tokens: (5) predicted H i mass derived using equation ( 1 ); and (6) calculated H i deficiencies. 3.2 H <sc>i</sc> kinematics of the NGC 7232/3 triplet Although the coarse velocity resolution of our observations does not allow for the detailed analysis of the kinematics of the triplet galaxy group and its surroundings, it is clear from the Fig. 5 that NGC 7232B has higher velocities and is kinematically different from NGC 7232 and NGC 7233 (velocity difference of up to 400 km s −1 ). The H i debris appears to have similar velocities to NGC 7233 and NGC 7232 within ∼200 km s −1 , which could indicate that most of this gas is coming from the interaction between the galaxy pair and not NGC 7232B. Figure 5. MeerKAT-64 H i velocity field map of the NGC 7232/3 triplet. The black stars indicate the optical centres of the triplet galaxies. 3.3 H <sc>i</sc> deficiency equation of the NGC 7232/3 triplet We determine the H i deficiency of each galaxy in the NGC 7232/3 triplet group to determine if the group spirals are H i -deficient or H i -rich. The H i deficiency is derived by comparing the observed H i mass to the expected H i mass for an isolated galaxy. The expected H i masses () are derived from the absolute B -magnitudes obtained from HyperLeda 4 (Makarov et al. 2014 ). We have used the scaling relation derived in (Jones et al. 2018 ) based on measurements or constraints on the H i masses of 844 isolated galaxies compiled by the AMIGA project (Analysis of the interstellar Medium in Isolated GAlaxies; Verdes-Montenegro et al. 2005 ): where log [ L B / L ⊙ ] is derived by where M bol, ⊙ is the Sun's bolometric absolute magnitude, we adopt M bol, ⊙ = 4.88 (Lisenfeld et al. 2011 ), D is the distance in Mpc, and B c is the absolute B -magnitude corrected for extinction. The H i deficiency is then defined by where is the H i mass derived from the observations. Positive values of DEF indicate H i deficiency while negative values indicate H i excess. We compare the expected H i mass for each galaxy to its H i mass derived from our observations (see Table 2 ). NGC 7232 and NGC 7233 are H i -deficient while NGC 7232B is found to have excess H i . Taking into account the uncertainties in B -magnitudes and the scatter in the scaling relation, we consider a galaxy to be H i -deficient when DEF > 0.2 and H i excess if DEF −0.2. The total H i mass of the NGC 7232/3 triplet including all the H i debris (i.e. H i streams and clouds) is ] = 9.84 ± 0.002. Comparing the total derived H i mass to the expected H i mass of , we find a total DEF of −0.23 ± 0.11, which indicates that the NGC 7232/3 galaxy triplet has an overall H i excess compared to field galaxies. 4 DISCUSSION One of the questions coming from our data is the possible origin of the H i debris observed. In this work, we search for signs of interaction within the NGC 7323/3 galaxy triplet and its surrounding environment. The detection of wide-spread H i debris around the galaxy triplet demonstrates the need for
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