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tokens: thick discs. We observed (see Table 1 ) the mid-plane of NGC 4111 with the SCORPIO in the wavelength range 4800–5600 Å with the spectral resolution ∼2.2 Å =55 km s −1 . The remaining five data sets were obtained using SCORPIO-2 at slightly lower spectral resolution (∼3.8 Å =95 km s −1 at 5100 Å) at the broader wavelength range (3600–7070 Å). Table 1. Long-slit spectroscopy of the sample galaxies. We reduced our spectroscopic observations with our own idl -based reduction pipeline. We estimated the night sky background from outer slit regions not covered by our target galaxies and an optimized sky subtraction technique that takes into account spectral resolution variations along the slit (Katkov Chilingarian 2011 ; Katkov, Sil'chenko Afanasiev 2014 ). All three galaxies were observed with the Infrared Array Camera (IRAC) at Spitzer Space Telescope in the imaging mode at wavelengths 3.6 μm and 4.5 μm. We fetched fully reduced 3.6 μm images from the Spitzer Heritage Archive. 1 2.3 Data analysis Van der Kruit Searle ( 1981 ) have shown that in case an isothermal disc in the equilibrium state the vertical disc density profiles are described by the law I = I 0 sech 2 ( z / z 0 ), where I 0 is the central intensity and z 0 is the disc scale-height. We fitted vertical profiles obtained by averaging Spitzer IRAC images along the radius using models including one and two components. We set central positions of both components to be the same in the case of two-component fitting but left the position itself a free parameter. Our results for NGC 4111 and NGC 5422 quantitatively agree with those presented in the S4G survey (Salo et al. 2015 ), however the results for NGC 4710 decomposition were not presented there. To derive internal kinematics and stellar population properties (mean ages and metallicities [Fe/H]) of thick and thin discs we first binned our long slit spectra in the spatial direction with the adaptive binning algorithm in order to reach the minimal signal-to-noise ratio S / N = 30 per bin per spectral pixel in the middle of the wavelength range. Then, in every bin we applied the nbursts full spectral fitting technique (Chilingarian et al. 2007a , b ) with a grid of high resolution stellar pegase.hr (Le Borgne et al. 2004 ) simple stellar population (SSP) models based on the ELODIE3.1 empirical stellar library (Prugniel et al. 2007 ). The nbursts technique implements a pixel space χ 2 minimization algorithm where observed spectrum is approximated by a stellar population model broadened with parametric line-of-sight velocity distribution (LOSVD) and multiplied by polynomial continuum (10th degree in our case) to take into account dust attenuation and/or possible flux calibration imperfections in both observations and models. We used Gaussian parametrization of the stellar LOSVD, except our higher resolution mid-plane spectra of NGC 4111 where we exploited the standard Gaussian–Hermite parametrization (van der Marel Franx 1993 ). The [Mg/Fe]