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We study the X-ray transient Swift J1745-26, using observations obtained fromits outburst in September 2012, up to its decay towards quiescence in March2013. We obtained optical and infrared observations, through override programmeat ESO/VLT with FORS2 and ISAAC instruments, and archival optical (VLT/VIRCAM),radio and X-ray (Swift) observations, to build the lightcurve and thebroad-band Spectral Energy Distribution (SED) of Swift J1745-26. We show that,during its outburst and also during its decay towards quiescence, SwiftJ1745-26 SED can be adjusted, from infrared up to X-rays, by the sum of both aviscous irradiated multi-colour blackbody emitted by an accretion disk, and asynchrotron powerlaw at high energy. In the radio domain, the SED arises fromsynchrotron emission from the jet. While our SED fitting confirms that thesource remained in the low/hard state during its outburst, we determine anX-ray spectral break at frequency 3.1 < nu_break < 3.4 x 10^14 Hz, and a radiospectral break at 10^12 Hz < nu_break < 10^13 Hz. We also show that the systemis compatible with an absorption Av of ~7.69 magnitudes, lies within a distanceinterval of D~[2.6-4.8] kpc, with an upper limit of orbital period P_orb = 11.3hours, and that the companion star is a late-type star of spectral type in therange K0 - M0 V, confirming that the system is a low-mass X-ray binary. Wefinally plot the position of Swift J1745-26 on an optical-infrared - X-rayluminosity diagram: its localization on this diagram is consistent with thesource staying in the low-hard state during outburst and decay phases.

Broad-band spectral energy distribution of the X-ray transient Swift J1745-26 from outburst to quiescence