tokens: (bottom) lines represent the synthetic spectra for assumed 12 C/ 13 C ratios. The red line is the best matching synthesis to the observed spectrum. Assumed 12 C/ 13 C ratios are also given in the panels. 4. Abundances from IGRINS Near-infrared Spectra High-resolution, high-S/N H - and K -band spectra of RHB stars reveal a rich assortment of atomic and molecular features (Figure 3 ). Having this opportunity, we were able to compute the abundances of 21 species of 20 elements along with 12 C/ 13 C ratios. For our three RHB stars, abundances of P, S, and K were obtained for the first time. All abundances and 12 C/ 13 C ratios were derived by applying the SYN method to the observed spectra. The atomic and molecular data used for abundance calculations and the analyses of all species are discussed in the following subsections. In all cases the individual line abundances are given in Table 3 and the abundance summaries for the stars are given in Tables 4 – 6 . 4.1. Atomic and Molecular Data We adopted the molecular data described in Afşar16 (and references therein) for CN, CO, and OH features and generated the atomic line list (Table 3 ) following a similar procedure to that of Afşar16 . We used the Arcturus infrared atlas (Hinkle et al. 1995 ) 10 10 Available at ftp://ftp.noao.edu/catalogs/arcturusatlas/ . along with atomic line lists from the National Institute of Standards and Technology (NIST) Atomic Spectra Database 11 11 https://physics.nist.gov/PhysRefData/ASD/lines_form.html and from the Kurucz ( 2011 ) database 12 12 http://kurucz.harvard.edu/linelists.html to identify promising atomic lines in our RHB stars. Accurate transition probability information for the atomic and molecular data is essential for a robust abundance analysis. For lines that have NIST transition probabilities rated A and B accuracy (uncertainty ≤10%), we adopted the NIST log gf values. However, laboratory transition probabilities for most of the species transitions in the IR are lacking. Therefore, we had to apply reverse solar analyses to determine the “astrophysical” log gf values of mostly neutral species of elements listed in Table 3 . Only a few ionized species could be identified (see Section 3.2 ), and among them we only applied reverse solar analysis to Yb ii . The transition probabilities ranked as C (accuracies 20%) in the NIST database were needed to be justified in most of the cases with their own reverse solar analyses. The sources of all transition probabilities are provided in Table 3 . For the reverse solar analyses we used the high-resolution infrared solar flux spectrum of Wallace Livingston ( 2003 ) and adopted the solar model atmosphere of ASF12 . The derived transition probabilities then were tested on the Arcturus atlas spectra (Hinkle et al. 1995 ), adopting the Arcturus abundances and model atmospheric parameters from Ramírez Allende Prieto ( 2011 ). Satisfactory agreement with the abundances derived by Ramírez Allende Prieto was achieved for
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