ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength I-Wavelength I-Wavelength B-Wavelength O B-Wavelength I-Wavelength O O B-Wavelength O B-Wavelength I-Wavelength O O B-Wavelength B-Wavelength B-Wavelength B-Wavelength O B-Wavelength I-Wavelength O O O B-Wavelength O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Database I-Database I-Database I-Database O B-Database O B-Citation I-Citation I-Citation I-Citation O O O B-Dataset I-Dataset O B-Dataset O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O B-Person O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Person I-Person I-Person O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O B-Citation I-Citation I-Citation I-Citation O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O B-Database O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O B-CelestialRegion I-CelestialRegion O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O B-CelestialObject
tokens: during the first step and varied the abundances of the individual elements using the same masks. For a few elements, we extracted the lines of the particular element from the common masks and ran SME with these individual masks. The abundances of O, Sr, La, and Eu were derived from the spectral synthesis of individual lines not falling into the chosen SME spectral regions: the O i IR triplet λλ7771.94, 7774.16 and 7775.39 Å; Sr i λλ4607.33 and 7070.07 Å; La ii λλ5114.56, 5301.97, 5303.55, 5805.78 and 5808.32 Å; and Eu ii λλ6437.64 and 6645.11 Å. The carbon and nitrogen abundances were estimated by simultaneous fitting of the C 2 and CN molecular lines distributed in all regions covered by the SME analysis. The atomic parameters of the lines were extracted from the Vienna Atomic Line Database ( vald ; Kupka et al. 1999 ) using its 3rd release ( vald3 ; Ryabchikova et al. 2015 ). The atomic parameters for the C 2 and CN molecular lines were taken from Brooke et al. ( 2013 ) and the Kurucz's website (see below), respectively. The isotopic structure (IS) of Cu ii , Ba ii , and Eu ii was taken into account. For elements with odd isotopes the synthetic calculations included hyperfine splitting (hfs). Most of the data for isotopic and hyperfine splitting were obtained from the website of R. L. Kurucz, 2 who collected data and a bibliography for individual atomic species. In particular, the hyperfine structure constants for Na i were taken from Griffith et al. ( 1977 ), Tsekeris, Liao Gupta ( 1976 ), and Yei, Sieradzan Havey ( 1993 ); for Sc i and ii from Ertmer Hofer ( 1976 ) and Mansour et al. ( 1989 ); for V i from Childs et al. ( 1979 ), Palmeri et al. ( 1995 ), and Unkel et al. ( 1989 ); for Mn i, ii from Blackwell-Whitehead et al. ( 2005 ) and Holt, Scholl Rosner ( 1999 ); for Co i from Pickering ( 1996 ); for Cu i from Fischer, Hühnermann Kollath ( 1967 ) and Ney ( 1966 ); for Y i from Dinneen et al. ( 1991 ) and Villemoes et al. ( 1992 ); and for Ba i from Villemoes et al. ( 1993 ). All hfs data were collected in a new data base (Pakhomov et al. in preparation) and used by the internal vald programs for the hfs calculations. The average abundances for the final atmospheric model of TYC 8606-2025-1 are given in log (X/H) + 12 units in the second column of Table 3 . The third column of this table presents the current solar photospheric abundances (Asplund et al. 2009 ; Scott et al. 2015a , b ; Grevesse et al. 2015 ), while the fourth columns lists the elemental abundances derived for TYC 8606-2025-1 relative to the Sun. The last column of Table 3 provides information about different effects taken into account in the SME or spectral synthesis analyses. For clarity, the elemental abundances of TYC 8606-2025-1 relative to the Sun are shown in Fig. 2 , highlighting the overabundance of s-process elements, with the Ba abundance increased by a factor of ≈3 with respect to solar. Figure 2. Elemental abundances of TYC 8606-2025-1 relative to the Sun.