Dust depletion of metals from local to distant galaxies - I. Peculiar nucleosynthesis effects and grain growth in the ISM

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Volume 666 (October 2022)

A&A, 666 (2022) A12

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This article has an erratum: [https://doi.org/10.1051/0004-6361/202243994e]

Table 4

Coefficients A2_X and B2_X resulting from the linear merged fit δ_X = A2_X +B2_X × [Zn/Fe] of the depletion sequences shown in Figs. 4, 2, B.2, the degrees of freedom v, and the Pearson correlation coefficients r.

X	SMC/LMC knee at [Fe/H] = −1.3			Constant α_X			v

	A2_X	B2_X	r	A2_X	B2_X	r
C	0.00	−0.10 ± 0.10	−0.10	0.00	−0.10 ± 0.10	−0.10	3
P	0.03 ± 0.05	−0.21 ± 0.08	−0.46	0.03 ± 0.05	−0.21 ± 0.08	−0.46	43
O	0.00 ± 0.00	−0.20 ± 0.05	−0.31	0.00 ± 0.00	−0.20 ± 0.05	−0.50	22
Cl	0.00	−0.12 ± 0.09	−0.80	0.00	−0.12 ± 0.09	−0.80	6
Kr	0.00	−0.04 ± 0.09	−0.53	0.00	−0.04 ± 0.09	−0.53	3
S	0.01 ± 0.02	−0.48 ± 0.04	−0.68	0.01 ± 0.02	−0.48 ± 0.04	−0.68	99
Zn	0.00 ± 0.01	−0.27 ± 0.03	−1.00 ^(a)	0.00 ± 0.01	−0.27 ± 0.03	−1.00 ^(a)
Ge	0.00	−0.40 ± 0.04	−0.91	0.00	−0.40 ± 0.04	−0.91	1
Mg	0.01 ± 0.03	−0.60 ± 0.04	−0.86	0.01 ± 0.03	−0.66 ± 0.04	−0.91	69
Si	−0.04 ± 0.02	−0.72 ± 0.03	−0.87	−0.04 ± 0.02	−0.75 ± 0.03	−0.88	151
Cu	0.00	−0.73 ± 0.04	−0.87	0.00	−0.73 ± 0.04	−0.87	4
Co	0.00	−0.89 ± 0.19	−0.87	0.00	−0.89 ± 0.19	−0.87	6
Mn	0.07 ± 0.02	−1.06 ± 0.03	−0.96	0.07 ± 0.02	−1.03 ± 0.03	−0.96	93
Cr	0.12 ± 0.01	−1.30 ± 0.01	−0.98	0.12 ± 0.01	−1.30 ± 0.01	−0.98	192
Ni	0.07 ± 0.02	−1.31 ± 0.03	−0.96	0.07 ± 0.02	−1.31 ± 0.03	−0.96	168
Fe	−0.01 ± 0.03	−1.26 ± 0.04	−1.00 ^(a)	−0.01 ± 0.03	−1.26 ± 0.04	−1.00 ^(a)
Al	0.00	−1.66 ± 0.35	−0.69	0.00	−1.66 ± 0.35	−0.69	7
Ti	−0.06 ± 0.03	−1.64 ± 0.04	−0.97	−0.07 ± 0.03	−1.67 ± 0.04	−0.97	81

Notes. Exceptions are Zn and Fe, which are taken from De Cia et al. (2016).^(a) r = −1 by construction. The coefficients are given for two assumptions on the knee position for the Magellanic Clouds. We recommend that the one with constant α_X is used.

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