Notes. RA and Dec coordinates correspond to the optical centres from NED. Errors on the total HI fluxes are evaluated as described in Sect. 3. ‘Flux (literature)’ shows the total fluxes measured from other surveys as follows: ^(⋄)Courtois et al. (2009); ^(△)Bureau et al. (1996); ^(*)Matthews et al. (1998); ^(°)Theureau et al. (1998); ^(▿)Schröder et al. (2001); ^(▾)Koribalski et al. (2004); ^(▴)HIPASS data reprocessed by us. The total flux uncertainty of the comparison spectra are calculated as described in Sect. 3 combining the noise in the spectrum and the flux-scale uncertainty of each survey except for ESO 358-G016 for which the flux-scale uncertainty was not provided. For this galaxy we show the uncertainty on the total flux given in Bureau et al. (1996). Columns ‘Morph.’ and ‘D₂₅(B)’ show the optical morphology and the optical size of our galaxies used in Sect. 3.2 to evaluate the expected HI content of our galaxies with the Haynes & Giovanelli’s (1984) method. D₂₅(B) is the optical isophotal diameter measured at 25 mag arcsec⁻² in B-band; we collected these values from NED for 17 out of 24 galaxies. Almost all of the optical diameters comes from RC3 catalogue (de Vaucouleurs et al. 1991), two out of 15 are from Lauberts & Valentijn (1989). We estimated D₂₅(B) for all the remaining galaxies except for FCC 323 as follows: from the optical multi-component decomposition made by Su et al. (2021), we scaled the r-band radial profile to B-band. In order to do this, we previously converted g–r from Venhola et al. (2019) to obtain B–r using the intermediate conversion formula g–r to B–g (Lupton 2005). In column ‘Notes’: HI def, HI dist, N 1365 s.group stand for HI deficient, HI morphologically disturbed galaxy, and galaxy included in the NGC 1365 subgroup, respectively.