[en] We report the results obtained by a broad-band (0.5–500 keV) data analysis of narrow-line Seyfert 1 galaxy NGC 4748 observed with an XMM-Newton/PN, INTEGRAL/ISGRI and SWIFT/BAT telescopes. This galaxy has a soft X-ray excess that is typical for the class of narrow-line Seyfert 1. The question of the origin of soft excess in such objects is still unclear. We tested and compared two spectral models for the soft X-ray spectra based on the different physical scenarios. The first one is based on the Done and Nayakshin model of two-phase accretion disc in a vertical direction, which includes two reflection zones with different ionization levels. According to this model, we found that a highly ionized reflection has the value of ionization $\mathrm{\xi <!--\; ??\; -->}\sim <!--\; ???\; -->3000\text{erg}{\text{s}}^{-<!--\; ???\; -->1}\text{cm}$ and is mostly responsible for the soft excess. This reflection becomes comparable with a low ionized one ($\mathrm{\xi <!--\; ??\; -->}\sim <!--\; ???\; -->30\text{erg}{\text{s}}^{-<!--\; ???\; -->1}\text{cm}$) in moderate X-ray range. However, this model requires also an additional component at soft energies with $kT\sim <!--\; ???\; -->300$ eV. The second model is an energetically self-consistent model and assumes that a soft excess arises from optically thick thermal Comptonization of the disc emission. Combination of the UV (from XMM/Optical monitor) and X-ray data in the latter model allowed us to determine a mass of the central black hole of $6.9\times <!--\; ??\; -->{10}^6{M}_{\odot <!--\; ???\; -->}$ and Eddington ratio ${\log }_{L/L_{Edd}}\simeq <!--\; ???\; -->-<!--\; ???\; -->0.57$. Also, we were not able to rule out one of competing models using only X-ray spectra of NGC 4748.