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# The formation of the Milky Way halo and its dwarf satellites; a NLTE-1D abundance analysis

L. Mashonkina, P. Jablonka, T. Sitnova, Yu. Pakhomov, P. North

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L. Mashonkina, P. Jablonka, T. Sitnova, Yu. Pakhomov, P. North. The formation of the Milky Way halo and its dwarf satellites; a NLTE-1D abundance analysis. Astronomy and Astrophysics - A&A, 2021, 650, pp.C1. 10.1051/0004-6361/201731582e. hal-03532459

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Submitted on 18 Jan 2022

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# The formation of the Milky Way halo and its dwarf satellites; a NLTE-1D abundance analysis

## II. Early chemical enrichment
(Corrigendum)

L. Mashonkina<fnref n="1" />,<fnref n="2" />✉, P. Jablonka<fnref n="3" />,<fnref n="4" />✉, T. Sitnova<fnref n="2" />✉, Yu. Pakhomov<fnref n="2" />, and P. North<fnref n="3" />✉

A&A, 608, A89 (2017), https://doi.org/10.1051/0004-6361/201731582

**Key words.** line: formation – nuclear reactions, nucleosynthesis, abundances – stars: abundances – stars: atmospheres – galaxies: abundances – errata, addenda

In Figs. 1 and 2, we present the corrected versions of Figs. 5 and 6 from Mashonkina et al. (2017). Compared with the original paper, the changes only concern including the X-axis in the bottom panels of the figures.

## References

Mashonkina, L., Jablonka, P., Sitnova, T., Pakhomov, Y., & North, P. 2017, A&A, 608, A89

<figure><img src="image_3.png" /><figcaption>**Fig. 1.** Stellar [Na/Mg] and [Al/Mg] LTE (**left column**) and NLTE (**right column**) abundance ratios in Sculptor (red circles), Ursa Minor (green circles), Sextans (squares), Fornax (rhombi), Boötes I (triangles), UMa II (inverted triangles), and Leo IV (five-pointed star) dSphs and the MW halo (black circles). The NLTE ratio [Na/Mg] = 0.68 for Sex 24–72 is not shown.</figcaption></figure>

<footnote n="1">¹ Universitäts-Sternwarte München, Scheinerstr. 1, 81679 München, Germany
e-mail: lyuda@usm.lmu.de</footnote>

<footnote n="2">² Institute of Astronomy, Russian Academy of Sciences, 119017 Moscow, Russia
e-mail: lima@inasan.ru</footnote>

<footnote n="3">³ Laboratoire d'Astrophysique, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland</footnote>

<footnote n="4">⁴ GEPI, Observatoire de Paris, CNRS, Université Paris Diderot, 92125 Meudon Cedex, France</footnote>
<figure><img src="image_4.png" /><figcaption>**Fig. 2.** *Left column:* [Sr/Fe] and [Ba/Fe] NLTE abundance ratios as a function of metallicity for our sample stars. *Right column:* [Sr/Mg] and [Ba/Mg] NLTE abundance ratios as a function of Mg abundance. Symbols and colours are the same as in Fig. 1. Upper limits in the Ba and Sr abundances are indicated with arrows.</figcaption></figure>