Identification of Absorption Lines of Heavy Metals in the Wavelength Range 0.97–1.32 μm

  title={Identification of Absorption Lines of Heavy Metals in the Wavelength Range 0.97–1.32 $\mu$m},
  author={Noriyuki Matsunaga and Daisuke Taniguchi and Mingjie Jian and Yuji Ikeda and Kei Fukue and Sohei Kondo and Satoshi Hamano and Hideyo Kawakita and Naoto Kobayashi and Shogo Otsubo and Hiroaki Sameshima and Keiichi Takenaka and Takuji Tsujimoto and Ayaka Watase and Chikako Yasui and Tomohiro Yoshikawa},
  journal={The Astrophysical Journal Supplement Series},
Stellar absorption lines of heavy elements can give us various insights into the chemical evolution of our Galaxy and other nearby galaxies. Recently developed spectrographs for the near-infrared wavelengths are becoming more and more powerful at producing a large number of high-quality spectra, but identification and characterization of the absorption lines in the infrared range remain to be fulfilled. We searched for lines of elements heavier than the iron group, i.e., those heavier than Ni… 

Absorption Lines in the 0.91–1.33 μm Spectra of Red Giants for Measuring Abundances of Mg, Si, Ca, Ti, Cr, and Ni

Red giants show a large number of absorption lines in both optical and near-infrared wavelengths. Still, the characteristics of the lines in different wave passbands are not necessarily the same. We

The effect of surface gravity on line-depth ratios in the wavelength range 0.97–1.32 µm

A line-depth ratio (LDR) of two spectral lines with different excitation potentials is expected to be correlated with the effective temperature (Teff). It is possible to determine Teff of a star

Line-depth ratios as indicators of effective temperature and surface gravity

The analysis of stellar spectra depends upon the effective temperature (Teff) and the surface gravity (log g). However, the estimation of log g with high accuracy is challenging. A classical approach

Effective temperatures of red supergiants estimated from line-depth ratios of iron lines in the YJ bands, 0.97-1.32μm

Determining the effective temperatures (Teff) of red supergiants (RSGs) observationally is important in many fields of stellar physics and galactic astronomy, yet some significant difficulties

Highly Sensitive, Non-cryogenic NIR High-resolution Spectrograph, WINERED

WINERED is a novel near-infrared (NIR) high-resolution spectrograph (HRS) that pursues the highest possible sensitivity to realize high-precision spectroscopy in the NIR as in the optical wavelength

The Galactic Distribution of Phosphorus: A Survey of 163 Disk and Halo Stars

Phosphorus (P) is a critical element for life on Earth, yet the cosmic production sites of P are relatively uncertain. To understand how P has evolved in the solar neighborhood, we measured



Fe i Lines in 0.91–1.33 μm Spectra of Red Giants for Measuring the Microturbulence and Metallicities

For a detailed analysis of stellar chemical abundances, high-resolution spectra in the optical have mainly been used, while the development of near-infrared (NIR) spectrograph has opened new

Line identification in high-resolution, near-infrared CRIRES spectra of chemically peculiar and Herbig Ae stars

Context. Contrary to the late-type stars, our knowledge of atomic transitions in intermediate-mass stars is still very poor. The recent availability of ESO’s high-resolution spectrograph CRIRES

WINERED High-resolution Near-infrared Line Catalog: A-type Star

We present a catalog of absorption lines in the z′, Y, and J bands that we identified in 21 Lyn, a slowly rotating A0.5 V star. We detected 155 absorption features in the high-resolution (0.90–1.35

Near-infrared spectroscopy of the Sun and HD 20010 - Compiling a new line list in the near-infrared

Context: Effective temperature, surface gravity, and metallicity are basic spectroscopic stellar parameters necessary to characterize a star or a planetary system. Reliable atmospheric parameters for

Chemical abundances of open clusters from high-resolution infrared spectra – II. NGC 752

We present a detailed near-infrared chemical abundance analysis of 10 red giant members of the Galactic open cluster NGC 752. High-resolution (R ≃ 45000) near-infrared spectral data were gathered

Correction of Near-infrared High-resolution Spectra for Telluric Absorption at 0.90–1.35 μm

We report a method of correcting a near-infrared (0.90–1.35 μm) high-resolution (λ/Δλ ∼ 28,000) spectrum for telluric absorption using the corresponding spectrum of a telluric standard star. The

Galactic abundance gradients from Cepheids - α and heavy elements in the outer disk

Context. Galactic abundance gradients set strong constraints to chemo-dynamical evolutionary models of the Milky Way. Given the period-luminosity relations that provide accurate distances and the

Neutron-Capture Elements in the Early Galaxy: Insights from a Large Sample of Metal-poor Giants

New abundances for neutron-capture (n-capture) elements in a large sample of metal-poor giants from the Bond survey are presented. The spectra were acquired with the KPNO 4 m echelle and coudé feed

GIANO-TNG spectroscopy of red supergiants in the young star cluster RSGC2

Aims. The inner disk of the Galaxy has a number of young star clusters dominated by red supergiants that are heavily obscured by dust extinction and observable only at infrared wavelengths. These

Method to estimate the effective temperatures of late-type giants using line-depth ratios in the wavelength range 0.97-1.32 μm

The effective temperature, one of the most fundamental atmospheric parameters of a star, can be estimated using various methods, and here we focus on the method using line-depth ratios (LDRs). This