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  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
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Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/31789
Title: Iron in X-COP: Tracing enrichment in cluster outskirts with high accuracy abundance profiles (Corrigendum)
Authors: GHIZZARDI, SIMONA 
MOLENDI, SILVANO 
Van der Burg, Remco
DE GRANDI, Sabrina 
BARTALUCCI, IACOPO 
GASTALDELLO, FABIO 
ROSSETTI, Mariachiara 
BIFFI, VERONICA 
BORGANI, STEFANO 
Eckert, Dominique
ETTORI, STEFANO 
GASPARI, MASSIMO 
GHIRARDINI, VITTORIO 
RASIA, ELENA 
Issue Date: 2021
Journal: ASTRONOMY & ASTROPHYSICS 
Number: 652
First Page: C3
Abstract: We discovered a conversion error in deriving the expected iron yield YFe for Maoz &Graur (2017) values (see gold shaded area in our Fig. 19 in the original paper). Expected yields are evaluated through equation 12 and converted to solar units (see Eq. 11). We adopt the solar abundance measurements by Asplund et al. (2009); under this assumption, the solar iron abundance is Zm; = 0:00124; this is the solar iron abundance by mass fraction with respect to the gas mass, namely (Fe=gas). This is the value reported in our Sect. 5.1 and used throughout the paper. However, when we derived YFe using the yIa, kIa, yCC, and kCC estimates from Maoz &Graur (2017), we erroneously used Zm; = 0:00174, which is the solar iron abundance by mass fraction with respect to the hydrogen mass, (Fe=H), leading to a wrong expected range for the iron yield. The correct estimate for YFe is YFe; = 3:65+-1 1:30 30Z. In the meantime, Freundlich &Maoz (2021) published updated values for Type-Ia supernova (SNIa) rates. Their new estimates provide kIa = 3:1+1:1-1:0 × 10-3M-1, which leads to YFe; = 2:34+0:63-0:56Z. By chance, the new updated value is not very different from the wrong value reported in Ghizzardi et al. (2021), leaving our discussion and main conclusions unchanged. The last paragraph in Sect. 5.2 should be replaced with: "Recently, it has been shown (see Maoz &Graur 2017 and Friedmann &Maoz 2018) that type Ia SN explosions in galaxy (Figure Presented) clusters are more frequent than in the field. If, following Maoz &Graur (2017), we assume a SNIa rate per unit mass of kIa = (5:4 ± 2:3) × 10-3M-1, we derive YFe; = 3:65+-1 1:3 3 Z. More recently, Freundlich &Maoz (2021) published updated values for SNIa rates in clusters, kIa = 3:1+1:1-1:0 ×10-3 M-1, which lead to YFe; = 2:34+0:63-0:56Z (gold shaded region in Fig. 19). This revised SN rate brings the expected effective yield closer, but it is still well below the measured ones." Figure 19 should be replaced with the one reported here.
URI: http://hdl.handle.net/20.500.12386/31789
URL: https://www.aanda.org/articles/aa/full_html/2021/08/aa38501e-20/aa38501e-20.html
ISSN: 0004-6361
DOI: 10.1051/0004-6361/202038501e
Fulltext: open
Appears in Collections:1.01 Articoli in rivista

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