SINFONI spectrum of the close double star located 21^″ northeastof the HH 250-IRS binary, initially suspected to be physically related to the system. Despite the low photospheric temperature indicated by the appearance of the NaI (2.206 μm) and CaI (2.262 μm) lines and the deep CO bands, the spectrum is distinctly different from that of a low-mass young stellar object, being instead typical of a late-type giant or supergiant star. The apparent emission at 2.166 μm is an artifact due to the presence of Brγ absorption in the spectrum of the star used for telluric features correction.