| Issue |
A&A
Volume 648, April 2021
|
|
|---|---|---|
| Article Number | C2 | |
| Number of page(s) | 2 | |
| Section | Extragalactic astronomy | |
| DOI | https://doi.org/10.1051/0004-6361/201834565e | |
| Published online | 19 April 2021 | |
Exploring He II λ1640 emission line properties at z ∼ 2−4 (Corrigendum)
1
Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
e-mail: themiyananayakkara@gmail.com
2
Instituto de Astrofisica e Ciencias do Espaco, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
3
ETH Zurich, Department of Physics, HIT J31.5, Wolfgang-Pauli-Strasse 27, 8093 Zurich, Switzerland
4
Univ. Lyon, Univ. Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon (CRAL) UMR 5574, 69230 Saint-Genis-Laval, France
5
Scuola Internazionale Superiore di Studi Avanzati (SISSA), Via Bonomea 265, 34136 Trieste, Italy
6
Institut für Astrophysik, Universität Göttingen, Friedrich-Hund Platz 1, 37077 Göttingen, Germany
7
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Versoix, Switzerland
Key words: galaxies: ISM / galaxies: star formation / galaxies: evolution / galaxies: high-redshift / errata, addenda
Due to an error introduced to the equivalent width measuring code during the refereeing process, the final published equivalent widths (EWs) were artificially elevated. Table 3 and Fig. 10 have been updated with the correct values. The He II λ1640 EW values still show an enhancement compared to the values predicted by the models. Our final conclusions therefore remain unchanged due to this update.
EWs of the MUSE He II λ1640 sample used in this analysis.
 |
Fig. 10.
EW comparison of the MUSE He II λ1640 sample using BPASS stellar population models. Left: C III]λ1907+C III]λ1909 EW vs. He II λ1640 EW. Right: O III]λ1666 EW vs. He II λ1640 EW. Galaxies with S/N ≥ 2.5 are shown by stars, and others are shown as lower limits to the EW as triangles. We compare our observed EWs with model tracks from the Xiao et al. (2018) BPASS binary tracks. Models were computed for a log10(nH) = 1.0 and Us = −1.5 at different metallicities between 2 Z⊙ to 1/200th Z⊙. The size of the symbols increases with time. EWs from the literature are also shown for comparison. |
References
- Xiao, L., Stanway, E. R., & Eldridge, J. J. 2018, MNRAS, 477, 904 [Google Scholar]
© ESO 2021
All Tables
All Figures
|
Fig. 10.
EW comparison of the MUSE He II λ1640 sample using BPASS stellar population models. Left: C III]λ1907+C III]λ1909 EW vs. He II λ1640 EW. Right: O III]λ1666 EW vs. He II λ1640 EW. Galaxies with S/N ≥ 2.5 are shown by stars, and others are shown as lower limits to the EW as triangles. We compare our observed EWs with model tracks from the Xiao et al. (2018) BPASS binary tracks. Models were computed for a log10(nH) = 1.0 and Us = −1.5 at different metallicities between 2 Z⊙ to 1/200th Z⊙. The size of the symbols increases with time. EWs from the literature are also shown for comparison. |
| In the text | |
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