A list of tantalum lines for the wavelength calibration of the Hamilton echelle spectrograph

Pakhomov, Yu. V.

doi:10.1134/s1063772915100054

Cited by 3 publications

(1 citation statement)

References 6 publications

(9 reference statements)

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“…A precise wavelength calibration is required to correctly perform the spectral averaging. We used a wavelength solution of the TaTh-Ar hollow cathode lamp (Pakhomov 2015) for the observations taken in 2011 March and the Ti-Ar lamp (Pakhomov & Zhao 2013) for the observations of 2012.…”

Section: Stellar Sample Observations and Atmospheric Parametersmentioning

confidence: 99%

SYSTEMATIC NON-LTE STUDY OF THE −2.6 ≤ [Fe/H] ≤ 0.2 F AND G DWARFS IN THE SOLAR NEIGHBORHOOD. II. ABUNDANCE PATTERNS FROM Li TO Eu*

Zhao

Mashonkina

Yan

et al. 2016

ApJ

142

158

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For the first time, we present an extensive study of stars with individual non-LTE (NLTE) abundances for 17 chemical elements from Li to Eu in a sample of stars uniformly distributed over the −2.62 [Fe/H] +0.24 metallicity range that is suitable for the Galactic chemical evolution research. The star sample has been kinematically selected to trace the Galactic thin and thick disks and halo. We find new results and improve earlier ones as follows: (i) the element-to-iron ratios for Mg, Si, Ca, and Ti form a metal-poor (MP) plateau at a similar height of 0.3 dex, and the knee occurs at common

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Section: Stellar Sample Observations and Atmospheric Parametersmentioning

confidence: 99%

SYSTEMATIC NON-LTE STUDY OF THE −2.6 ≤ [Fe/H] ≤ 0.2 F AND G DWARFS IN THE SOLAR NEIGHBORHOOD. II. ABUNDANCE PATTERNS FROM Li TO Eu*

Zhao

Mashonkina

Yan

et al. 2016

ApJ

142

158

View full text Add to dashboard Cite

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VALD in Astrophysics

Pakhomov

Ryabchikova

2022

Communications in Computer and Information Science

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Automatic Échelle Spectrograph Wavelength Calibration

Brandt

McCully

2020

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Time-domain astronomy and the increasing number of exoplanet candidates call for reliable, robust, and automatic wavelength calibration. We present an algorithm for wavelength-calibrating échelle spectrographs that uses order-by-order extracted spectra and a list of laboratory wavelengths. Our approach is fully automatic and does not need the pixel locations of certain spectral features with which to anchor the wavelength solution, nor the true order number of each diffraction order. We use spectral features that are duplicated in adjacent orders to establish the scale-invariant component of the wavelength solution. We then match the central wavelengths of spectral features to laboratory wavelengths to establish the scale and higher-order components of the wavelength solution. We demonstrate our method on the four spectrographs of Las Cumbres Observatory’s Network of Robotic Échelle Spectrographs (NRES), on the High Accuracy Radial Velocity Planet Searcher (HARPS) spectrograph, and on synthetic data. We obtain a velocity-equivalent precision of ∼10 m s−1 on NRES. We achieve ∼1 m s−1 on HARPS, which agrees with the precision reported by the HARPS team. On synthetic data, we achieve the velocity precision set by Gaussian centroiding errors. Our algorithm likely holds for a wide range of spectrographs beyond the five presented here. We provide an open-source Python package, xwavecal, which outputs wavelength-calibrated spectra as well as the wavelengths of spectral features.

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A list of tantalum lines for the wavelength calibration of the Hamilton echelle spectrograph

Cited by 3 publications

References 6 publications

SYSTEMATIC NON-LTE STUDY OF THE −2.6 ≤ [Fe/H] ≤ 0.2 F AND G DWARFS IN THE SOLAR NEIGHBORHOOD. II. ABUNDANCE PATTERNS FROM Li TO Eu*

SYSTEMATIC NON-LTE STUDY OF THE −2.6 ≤ [Fe/H] ≤ 0.2 F AND G DWARFS IN THE SOLAR NEIGHBORHOOD. II. ABUNDANCE PATTERNS FROM Li TO Eu*

VALD in Astrophysics

Automatic Échelle Spectrograph Wavelength Calibration

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