We present the orbital and physical parameters of a newly discovered low-mass detached eclipsing binary from the All-Sky Automated Survey ( ASAS ) database : ASAS J011328-3821.1 A – a member of a visual binary system with the secondary component separated by about 1.4 seconds of arc .
The radial velocities were calculated from the high-resolution spectra obtained with the 1.9-m Radcliffe/GIRAFFE , 3.9-m AAT/UCLES and 3.0-m Shane/HamSpec telescopes/spectrographs on the basis of the todcor technique and positions of H _ { \alpha } emission lines .
For the analysis we used V and I band photometry obtained with the 1.0-m Elizabeth and robotic 0.41-m PROMPT telescopes , supplemented with the publicly available ASAS light curve of the system .

We found that ASAS J011328-3821.1 A is composed of two late-type dwarfs having masses of M _ { 1 } = 0.612 \pm 0.030 M _ { \odot } , M _ { 2 } = 0.445 \pm 0.019 M _ { \odot } and radii of R _ { 1 } = 0.596 \pm 0.020 R _ { \odot } , R _ { 2 } = 0.445 \pm 0.024 R _ { \odot } , both show a substantial level of activity , which manifests in strong H _ { \alpha } and H _ { \beta } emission and the presence of cool spots .
The influence of the third light on the eclipsing pair properties was also evaluated and the photometric properties of the component B were derived .
Comparison with several popular stellar evolution models shows that the system is on its main sequence evolution stage and probably is more metal rich than the Sun .
We also found several clues which suggest that the component B itself is a binary composed of two nearly identical \sim 0.5 M _ { \odot } stars .