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tokens: the CH features and C i lines in metal-poor dwarfs with [Fe/H] –3.0 (see Fabbian et al. 2009 ; Jacobson Frebel 2015 ; Placco et al. 2016a ), in what follows we shall assume that this correction is not well-determined below [Fe/H] ≲ −3.0, and make the conservative assumption that A (C i ) 3D,NLTE – A (CH) 3D,LTE = 0.0, for all [Fe/H], and hence A (CH) 3D,NLTE = A (CH) 3D,LTE . The reader should bear in mind that the 3D,NLTE corrections we shall present in what follows are most likely less extreme than would be obtained by adoption of the equation in the previous paragraph. 4. Revised <italic>A</italic>(C) versus [Fe/H] and [C/Fe] versus [Fe/H] Diagrams 4.1. The Yoon et al. (<xref ref-type="bibr" rid="apjab1f84bib113">2016</xref>) Sample of CEMP Stars With the 3D–1D and NLTE–LTE corrections in hand, we now investigate their effect on the distribution of the CEMP-no stars in the ( A (C), [Fe/H]) and ([C/Fe], [Fe/H]) planes. Figure 4 presents the data for the CEMP-no and CEMP-s objects compiled by Yoon et al. ( 2016 ), 7 7 We used only stars in the Yoon et al. ( 2016 ) catalog for which the [C/Fe] values were based on the CH G -band. While this does not affect the CEMP-no stars, it excludes some 15 CEMP-s objects. We also required the presence of [Ba/Fe] to identify membership of the CEMP-no and CEMP-s subclasses, except for stars with [Fe/H] −3.3, where in the absence of detected [Ba/Fe] we assume CEMP-no status. together with those for an additional recently reported eight CEMP-no stars presented in Table 4 , and four stars identified in Table 6 . The effects of the corrections to A (C), [C/Fe], and [Fe/H] are presented in the three rows of the figure. The uppermost row, panels (a) and (b), show data obtained using 1D,LTE for A (C) 1D,LTE and [C/Fe] 1D,LTE versus [Fe/H] 1D,LTE , respectively. Also shown in the top left panel (a) are the the ellipses containing the Groups I, II, and III of Yoon et al. ( 2016 ), together with the “high-carbon band” (horizontal orange line) and the “low-carbon band” (horizontal light blue line) of Spite et al. ( 2013 ), Bonifacio et al. ( 2015 , 2018 ), and Caffau et al. ( 2018 ) (truncated on the right by the [C/Fe] = +1.0 locus). 8 8 We draw the reader’s attention to the fact that the Yoon et al. ( 2016 ) model contains three components, while that of Caffau et al. ( 2018 ) has only two. The question one might ask is: how many components are required to best describe the stellar distribution? We shall discuss this further in Sections 7.1 and 8 . In these panels, (a) and (b), red and gray symbols refer to CEMP-no stars on the one hand, and CEMP-s stars on the other, and in what follows in the middle and bottom rows the symbol for each star will retain the same color as adopted in these uppermost panels. The full and dotted lines in all panels represent the loci of the [C/Fe] > +0.7 divide between C-normal and CEMP stars, and [C/Fe] = 0.0, respectively. Figure 4. Carbon vs. iron abundances for CEMP-no (red symbols)