TOPoS

VI. The metal-weak tail of the metallicity distribution functions of the Milky Way and the Gaia-Sausage-Enceladus structure*
(Corrigendum)

P. Bonifacio<fnref n="1" />, L. Monaco<fnref n="2" />, S. Salvadori<fnref n="3" />,<fnref n="4" />, E. Caffau<fnref n="1" />, M. Spite<fnref n="1" />, L. Sbordone<fnref n="5" />, F. Spite<fnref n="1" />, H.-G. Ludwig<fnref n="6" />,
P. Di Matteo<fnref n="1" />, M. Haywood<fnref n="1" />, P. François<fnref n="1" />,<fnref n="7" />, A. J. Koch-Hansen<fnref n="8" />, N. Christlieb<fnref n="6" />, and S. Zaggia<fnref n="9" />

A&A, 651, A79 (2021), https://doi.org/10.1051/0004-6361/202140816

**Key words.** stars: Population II – stars: abundances – Galaxy: abundances – Galaxy: halo – errata, addenda

We realised that there was a mistake in the code that com-
puted parameters for the photometric data sample. The effec-
tive temperature was not computed according to the formula in
footnote 3. As a consequence the surface gravity and metallicit-
ity were also computed incorrectly. We also realised that almost
50% of the lines in the table were duplicated. Furthermore, for
301 763 stars, the interpolation arrived at the edge in metallicity
of the synthetic grid (+0.5) and the program was not extrapolat-
ing. We removed these stars from the final catalogue. A new cat-
alogue, containing 12 894 443 unique stars, has been produced
correcting these two mistakes and deposited at CDS. In the paper
this impacts only Fig. 8, which is corrected in this *corrigendum*,
and the number of stars in this catalogue cited in Sect. 5.2; it
should read: “The final sample, which we refer to in the follow-
ing as ‘photometric’, consists of 12 894 443 unique stars”. None
of the conclusions of the paper are altered by this change.

<figure><img src="image_1.png" /><figcaption>Fig. 8. Distribution of photometric metallicities for the photometric and spectroscopic samples. Each sample has been normalised so that the area under the histogram is equal to one.</figcaption></figure>

<footnote n="1">¹ GEPI, Observatoire de Paris, Université PSL, CNRS, Place Jules Janssen, 92195 Meudon, France
e-mail: Piercarlo.Bonifacio@obspm.fr</footnote>

<footnote n="2">² Departamento de Ciencias Fisicas, Universidad Andres Bello, Fernandez Concha 700, Las Condes, Santiago, Chile</footnote>

<footnote n="3">³ Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, Via G. Sansone 1, 50019 Sesto Fiorentino, Italy</footnote>

<footnote n="4">⁴ INAF/Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy</footnote>

<footnote n="5">⁵ European Southern Observatory, Casilla 19001, Santiago, Chile</footnote>

<footnote n="6">⁶ Zentrum für Astronomie der Universität Heidelberg, Landessternwarte, Königstuhl 12, 69117 Heidelberg, Germany</footnote>

<footnote n="7">⁷ UPJV, Université de Picardie Jules Verne, 33 rue St Leu, 80080 Amiens, France</footnote>

<footnote n="8">⁸ Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12, 69120 Heidelberg, Germany</footnote>

<footnote n="9">⁹ INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova I-35122, Italy</footnote>

<footnote>* Spectroscopic and photometric metallicities derived and discussed in this paper as well as orbital actions computed and discussed this paper are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/666/C1</footnote>