We had reported in ( 2 ) on the near-infrared ( NIR ) identification of a possible counterpart to the black hole candidate XTE J1908+094 obtained with the ESO/NTT .
Here , we present new , follow-up , CFHT adaptive optics observations of the XTE J1908+094 field , which resolved the previously proposed counterpart in two objects separated by about 0 { \hbox to 0.0 pt { . } } ^ { \prime \prime } 8 .
Assuming that both objects are potential candidate counterparts , we derive that the binary system is a low-mass system with a companion star which could be either an intermediate/late type ( A-K ) main sequence star at a distance of 3-10 kpc , or a late-type ( > K ) main sequence star at a distance of 1-3 kpc .
However , we show that the brighter of the two objects ( J \sim 20.1 , H \sim 18.7 , K ^ { \prime } \sim 17.8 ) is more likely to be the real counterpart of the X-ray source .
Its position is more compatible with our astrometric solution , and colours and magnitudes of the other object are not consistent with the lower limit of 3 kpc derived independently from the peak bolometric flux of XTE J1908+094 .
Further multi-wavelength observations of both candidate counterparts are crucial in order to solve the pending identification .