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Stellar population astrophysics (SPA) with the TNG : Identification of a sulphur line at λair = 1063.6 nm in GIANO-B stellar spectra

Ryde, N. LU orcid ; Hartman, Henrik LU orcid ; Oliva, E. ; Origlia, L. ; Sanna, N. ; Rainer, M. ; Thorsbro, B. LU orcid ; Dalessandro, E. and Bono, G. (2019) In Astronomy and Astrophysics 631.
Abstract

Context. In the advent of new infrared high-resolution spectrometers, accurate and precise atomic data in the infrared are urgently needed. Identifications, wavelengths, strengths, broadening, and hyper-fine splitting parameters of stellar lines in the near-infrared are in many cases not accurate enough to model observed spectra, and in other cases, these parameters do not even exist. Some stellar features are unidentified. Aims. The aim with this work is to identify a spectral feature at λvac = 1063.891 nm or λair = 1063.600 nm that is visible in spectra of stars of different spectral types that are observed with the GIANO-B spectrometer. Methods. The search for spectral lines to match the unidentified feature in... (More)

Context. In the advent of new infrared high-resolution spectrometers, accurate and precise atomic data in the infrared are urgently needed. Identifications, wavelengths, strengths, broadening, and hyper-fine splitting parameters of stellar lines in the near-infrared are in many cases not accurate enough to model observed spectra, and in other cases, these parameters do not even exist. Some stellar features are unidentified. Aims. The aim with this work is to identify a spectral feature at λvac = 1063.891 nm or λair = 1063.600 nm that is visible in spectra of stars of different spectral types that are observed with the GIANO-B spectrometer. Methods. The search for spectral lines to match the unidentified feature in line lists from standard atomic databases was not successful. However, by investigating the original published laboratory data, we were able to identify the feature and solve the problem. To confirm its identification, we modelled the presumed stellar line in the solar intensity spectrum and found an excellent match. Results. We find that the observed spectral feature is a stellar line originating from the 4s′-4p′ transition in S I, and that the reason for its absence in atomic line databases is a neglected air-to-vacuum correction in the original laboratory measurements from 1967 for this line only. From interpolation we determine the laboratory wavelength of the S I line to be λvac = 1063.8908 nm or λair = 1063.5993 nm, and the excitation energy of the upper level to be 9.74978 eV.

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organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
Atomic data, Infrared: Stars, Instrumentation: Spectrographs, Line: Identification, Methods: Laboratory: Atomic, Techniques: Spectroscopic
in
Astronomy and Astrophysics
volume
631
article number
L3
publisher
EDP Sciences
external identifiers
  • scopus:85074457969
ISSN
0004-6361
DOI
10.1051/0004-6361/201936594
language
English
LU publication?
yes
id
2e7be79c-3712-4fe3-b912-bcb6b21ed25d
date added to LUP
2019-11-18 14:53:58
date last changed
2024-04-16 23:34:46
@article{2e7be79c-3712-4fe3-b912-bcb6b21ed25d,
  abstract     = {{<p>Context. In the advent of new infrared high-resolution spectrometers, accurate and precise atomic data in the infrared are urgently needed. Identifications, wavelengths, strengths, broadening, and hyper-fine splitting parameters of stellar lines in the near-infrared are in many cases not accurate enough to model observed spectra, and in other cases, these parameters do not even exist. Some stellar features are unidentified. Aims. The aim with this work is to identify a spectral feature at λ<sub>vac</sub> = 1063.891 nm or λ<sub>air</sub> = 1063.600 nm that is visible in spectra of stars of different spectral types that are observed with the GIANO-B spectrometer. Methods. The search for spectral lines to match the unidentified feature in line lists from standard atomic databases was not successful. However, by investigating the original published laboratory data, we were able to identify the feature and solve the problem. To confirm its identification, we modelled the presumed stellar line in the solar intensity spectrum and found an excellent match. Results. We find that the observed spectral feature is a stellar line originating from the 4s′-4p′ transition in S I, and that the reason for its absence in atomic line databases is a neglected air-to-vacuum correction in the original laboratory measurements from 1967 for this line only. From interpolation we determine the laboratory wavelength of the S I line to be λ<sub>vac</sub> = 1063.8908 nm or λ<sub>air</sub> = 1063.5993 nm, and the excitation energy of the upper level to be 9.74978 eV.</p>}},
  author       = {{Ryde, N. and Hartman, Henrik and Oliva, E. and Origlia, L. and Sanna, N. and Rainer, M. and Thorsbro, B. and Dalessandro, E. and Bono, G.}},
  issn         = {{0004-6361}},
  keywords     = {{Atomic data; Infrared: Stars; Instrumentation: Spectrographs; Line: Identification; Methods: Laboratory: Atomic; Techniques: Spectroscopic}},
  language     = {{eng}},
  month        = {{11}},
  publisher    = {{EDP Sciences}},
  series       = {{Astronomy and Astrophysics}},
  title        = {{Stellar population astrophysics (SPA) with the TNG : Identification of a sulphur line at λ<sub>air</sub> = 1063.6 nm in GIANO-B stellar spectra}},
  url          = {{http://dx.doi.org/10.1051/0004-6361/201936594}},
  doi          = {{10.1051/0004-6361/201936594}},
  volume       = {{631}},
  year         = {{2019}},
}