Stellar population astrophysics (SPA) with the TNG
| العنوان: | Stellar population astrophysics (SPA) with the TNG |
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| المؤلفون: | Emanuele Dalessandro, Monica Rainer, Nicoletta Sanna, Livia Origlia, Ernesto Oliva, Giuseppe Bono, Nils Ryde, Henrik Hartman, B. Thorsbro |
| المصدر: | Astronomy & Astrophysics. 631:L3 |
| بيانات النشر: | EDP Sciences, 2019. |
| سنة النشر: | 2019 |
| مصطلحات موضوعية: | Physics, 010504 meteorology & atmospheric sciences, Stellar population, Spectrometer, Astronomy and Astrophysics, Context (language use), Astrophysics, Stellar classification, 01 natural sciences, Spectral line, Astronomical spectroscopy, Stars, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation) |
| الوصف: | 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. |
| تدمد: | 1432-0746 0004-6361 |
| الوصول الحر: | https://explore.openaire.eu/search/publication?articleId=doi_________::3ad8434a42963ccb557d5a7cb1097c72Test https://doi.org/10.1051/0004-6361/201936594Test |
| حقوق: | OPEN |
| رقم الانضمام: | edsair.doi...........3ad8434a42963ccb557d5a7cb1097c72 |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 14320746 00046361 |
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