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Two faint X-ray pulsars, AX J1749.1 −2733 and AX J1749.2 −2725, located in the direction to the Galactic Center, were studied using data of INTEGRAL, XMMNewtonand CHANDRA observatories, in X-rays and SOFI/NTT in the infrared band. Combi ning data from X-ray observatories positions of both sources were determined with the uncertai nty better than∼ 1 that allowed us to identify unambiguously their optical counterparts. The following analysis of the photometry data leads us to the conclusion that the AX J1749.2 −2725 optical counterpart is a massive star of the B3 class and the system is located behind of the Galactic C enter at a distance of ∼ 14.4 kpc from us. The lack of statistics of the measurements in the K-band and a data shortage in other wavebands prevents firm conclusions about the spectral clas s of the AX J1749.1 −2733 counterpart. However, taking into account the similarity of proper ties of both pulsars we suppose that AX J1749.1−2733 should have an optical companion of the similar class an d that both sources are located behind of the Galactic Center, probably in the Pe rseus arm.

The study of the nature of sources AXJ1749.1-2733 and AX J1749.2-2725