Table 1.
Abundances and abundance ratios within the 3.4 arcmin wide (in the cross-dispersion direction) extraction region.
| Source | A 3526 | M 49 | M 87 | NGC 4636 | NGC 4649 | NGC 5044 | NGC 5813 | NGC 5846 |
|---|---|---|---|---|---|---|---|---|
| r/r500 | 0.026 | 0.018 | 0.012 | 0.022 | 0.015 | 0.034 | 0.031 | 0.036 |
| kpc | 43.2 | 18.7 | 17.7 | 15.6 | 15.6 | 37.7 | 26.9 | 25.8 |
| Model | NH+2T | GDEM | 2T+PL | 2T | 1T | GDEM | 2T | 2T |
| C-stat./d.o.f. | 2186/1088 | 852/544 | 3954/1111 | 748/480 | 1530/1096 | 1670/1094 | 2480/1649 | 1825/1093 |
| σN/Fe | ∼7σ | ∼3σ | ∼9σ | ∼4σ | ∼3σ | ∼5σ | ∼5σ | ∼3σ |
| N/O | 2.7 ± 0.5 | 2.7 ± 1.0 | 2.2 ± 0.3 | 3.3 ± 1.1 | 2.9 ± 1.0 | 2.2 ± 0.5 | 3.2 ± 0.9 | 2.7 ± 0.8 |
| N/Fe | 1.5 ± 0.2 | 1.6 ± 0.6 | 1.8 ± 0.2 | 1.9 ± 0.5 | 2.4 ± 0.8 | 1.4 ± 0.3 | 1.9 ± 0.4 | 2.3 ± 0.7 |
| O/Fe | 0.54 ± 0.04 | 0.59 ± 0.10 | 0.82 ± 0.03 | 0.59 ± 0.08 | 0.84 ± 0.11 | 0.65 ± 0.05 | 0.58 ± 0.07 | 0.86 ± 0.12 |
| Ne/Fe | 0.57 ± 0.06 | 0.66 ± 0.17 | 0.55 ± 0.05 | 0.64 ± 0.12 | 1.07 ± 0.19 | 0.68 ± 0.08 | 0.53 ± 0.09 | 0.71 ± 0.14 |
| Mg/Fe | 0.66 ± 0.07 | 0.79 ± 0.19 | 0.24 ± 0.04 | 0.64 ± 0.13 | 1.40 ± 0.23 | 0.77 ± 0.08 | 0.83 ± 0.11 | 0.66 ± 0.14 |
| Fe | 1.02 ± 0.03 | 1.50 ± 0.12 | 0.55 ± 0.01 | 0.66 ± 0.04 | 0.55 ± 0.03 | 0.78 ± 0.03 | 0.92 ± 0.04 | 0.77 ± 0.05 |
| Ni/Fe | 1.2 ± 0.1 | 1.8 ± 0.5 | 0.65 ± 0.07 | 2.0 ± 0.4 | 2.5 ± 0.4 | 1.5 ± 0.3 | – | 2.0 ± 0.4 |
Notes. Abundances and abundance ratios are given according to the proto-solar abundance of Lodders et al. (2009). Statistical uncertainties (1σ) are quoted here. Systematic uncertainties on the abundance ratios are estimated in Sect. 4. σN/Fe is the significance level of nitrogen detection according to the N/Fe ratio (to be greater than zero). The uncertainties shown are 1σ statistical error bars. 1T, 2T, and GDEM refer to single-temperature, two-temperature, and multi-temperature DEM distribution (Sect. 3). For A 3526, “NH” refers to a free Galactic hydrogen column density in the spectral analysis. The Galactic hydrogen column densities for the other seven systems are frozen to literature values. For M 87, we use a power law to model the non-thermal component, which varies between the two observations (Werner et al. 2006a). For NGC 5813, the Ni abundance cannot be constrained, and we fix it to solar during the fitting.
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