at \sim 0.2 M _ { \odot } .
We detected 74 companion candidates , 34 of these reported for the first time .
Twenty-five companions are likely physically bound , partly confirmed by follow-up observations .
Four candidate companions are likely unrelated field stars .
Assuming physical association with their host star , estimated companion masses are as low as \sim 2 M _ { \mathrm { Jup } } .
The inferred multiplicity frequency within our sensitivity limits between \sim 10–1500 AU is 26.3 ^ { +6.6 } _ { -4.9 } \% .
Applying a completeness correction , 62 % \pm 14 % of all Taurus stars between 0.7 and 1.4 M _ { \odot } appear to be multiple .
Higher order multiples were found in 1.8 ^ { +4.2 } _ { -1.5 } \% of the cases , in agreement with previous observations of the field .
We estimate a sub-stellar companion frequency of \sim 3.5–8.8 % within our sensitivity limits from the discovery of two likely bound and three other tentative very low-mass companions .
This frequency appears to be in agreement with what is expected from the tail of the stellar companion mass ratio distribution , suggesting that stellar and brown dwarf companions share the same dominant formation mechanism .
Further , we find evidence for possible evolution of binary parameters between two identified sub-populations in Taurus with ages of \sim 2 Myr and \sim 20 Myr , respectively .