  We report the results of a comprehensive analysis of X-ray (Chandra and Swift
observatories), optical (Southern African Large Telescope, SALT) and
near-infrared (the VVV survey) observations of the Be/X-ray binary pulsar
2S1553-542. Accurate coordinates for the X-ray source are determined and are
used to identify the faint optical/infrared counterpart for the first time.
Using VVV and SALTICAM photometry, we have constructed the spectral energy
distribution (SED) for this star and found a moderate NIR excess that is
typical for Be stars and arises due to the presence of circumstellar material
(disk). A comparison of the SED with those of known Be/X-ray binaries has
allowed us to estimate the spectral type of the companion star as B1-2V and the
distance to the system as $>15$ kpc. This distance estimation is supported by
the X-ray data and makes 2S1553-542 one of the most distant X-ray binaries
within the Milky Way, residing on the far side in the Scutum-Centaurus arm or
even further.
