Context :

Aims : We present results of the combined photometric and spectroscopic analysis of three detached eclipsing binaries , which secondary components are not visible or very hard to identify in the optical spectra – ASAS J052743-0359.7 , ASAS J065134-2211.5 , and ASAS J073507-0905.7 .
The first one is a known visual binary ADS 4022 , and we found that it is a quadruple system , composed of two spectroscopic binaries , one of which shows eclipses .
None of the systems was previously recognized as a spectroscopic binary .

Methods : Using the following telescopes/spectrographs : Subaru/IRCS , CTIO-1.5m/CHIRON , Euler/CORALIE , MPG-2.2m/FEROS , OAO-188/HIDES , and TNG/HARPS-N , we collected a number of high-resolution optical and IR spectra to calculate the radial velocities ( RVs ) and later combined them with MITSuME and ASAS photometry .
The Subaru/IRCS infra-red spectra were crucial for secure identification of the cooler components ’ lines .
RV measurements were done with the TODCOR technique , and RV curves modelled with our own procedure V2FIT .
Light curve modelling was performed with JKTEBOP and PHOEBE codes .
Temperatures and metallicities of two systems were estimated from spectra .
For the ADS 4022 system we also used the archival WDS data and new SOAR observations in order to derive the orbit of the visual pair for the first time .
Ages were estimated by comparing our results with PARSEC isochrones .

Results : The eclipsing pair ASAS J052743-0359.7 A ( P = 5.27 d ) is composed of a 1.03 ( 6 ) M _ { \odot } , 1.03 ( 2 ) R _ { \odot } primary and a 0.60 ( 2 ) M _ { \odot } , 0.59 ( 2 ) R _ { \odot } secondary .
The components of the P = 21.57 d non-eclipsing pair B likely have masses in between the two eclipsing components , and both pairs are on a \sim 188 yr orbit around their common centre of mass .
The system ASAS J065134-2211.5 ( P = 8.22 d ) consists of a 0.956 ( 12 ) M _ { \odot } , 0.997 ( 4 ) R _ { \odot } primary and a 0.674 ( 5 ) M _ { \odot } , 0.690 ( 7 ) R _ { \odot } secondary .
Finally , ASAS J073507-0905.7 ( P = 1.45 d ) , which consists of a 1.452 ( 34 ) M _ { \odot } , 1.635 ( 12 ) R _ { \odot } primary and a 0.808 ( 13 ) M _ { \odot } , 0.819 ( 11 ) R _ { \odot } secondary , is likely a pre-main-sequence system .
In all cases secondary eclipses are total .

Conclusions :