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tokens: by Proshina et al. (2020) . 2. Observations and the data involved Our long-slit spectral observations were made with a multi-mode focal reducer SCORPIO-2 ( Afanasiev Moiseev 2011 ) at the prime focus of the Russian 6 m telescope of the Special Astrophysical Observatory, Russian Academy of Sciences. UGC 5936 was observed on February 28, 2014. In these observations, the 1′′ slit was aligned with the major axis, PA(slit) = 83deg, and the total exposure time was 75 min; also the target was exposed in the orientation through the neighbouring dwarf galaxy, PA(slit) = 135deg, with the exposure time of 45 min. The seeing during these observations was mediocre, F W H M = 3′′. We used the VPHG1200@540 grism providing an intermediate spectral resolution F W H M ≈ 5 Å in the wavelength region from 3700 Å to 7200 Å. This spectral range includes a set of strong absorption and emission lines making it suitable to analyse both stellar and gaseous kinematics of the galaxy as well as the gas excitation and chemistry and properties of the stellar populations. The slit is 6′ in length, which allowed us to use the edge spectra for subtraction of the sky background. The CCD E2V CCD42-90, with a format of 2048 × 4600, using in the 1 × 2 binning mode provided a spatial scale of 0.357 ′′/px and a spectral sampling of 0.86 Å/px. The data reduction as well as kinematics and stellar population characteristics derivation were standard for our SCORPIO-2 data; see for example Sil’chenko et al. (2019) or Proshina et al. (2020) . We used the g r -band images from the SDSS/DR9 archive ( Ahn et al. 2012 ) to study the large-scale structure of the galaxy. 3. Photometric and dynamical structure of UGC 5936 The smooth lenticular galaxy UGC 5936 (see 2MASS J -band image, Fig. 1 , lower middle) possesses a large pseudo-ring which looks unclosed in the optical continuum bands (Fig. 1 , upper left). However Fig. 1 (lower right), which shows the WISE/W3 data in the 12 μ m band delineates a perfect closed ring; in this figure hot dust heated by star formation reveals its organisation in a typical S0 outer ring structure. The colour map (Fig. 1 , upper right), demonstrates the blue colour of the ring, which is narrow to the east and splits into two arcs to the west, as well as the red colour of the arc connecting the core and the western part of the ring. The western blue-ring structures correspond to the ring in the unsharp-masked image (Fig. 1 , upper middle). Interestingly, the GALEX near-ultraviolet (NUV) map (Fig. 1 , lower left), which also refers to young star concentration, shows UV flux excesses beyond the borders of the continuum-band pseudo-ring; the offset is seen especially well at the major axis. To the south-east from UGC 5936, a small satellite, SDSS J105009.10+362009.9 , is observed at 15 kpc projected onto the sky plane; this satellite is observed at 19 kpc if we suggest that it lies in the plane of the UGC 5936 disc. This small satellite is very blue. According to