Based on a collection of high-dispersion spectra obtained at Okayama Astrophysical Observatory, the atmospheric parameters ($T_{\mathrm{eff}}, \log g, v_{\mathrm{t}}$, and $\mathrm{[Fe/H]}$) of 160 mid-F through early-K stars were extensively determined by the spectroscopic method using the equivalent widths of Fe I and Fe II lines along with the numerical technique of Takeda et al. (2002, PASJ, 54, 451). The results are comprehensively discussed and compared with the parameter values derived by different approaches (e.g., photometric colors, theoretical evolutionary tracks, Hipparcos parallaxes, etc.) as well as with the published values found in various literature. It has been confirmed that our purely spectroscopic approach yields fairly reliable and consistent results.

A computer program has been developed for determining the fundamental model atmosphere parameters ($T_\mathrm{eff}$, $\log g$, $v_\mathrm{t}$, $[\mathrm{Fe/H}]$) of solar-type stars, which is based on the equivalent widths for a well-chosen set of Fe i and Fe ii lines. The basic principle of this method is to find the solution in the $(T_\mathrm{eff}$, $\log g$, $v_\mathrm{t})$ space, which minimizes the sum of the dispersion of the Fe i abundances and the square of the Fe i–Fe ii abundance difference. An application of this code to the observed solar equivalent widths turned out to yield satisfactory results, which are more or less consistent with the actual parameters of the Sun. The numerical performance of this approach as well as the errors involved in the resulting solutions are discussed.

High $\mathrm{S/N}$ ratio (350–600) and high resolution ($R \sim 90000$) spectral data covering the wavelength region between 4200–8800$\,{Å}$ were obtained for 12 planet-harboring stars with the SUBARU/HDS. Detailed abundance analyses were carried out for these stars using the solar spectrum as a reference. Atmospheric parameters ($T_\mathrm{eff}, \log g$, microturbulent velocity $\xi_\mathrm{t}$, and $[\mathrm{Fe/H}]$) were determined spectroscopically using selected Fe I and Fe II lines. The abundances of 25 other elements have been determined relative to the Sun in a strictly differential manner. Three out of 12 stars (HD 82943, HD 92788, and HD 134987) are definitely metal rich, and two stars (HD 114762 and HD 190228) are metal deficient. The abundances in the remaining seven stars (HD 106252, HD 130322, HD 141937, HD 168746, HD 187123, HD 192263, HD 209458) coincide with the Sun. We find that the abundances of both volatile and refractory elements behave similarly in these stars, and do not confirm any significant dependence on the condensation temperature, $T_\mathrm{c}$. Comparisons of the $[\mathrm{X/Fe}]$ vs $[\mathrm{Fe/H}]$ relations for 19 elements between planet-harboring stars and nearby field stars reveal no distinct anomaly, except for possible enhancements of V and Co in the former group. These results suggest that the observed over-abundances of metallic elements in planet-harboring stars relative to normal disk stars in the solar neighborhood are primordial, and can be interpreted as being a consequence of the galactic chemical evolution.

In this open-label study, IVCYC improved symptoms, pulmonary function tests and HRCT findings in patients with PM/DM. Longitudinal controlled studies are required to further confirm the efficacy of IVCYC.