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We present the new results of our long-term observational project to detectthe small variations in the orbital periods of low-mass and short-periodeclipsing binaries. About 120 new precise mid-eclipse times were obtained forthree relatively well-known dwarf eclipsing binaries: SDSS J143547.87+373338.5(P = 0.126 d), NSVS 07826147 (0.162 d), and NSVS 14256825 (0.110 d).Observed-minus-calculated (O-C) diagrams of these systems were analyzed usingall accurate timings, and, where possible, new parameters of the light-timeeffect were calculated. For the first time, we derive (or improve upon previousfindings with regard to) the short orbital periods of 13 and 10 years ofpossible third bodies for SDSS J143547.87+373338.5 and NSVS 07826147,respectively. In these binaries, our data show that period variations can bemodeled simply on the basis of a single circumbinary object. For the first twoobjects, we calculated the minimum mass of the third components to be 17 MJ,and 1.4 MJ respectively, which corresponds to the mass of a brown dwarf or agiant planet. For NSVS 14256825, the cyclical period changes caused by a singleadditional body cannot be confirmed by our recent eclipse time measurements.More complex behavior connected with two orbiting bodies, or yet unknowneffects, should be taken into account.

Possible substellar companions in dwarf eclipsing binaries: SDSS J143547.87+373338.5, NSVS 7826147, and NSVS 14256825