Notes. (1) Galaxy name; (2) Luminosity of the [C II] line, calculated by directly integrating over the continuum-subtracted spectrum in the ±2.5 σ range; (3) Luminosity of the [C II] line derived from the Gaussian fitting; (4) Velocity difference between the redshifts derived from the [C II]₁₅₈ and rest-UV emission lines, where Δv = c Δz/(1 + z_UV), and Δz = z_[CII] − z_UV; (5) FWHM of the line obtained from the extracted spectrum; (6) Absolute maximum projected velocity obtained from visual inspection of the moment 1 maps of the line (see Sect. 5), with a typical 1-σ uncertainty of ≃75 km s⁻¹; (7) Reference SPW-averaged size (FWHM) of the synthesized Gaussian beam; (8) Position angle of the beam; (9) Intrinsic size (FWHM) of the source line emission; (10–11) Circularized intrinsic size (FWHM); (12) PSF scaling factor for unresolved component subtraction; (13) Fraction of extended emission (f_ext) after PSF-scaled subtraction from the source image. ^(⋄)Expected redshift based on the CO(4→3) line detection (González-López et al., in prep.). ^( † )The line in W0236+0528 is only considered as a tentative detection (see Sect. 4.1) and it is excluded from the results and discussion sections. ^( * )The line in W0410–0913 is redshifted out of the frequency range covered by the observations presented here, and only the bluest part of the profile is detected (see Fig. 2 and details in Sect. 4.1). Therefore, Col. (2) is the flux accounted by the small portion of the observed line profile, while Col. (3) is the total flux of the Gaussian fit, considering the assumptions described in Sect. 3.