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We study a possibility to detect signatures of brown dwarf companions in acircumstellar disc based on spectral energy distributions (SED). We present theresults of SED simulations for a system with a 0.8 $M_{\odot}$ central objectand a companion with a mass of 30 $M_J$ embedded in a typical protoplanetarydisc. We use a solution to the one-dimensional radiative transfer equation tocalculate the protoplanetary disc flux density and assume, that the companionmoves along a circular orbit and clears a gap. The width of the gap is assumedto be the diameter of the brown dwarf Hill sphere. Our modelling shows that thepresence of such a gap can initiate an additional minimum in the SED profile ofa protoplanetary disc at $\lambda = 10 - 100$ $\mu$m. We show that the depth ofthis minimum and the wavelength of the maximum difference between the SEDs ofthe system with and without a companion are related to the companion mass andits proximity to the star. We found that it is possible to detect signatures ofthe companion when it is located within 10 AU, even when it is as small as 3$M_J$. We also analyse how the disc parameters (the inner radius and thetemperature profile) change the maximum difference between the SEDs for thesame systems with and without a companion. The SED of a protostellar disc witha massive fragment might have a similar double peaked profile to the SED of amore evolved disc that contains a gap. However, in this case, it will be causedby the presence of an additional maximum at shorter wavelengths and will besimilar only when the massive fragment is relatively cold ($\sim$400 K).

The Influences of Forming Companions on the Spectral Energy Distributions of Stars with Circumstellar Discs