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tokens: in the closure phases across these spectral channels at 200 cycles/arcsec (cf. Sect. 4.3 , Fig. 6). However, we cannot currently exclude an uncertainty of the position of the dominant spot of this order in the imaging process. 4.5. Fundamental parameters of R Scl Table 5 Fundamental properties of R Scl used in this work. Notes. 1: Discussion in Sect. 2.1 ; 2: Whitelock et al. (2008) ; 3: integrated photometry, see Sect. 2.1 ; 4: this work, average of our three epochs, see Sect. 4 ; 5: calculated from 2 and 4; 6: calculated from 3 and 4; 7: calculated from 2 and 3; 8: 7 and 8 with evolutionary tracks by Lagarde et al. (2012) ; 9: 6 and 9. Fig. 11 Position of R Scl in the HR diagram together with evolutionary tracks by Lagarde et al. (2012) . The tracks are those without rotation and reach up to the start of the TP-AGB. Masses are ZAMS masses; values in parenthesis are masses at the start of the TP-AGB, that is, at the end of the shown tracks. Table 5 summarizes the fundamental parameters of R Scl that we used in this work, including our adopted values for the bolometric flux and distance, the measured Rosseland angular diameter, and the derived effective temperature and luminosity. We note that the distance to R Scl is quite uncertain, as discussed in Sect. 2.1 , which is reflected in its large adopted error. Figure 11 shows the position of R Scl in the Hertzsprung-Russell (HR) diagram based on the effective temperature and luminosity. This figure includes stellar evolutionary tracks by Lagarde et al. (2012) for zero age main sequence (ZAMS; initial) masses between 1 and 2.5 . These tracks reach up to the start of the thermally pulsing (TP) AGB, at which point the mass range is 0.7 to 2.5 . The position of R Scl is consistent with an evolutionary phase shortly beyond the start of the TP-AGB and with an initial mass interval between 1 and 2 . We also compared the position of R Scl to the tracks of the TP-AGB by Marigo et al. (2013) as shown by Klotz et al. (2013) . Here, R Scl is also consistent with masses at the start of the TP-AGB between about 1 and 2 , that is, not significantly below 1 and not significantly above 2 . These are evolutionary tracks for single stars, while a binary companion has been detected for R Scl. However, based on the estimates for the binary companion mass and separation ( Maercker et al. 2016 ), it is unlikely that the companion has affected the evolution of R Scl to the AGB. As a result, we estimate the initial mass of R Scl to be 1.5 0.5 and the current mass to be 1.3 0.6 . Together with our estimate of the radius, these values correspond to a surface gravity of –0.6 0.4. The mass of R Scl can also be estimated by the pulsation properties. We used the formula from Wood (1990) , where is the pulsation constant, and and are the mass and radius in solar units. We estimated a value of 0.093 0.005 for the given ranges of masses and pulsation periods based on Fox Wood (1982) and assuming fundamental pulsation