Notes. The table gives all binary candidates among the WN stars in the BAT99 catalog (excluding BAT99 118, see text for details). The columns are from left to right: BAT99 catalog number, reference, aliases, spectral types, and Smith visual magnitudes. In columns 6–10, we list X-ray luminosities, whether the systems show the presence of two or more components in their spectra (composite), and whether they are eclipsing (wind or photospheric), significantly RV variable (cf. FMG2003, S2008), and periodically RV variable. The final column shows the suggested configuration based on this study and previous studies. Bolded entries correspond to objects that are confirmed in this work as binary or multiple. Entries taken from references in Col. 2, with the exception unless otherwise noted with a footmark. Colons stand for uncertain entries. ^(a)Taken from Guerrero & Chu (2008a,b), except for BAT99 6, which is derived in this work. ^(f)Not confirmed by our study. ^(g)Reported by FMG03, but reported as undetected by Guerrero & Chu (2008a). ^(h)A single faint eclipse is obtained with the period P = 5.2 d, unequal to the spectroscopically derived period (2.3 d). ⁽ⁱ⁾Uncertain, possibly single. ^(j)Revised from WN4b to WC4 in our study. ^(p)A potential detection was reported by Townsley et al. (2006) but was not confirmed by Guerrero & Chu (2008a). ^(s)Periodic RV variability for WR star; better data needed to confirm periodicity of OB-type companion. ^(t)Spectral types adopted from Neugent et al. (2018), unless otherwise stated.

References.^(b)Niemela et al. (2001), Koenigsberger et al. (2003). ^(c)This study. ^(d)S2008. ^(e)FMG03. ^(k)Crowther & Walborn (2011). ^(l)Taylor et al. (2011). ^(m)Schnurr et al. (2009). ⁽ⁿ⁾Crowther et al. (2016). ^(o)Pollock et al. (2018), Tehrani et al. (2019). ^(q)Shenar et al. (2017). ^(r)Foellmi et al. (2006).