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The multiple system V505 Sagittarii is composed of at least three stars: acompact eclipsing pair and a distant component, which orbit is measureddirectly using speckle interferometry. In order to explain the observed orbitof the third body in V505 Sagittarii and also other observable quantities,namely the minima timings of the eclipsing binary and two different radialvelocities in the spectrum, we thoroughly test a fourth-body hypothesis - aperturbation by a dim, yet-unobserved object. We use an N-body numericalintegrator to simulate future and past orbital evolution of 3 or 4 componentsin this system. We construct a suitable chi^2 metric from all availablespeckle-interferometry, minima-timings and radial-velocity data and we scan apart of a parameter space to get at least some of allowed solutions. Inprinciple, we are able to explain all observable quantities by a presence of afourth body, but the resulting likelihood of this hypothesis is very low. Wealso discuss other theoretical explanations of the minima timings variations.Further observations of the minima timings during the next decade orhigh-resolution spectroscopic data can significantly constrain the model.

A unified solution for the orbit and light-time effect in the V505 Sgr system