Erratum: The progenitors of compact-object binaries: Impact of metallicity, common envelope and natal kicks (Monthly Notices of the Royal Astronomical Society (2018) 480 (2011-2030) DOI: 10.1093/mnras/sty1999)

Our paper 'The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicksi was published in MNRAS 480, p2011-2030 (2018). After publication, we found a bug in the script we used to produce Table 2 and Fig. 15. For this reason, Section 3.5 in the manuscript needs to be amended and some of the considerations in the Conclusions (in Section 4) must be updated. Nevertheless, the main conclusions presented in the published article are not affected by the bug. In the following, we list the changes with respect to the published version of the paper. (i) Fig. 15 at page 18 should be replaced with the one reported in this Erratum. (ii) Table 2 at page 19 should be replaced with the one reported in this Erratum. (iii) The last paragraph in the second column of page 13 should be replaced by: Our estimate of Rloc,DNS spans from ∼5 Gpc-3 yr-1 (for a1) to ∼103 Gpc-3 yr-1 (for CC15α3 and CC15α5). The local merger rate density of BHNSs Rloc,BHNS spans from ∼10-2 to ∼103 Gpc-3 yr-1, while the local merger rate density of BHBs Rloc,BHB spans from ∼10-1 to ∼4 × 103 Gpc-3 yr-1.' (iv) The first paragraph in the first column of page 14 should be substituted by: The simulations with high core-collapse SN kicks (α1, α3 and α5) are not consistent with the local merger rate density of DNSs inferred from GW170817 (Abbott et al. 2017b). In contrast, the simulations with low core-collapse SN kicks and α ≥ 3 (CC15α3 and CC15α3) are fairly consistent with the local merger rate of DNSs inferred from GW170817. Model 2 applied to CC15α5 gives an estimate of the local merger rate density of DNSs which is in good agreement with the value inferred from GW170817.' (v) In the first column of page 14, the last three lines of the third paragraph change to: [...] whereas model 2 predicts Rloc,BHB ∼ 40 - 90 Gpc-3 yr-1, which is perfectly within the LIGO-Virgo 90 per cent credible interval.' (vi) Finally, the last paragraph of Section 4 (page 18) should be replaced by: Table 2. Local merger rate density. (Table Presented). In contrast, the local merger rate density of DNSs strongly depends on both CE parameters and SN kicks (Fig. 15). Only simulations with lowSNkicks and high values of a (CC15a3 and CC15a5) match the local merger rate density inferred from GW170817 (Rloc,DNS = 1540+3200 -1220 Gpc-3 yr-1, Abbott et al. 2017b). This result adds another piece to the intricate puzzle of natal kicks and DNS formation.' We apologize for the inconvenience. (Figure Presented).