Issue |
A&A
Volume 671, March 2023
|
|
---|---|---|
Article Number | A130 | |
Number of page(s) | 16 | |
Section | Catalogs and data | |
DOI | https://doi.org/10.1051/0004-6361/202244811 | |
Published online | 17 March 2023 |
Center-to-limb variation of spectral lines and continua observed with SST/CRISP and SST/CHROMIS★
1
Institute for Solar Physics, Dept. of Astronomy, Stockholm University, Albanova University Centre,
106 91
Stockholm,
Sweden
2
Leibniz-Institut für Astrophysik Potsdam (AIP),
An der Sternwarte 16,
14482
Potsdam,
Germany
e-mail: apietrow@aip.de
3
Observatoire de Genève, Université de Genève,
Chemin Pegasi 51,
1290
Sauverny,
Switzerland
4
Institute of Theoretical Astrophysics, University of Oslo,
PO Box 1029
Blindern,
0315
Oslo,
Norway
5
Rosseland Centre for Solar Physics, University of Oslo,
PO Box 1029
Blindern,
0315
Oslo,
Norway
Received:
25
August
2022
Accepted:
6
December
2022
Context. Observations of center-to-limb variations (CLVs) of spectral lines and continua provide a good test for the accuracy of models with a solar and stellar atmospheric structure and spectral line formation. They are also widely used to constrain elemental abundances, and are becoming increasingly more important in atmospheric studies of exoplanets. However, only a few such data sets exist for chromospheric lines.
Aims. We aim to create a set of standard profiles by means of mosaics made with the CRISP and CHROMIS instruments of the Swedish 1-m Solar Telescope (SST), as well as to explore the robustness of said profiles obtained using this method.
Methods. For each spectral line, we used a mosaic that ranges from the center to the limb. Each of these mosaics were averaged down to 50 individual spectral profiles and spaced by 0.02 in the μ scale. These profiles were corrected for p-mode oscillations, and their line parameters (equivalent width, line shift, full-width at half-maximum, and line depth) were then compared against literature values whenever possible.
Results. We present a set of 50 average profiles that are spaced equidistantly along the cosine of the heliocentric angle (μ) by steps of 0.02 for five continuum points between 4001 and 7772 Å, as well as ten of the most commonly observed spectral lines at the SST (Ca II H & K, Ηβ, Mg I 5173 Å, C I 5380 Å, Fe I 6173 Å, Fe I 6301 Å, Ha, O I 7772 Å, and Ca II 8542 Å).
Conclusions. The CLV of line profiles and continua are shared in the CDS as machine readable tables, providing a quantitative constraint on theoretical models that aim to model stellar atmospheres.
Key words: methods: observational / line: formation / Sun: photosphere / Sun: chromosphere / Sun: atmosphere
CLV profiles are also available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/671/A130
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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