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tokens: from the MPA-JHU DR7 catalogue, and we obtained MBH only for galaxies classified as ellipticals (see Section 3 ). The values are given in Table 8 . MLLINERs cover the range between log (MBH/M ⊙ ) = 7.03–8.57 with a median value of log (MBH/M ⊙ ) = 7.45, while LLINERs show MBH in the range log (MBH/M ⊙ ) = 6.24–8.54 and median value of log (MBH/M ⊙ ) = 8.04. Interestingly, our MLLINERs do not contain the most massive BHs in their centres. It could be surprising that MLLINERs, having on average higher SFRs than LLINERs, show in general lower stellar masses. Different works, both observational (Kauffmann et al. 2003b ; Mateus et al. 2006 ; Leauthaud et al. 2012 ; Pérez et al. 2013 ) and numerical (Shankar et al. 2006 ; Behroozi et al. 2012 ), revealed a stellar mass of ∼6 × 10 10 M ⊙ as critical for the growth rate of stellar populations. In particular, in Pérez et al. ( 2013 ) by studying a 3D spectroscopic sample of 105 local galaxies, the authors found that in galaxies more massive than 5 × 10 10 M ⊙ the inner regions ( 0.5 R 50 ) grew as much as 50–100 per cent faster than in the lower mass galaxies. They found that the peak of relative growth rates of inner and outer galaxy regions correspond to the stellar mass of 6–7 × 10 10 M ⊙ (see their fig. 5), while for lower and higher masses the growth rate decreases and therefore SFRs (LSF) as well. The median stellar mass of our MLLINERs (6.58 × 10 10 M ⊙ ) corresponds perfectly to this region, while for most LLINERs their stellar masses are already higher and correspond to lower values of the relative growth rate (lower LSF). This explains why MLLINERs having in average lower stellar masses in comparison to LLINERs, have higher LSF. In addition, we studied the stellar mass distributions of MLLINERs and LLINERs for the three morphological groups. Table 9 shows the median stellar masses for different morphological types. As can be seen, of three morphological types the highest difference was obtained for early-type galaxies. These galaxies represent a significant fraction of MLLINERs (40 per cent, see Fig. 8 ) and their median mass corresponds exactly to the highest relative growth rate of stellar populations (according to Pérez et al. 2013 ), which then could explain their high SFR values. This is not the case for early-type LLINERs that are characterized by higher stellar masses (lower growth rates) and lower SFRs. Table 9. Median total stellar masses of MLLINERs and LLINERs in relation to morphology (given as logarithm and in M ⊙ ). 5.1.2 Extinction We found that our MLLINERs can be hosted by galaxies with a wide range of extinctions. When using the Av measurements based on the Hα and Hβ emission lines, we find that most of them reside in galaxies with high extinctions. The median Av is 1.65 mag, covering the range 0.49–3.46 mag (see Fig. 7 , top plot). For comparison, the bottom plot in Fig. 7 shows the Av distributions of LLINERs and MLLINERs when taking into account the SDSS MPA-JHU DR7 3