Context : Massive binaries play a crucial role in the Universe .
Knowing the distributions of their orbital parameters is important for a wide range of topics from stellar feedback to binary evolution channels and from the distribution of supernova types to gravitational wave progenitors , yet no direct measurements exist outside the Milky Way .

Aims : The Tarantula Massive Binary Monitoring project was designed to help fill this gap by obtaining multi-epoch radial velocity ( RV ) monitoring of 102 massive binaries in the 30 Doradus region .

Methods : In this paper we analyze 32 FLAMES/GIRAFFE observations of 93 O- and 7 B-type binaries .
We performed a Fourier analysis and obtained orbital solutions for 82 systems : 51 single-lined ( SB1 ) and 31 double-lined ( SB2 ) spectroscopic binaries .

Results : Overall , the binary fraction and orbital properties across the 30 Doradus region are found to be similar to existing Galactic samples .
This indicates that within these domains environmental effects are of second order in shaping the properties of massive binary systems .
A small difference is found in the distribution of orbital periods , which is slightly flatter ( in log space ) in 30 Doradus than in the Galaxy , although this may be compatible within error estimates and differences in the fitting methodology .
Also , orbital periods in 30 Doradus can be as short as 1.1 d , somewhat shorter than seen in Galactic samples .
Equal mass binaries ( q > 0.95 ) in 30 Doradus are all found outside NGC 2070 , the central association that surrounds R136a , the very young and massive cluster at 30 Doradus’s core .
Most of the differences , albeit small , are compatible with expectations from binary evolution .
One outstanding exception , however , is the fact that earlier spectral types ( O2–O7 ) tend to have shorter orbital periods than later spectral types ( O9.2–O9.7 ) .

Conclusions : Our results point to a relative universality of the incidence rate of massive binaries and their orbital properties in the metallicity range from solar ( Z _ { \odot } ) to about half solar .
This provides the first direct constraints on massive binary properties in massive star-forming galaxies at the Universe ’ s peak of star formation at redshifts z \sim 1 to 2 which are estimated to have Z \sim 0.5 Z _ { \odot } .