High Dispersion Spectrograph (HDS) for the Subaru Telescope

By K. Noguchi, Wak Aoki, S. Kawanomoto, H. Ando, Satoshi Honda, H. Izumiura, E. Kambe, K. Okita, K. Sadakane, Bun'ei Sato and 5 more. 2002

298 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/1bcb9a5b1e93135a9a807a5108f68f03cb0bfa08

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Timothy C. Beers
2. A. Frebel
3. J. Norris
4. Wak Aoki
5. N. Christlieb
6. S. Ryan
7. Martin Asplund
8. Y. S. Lee

In Atomic and Molecular Physics, and Optics

1. Martin Asplund
2. P. Prugniel
3. Yue Wu
4. Timothy C. Beers
5. S. Wanajo
6. A. Frebel

In Instrumentation

1. Timothy C. Beers
2. A. Frebel
3. J. Norris
4. Y. S. Lee
5. Wak Aoki
6. Brian Yanny
7. Martin Asplund
8. C. Rockosi

Citations in the corpus

• Neutron-Capture Elements in the Very Metal Poor Star HD 122563 (2006, methodology): “In order to measure Ba lines at 5853 and 6141 8, a spectrum covering 5090–6410 8 was obtained during the HDS commissioning.”
• Spectroscopic Studies of Very Metal-poor Stars with the Subaru High Dispersion Spectrograph. III. Light Neutron-Capture Elements (2005, methodology): “The spectrum shift during one night is at most 0.5 pixel (0.45 km s 1), which corresponds to a temperature variation of 4 C (Noguchi et al. 2002), if the setup is not changed during the night.”
• Automatic determination of stellar atmospheric parameters and construction of stellar spectral templates of the Guoshoujing Telescope (LAMOST) (2011, methodology): “The high resolution spectra were obtained by Keck I/HIRES (Vogt et al. 1994), Keck II/ESI (Sheinis et al. 2002), VLT/UVES, HET/HRS (Ramsey et al. 1998; Tull 1998), and SUBARU/HDS (Noguchi et al. 2002); details about the methods for determining the parameters of these different spectra are described ”
• Carbon-enhanced Metal-poor Stars. I. Chemical Compositions of 26 Stars (2006, methodology): “We have thus far obtained spectra for 26 stars with the Subaru Telescope High Dispersion Spectrograph (Noguchi et al. 2002); we report on their chemical compositions in this paper.”
• Spectroscopic Studies of Extremely Metal-Poor Stars with the Subaru High Dispersion Spectrograph. II. The r-Process Elements, Including Thorium (2004, methodology): “In Honda et al. (2003; hereafter Paper I), we reported equivalent width measurements of absorption lines in high-quality spectra of 22 very metalpoor stars obtained with the Subaru Telescope High Dispersion Spectrograph (HDS; Noguchi et al. 2002).”
• CARBON-ENHANCED METAL-POOR STARS IN SDSS/SEGUE. I. CARBON ABUNDANCE ESTIMATION AND FREQUENCY OF CEMP STARS (2013, methodology): “The majority of the stars in Table 1 were analyzed by Aoki et al. (2008, 2013), who obtained high-dispersion (R ∼ 36,000) spectra with the Subaru Telescope High Dispersion Spectrograph (Noguchi et al. 2002).”
• HE 1327–2326, an Unevolved Star with [Fe/H] < –5.0. I. A Comprehensive Abundance Analysis (2005, result): “As has been reported by Frebel et al. (2005), spectra of the subgiant or dwarf HE 1327 2326 obtained with the Subaru Telescope High Dispersion Spectrograph (HDS; Noguchi et al. 2002) in 2004 May and June revealed that its Fe abundance is even lower than that of HE 0107 5240.”
• HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS FROM SDSS/SEGUE. I. ATMOSPHERIC PARAMETERS AND CHEMICAL COMPOSITIONS (2012, methodology): “Observations and Data Reduction Acceptable quality high-resolution snapshot spectra for 137 of the original 143 target stars selected above were obtained with the Subaru Telescope High Dispersion Spectrograph (HDS: Noguchi et al. 2002) in four observing runs in 2008 (March, May, July, and October).”
• Ground-based detection of sodium in the transmission spectrum of exoplanet HD209458b (2008, methodology): “HD209458 was observed on the night of October 24, 2002, using the High Dispersion Spectrograph (HDS; Noguchi et al. 2002) on the Subaru telescope.”