tokens: The photometric and log g pairs and final adopted , log g , ξ , and v sin i of the stars are tabulated in Table 2 . Figure 1. Comparison between the observed (black points) and synthetic (colored solid lines) H β profiles of the stars for the adopted atmospheric parameters given in Table 2 . Figure 2. Determination of the microturbulences by minimizing the standard deviation of . Table 2 Derived Atmospheric Parameters and Rotational Velocities of the Stars Notes. a The data are from Paunzen ( 2015 ) for HD 23193, and Hauck Mermilliod ( 1998 ) for HD 170920. b The data are from Hauck Curchod ( 1980 ). c The data are from Høg et al. ( 2000 ). d E ( B−V ) = 0.07 for HD 170920. 3.2. Chemical Abundances from Spectrum Synthesis For the spectrum synthesis, we used the atomic line list of Kılıçoğlu et al. ( 2016 ) compiled from Kurucz’s Line Database, 4 4 http://kurucz.harvard.edu/linelists/gfhyperall/gfhyperall.dat VALD (Piskunov et al. 1995 ; Ryabchikova et al. 1997 ; Kupka et al. 1999 , 2000 ), the NIST atomic database (Kramida et al. 2015 ), and various available sources of the oscillator strengths. We initially selected unblended (or slightly blended) lines of the elements (141 lines for HD 23193, 281 lines for HD 170920) in the high-resolution spectra of the stars. We then fitted these selected lines with synthetic line profiles produced by SYNSPEC49 and its SYNPLOT interface. The code was modified to minimize the between the model and the observed points, using the Levenberg–Marquardt algorithm (Markwardt 2009 ). The abundances of the elements were adjusted until the best-fit between the synthetic and observed line profiles. The synthetic spectra were broadened by the rotational velocity, microturbulence, and instrumental profile. We computed the ATLAS9 model atmosphere to derive the abundances of both stars. For the chemically peculiar Am star HD 23193, we also computed an ATLAS12 (Kurucz 2005 ) model atmosphere based on the derived abundances with ATLAS9, and refined its elemental abundances. 4. Evolutionary Status Using the effective temperatures (derived in this study) and the luminosities (calculated from the parameters given in Table 3 ), we plotted the target stars on a theoretical HR diagram (Figure 3 ). We used the evolutionary tracks having various masses (i.e., 2.2, 3.0 M ⊙ ) and solar metallicity to estimate the masses of the stars (Salasnich et al. 2000 ). For their ages, we considered the isochrones with various ages (i.e., 430, 530, 600, and 665 Myr) and solar metallicity (Bressan et al. 2012 ). We found a mass of 2.3 ± 0.1 M ⊙ for HD 23193, and 2.9 ± 0.1 M ⊙ for HD 170920. The estimated age of HD 23193 is 635 ± 33 Myr, and the age of HD 170920 is 480 ± 50 Myr. Figure 3. Location of the stars on the HR diagram. Table 3 Calculated Parameters of the Stars for the H-R Diagram Note. , π , and BC are from Høg et al. ( 2000 ), van Leeuwen ( 2007 ), and Torres ( 2010 ), respectively. As shown in Figure 3 , the age (635 ± 33 Myr)
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