Notes. ΔT_eff in kK; Δlog g in dex; Δv_mic in km s⁻¹. Bold faced numbers are upper limits.

EWs – equivalent width measurements; LPF – line profile fitting; LDR – line depth ratio; (a) – The numbers given in this column may be lower than the total number of stars investigated in the corresponding work (for more information see Section 3). (b) – In O and very early B-type stars, this spectral line is very sensitive to v_mic (Lyubimkov, Rostopchin, Lambert 2004; Markova et al. 2020). (c) – NLTE effects taken into account. CLW06=Crowther, Lennon and Walborn (2006); MPL18=Markova et al. (2018); MP08=Markova & Puls (2008); markova08=Markova et al. (2008); LPA07=Lefever et al. (2007); McE99=McE99; FP12=Firnstein & Przybilla (2012); TT95=Takeda & Takada-Hidai (1995); neg15=Negueruela et al (2015); N15=Niemczura et al. (2015); N17=Niemczura et al. (2017); Kah16=Kahraman et al. (2016); T07=Trundle et al. (2007); H07=Hunter et al (2007); H09=Hunter et al. (2009); Mor06=Morel etal. (2006); Mor08=Morel, Hubrig, Briquet (2008); PNB08=Przybilla, Nieva & Butler (2008); NS11=Nieva & Simon-Diaz (2011); NP12=Nieva & Przybilla (2012); K91=Kilian et al. (1991); K94a=Kilian (1994); K94b=Kilian et al. (1994); GFP97=Giridhar, Ferro & Parrao (1997)