  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.
  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 IR 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.
  The eclipsing pair A052743 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$188 yr
orbit around their common centre of mass. The system A065134 ($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, A073507 ($P=1.45$ 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 PMS system.
