| Issue |
A&A
Volume 688, August 2024
|
|
|---|---|---|
| Article Number | C2 | |
| Number of page(s) | 1 | |
| Section | Galactic structure, stellar clusters and populations | |
| DOI | https://doi.org/10.1051/0004-6361/202450839e | |
| Published online | 12 August 2024 | |
Hunting young stars in the Galactic centre
Hundreds of thousands of solar masses of young stars in the Sagittarius C region (Corrigendum)
European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
e-mail: francisco.nogueraslara@eso.org
Key words: dust / extinction / HII regions / Galaxy: center / Galaxy: nucleus / Galaxy: structure / errata, addenda
We have detected an error in Fig. 7 of Nogueras-Lara (2024). The fraction of stellar mass corresponding to the central nuclear stellar disc (NSD), obtained by Nogueras-Lara et al. (2022), was erroneously multiplied by ten in the age bin between 0.06 and 0.5 Gyr in the figure. Additionally, the colours in the zoom-in panel were switched between the Sgr C and Sgr B1 regions. Figure 1 shows the corrected version.
 |
Fig. 1. Comparison between the stellar population present in the central region of the NSD, Sgr B1 (data extracted from Fig. 4 in Nogueras-Lara et al. 2022), and Sgr C (this work). The zoomed-in image shows the youngest age bin, where Sgr B1 and Sgr C show an excess of young stars in comparison to the central region of the NSD. |
References
- Nogueras-Lara, F. 2024, A&A, 681, L21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
- Nogueras-Lara, F., Schödel, R., & Neumayer, N. 2022, Nature Astronomy, 6, 1178 [NASA ADS] [CrossRef] [Google Scholar]
© The Authors 2024
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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All Figures
|
Fig. 1. Comparison between the stellar population present in the central region of the NSD, Sgr B1 (data extracted from Fig. 4 in Nogueras-Lara et al. 2022), and Sgr C (this work). The zoomed-in image shows the youngest age bin, where Sgr B1 and Sgr C show an excess of young stars in comparison to the central region of the NSD. |
| In the text | |
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