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tokens: the LAEs in each band (AB); (4) lensing magnification factors derived in Shu et al. ( 2016c ) for the first four lensed LAEs, Marques-Chaves et al. ( 2017 ) for BG1429+1202, and in Section 3 for BG1501+3042; (5) stellar UV continuum slope (equation 2 ), UV dust extinction (AB mag, equation 3 ), and colour excess of the stellar continuum assuming the Reddy et al. ( 2015 ) attenuation curve; (6) observed flux (units of 10 −16 erg s −1 cm −2 ), rest-frame equivalent width (Å), and full width at half-maximum (km s −1 ) of the Lyα line; (7) centroid velocity of Lyα and ISM absorption lines (average) relative to the systemic redshift (km s −1 ); (8) low-ISM and H i covering fractions using the depth of the average absorption line profile of ISM lines (Si ii 1260 Å, C ii 1334 Å, and Si ii 1526 Å) and using the relation of Gazagnes et al. ( 2018 ), respectively; (9) intrinsic UV absolute magnitudes (AB) and star formation rates (M ⊙ yr −1 ; equation 4 ); (10) intrinsic Lyα luminosity (units of 10 42 erg s −1 ) and star formation rates (M ⊙ yr −1 ; equation 9 ); and (11) Lyα escape fraction. a The ACAM/WHT i -band data of BG0201+3228 are affected by a high background level. The projected separation between the centroids of the two components in the source plane is about 0.46 ± 0.06 arcsec which at z = 2.645 corresponds to 3.8 ± 0.6 kpc for the adopted cosmology, suggestive of a close interacting/merging system. Nevertheless, we cannot confirm unambiguously the merging scenario as no velocity offset between the lensed images ‘A’ and ‘B’ is clearly detected in the available spectrum (with a resolution of ≃ 450 km s −1 FWHM). The sources have effective radius kpc and kpc. 4 RESULTS FROM IMAGING DATA 4.1 Photometry As seen in Fig. 1 the morphology of the LAEs in this sample consists of complex arc-like features with multiple lensed images seen in the observer plane. Given the typical ∼0.8 arcsec FWHM seeing of the GTC, WHT, and CFHT images, there is light contamination from the foreground lens galaxies. In order to perform a clean photometry of the lensed images, we use the two-dimensional fitting program galfit (Peng et al. 2002 , 2010 ) to model and substract the light distribution of the foreground lens (and in some cases additionally nearby objects). We use Sérsic profiles centred at the centroids of each LRG light emission allowing only two pixels freedom (∼0.5 arcsec). For the four lensed LAEs with HST imaging, we use the models of the foreground lens presented in Shu et al. ( 2016c ) as priors in our modelling (i.e. effective radius, minor-to-major axial ratio, and major-axis position angle). Nearby stars were used as PSF models. We further use SExtractor (Bertin Arnouts 1996 ) to measure the magnitudes in each band. To do so, we use aperture photometry using apertures with diameters of 2.5 times the FWHM of the PSF. Aperture photometry was performed for compact lensed morphologies, such as the lensed images of BG0755+3445, BG1429+1202 and the