Table 2
XMM-Newton/RGS cooling flow modeling and O vii local fits.
| 0.8′ region | 3.4′ region | Highest σrf | UV / FUSE | ||||||||
|
|
|||||||||||
| Source | M⊙ yr-1 | T (keV) | O/Fe | O viir | O viif | O viir | O viif | O viir | O viif | O vi | M⊙ yr-1 |
|
|
|||||||||||
| IC 1459 | 0.22 ± 0.04 | 0.79 ± 0.09 | 1.50 ± 0.30 | 0.04 ± 0.04 | − | 0.18 ± 0.07* | −* | 2.5 | − | Y | 1.55 |
| M 84 | 0.48 ± 0.02 | 1.10 ± 0.04 | 0.79 ± 0.06 | 0.11 ± 0.03* | 0.03 ± 0.02* | 0.03 ± 0.03 | − | 3.5 | 1.2 | Y | 0.32 |
| M 86 | 0.55 ± 0.02 | 1.35 ± 0.06 | 0.89 ± 0.07 | 0.29 ± 0.08 | − | 0.50 ± 0.16* | 0.48 ± 0.19* | 3.2 | 2.6 | P | 0.26 |
| M 89 | 0.30 ± 0.03 | 0.83 ± 0.06 | 0.94 ± 0.13 | − | 0.09 ± 0.04 | 0.15 ± 0.09* | 0.24 ± 0.09* | 1.7 | 2.6 | P | 0.24 |
| NGC 1316 | 0.30 ± 0.01 | 1.07 ± 0.04 | 0.90 ± 0.06 | 0.12 ± 0.02* | 0.07 ± 0.02* | 0.13 ± 0.03 | 0.04 ± 0.03 | 5.2 | 3.5 | Y | 0.78 |
| NGC 1332 | 0.24 ± 0.02 | 0.83 ± 0.06 | 0.60 ± 0.12 | 0.03 ± 0.02* | 0.03 ± 0.02* | − | − | 1.5 | 1.5 | UL | − |
| NGC 1404 | 1.19 ± 0.04 | 0.97 ± 0.03 | 0.56 ± 0.05 | 0.07 ± 0.06* | 0.10 ± 0.06* | − | − | 1.1 | 1.7 | UL | 0.19 |
| NGC 4636 | 1.14 ± 0.02 | 1.06 ± 0.02 | 0.57 ± 0.02 | 0.09 ± 0.04 | 0.14 ± 0.04 | 0.23 ± 0.07* | 0.28 ± 0.07* | 3.2 | 3.9 | Y | 0.27 |
| NGC 5846 | 1.77 ± 0.02 | 1.13 ± 0.02 | 0.62 ± 0.03 | 0.07 ± 0.02* | 0.03 ± 0.02* | 0.08 ± 0.03 | 0.03 ± 0.02 | 3.3 | 1.5 | Y | 0.87 |
Notes. Cooling rates, temperatures, and O/Fe abundance ratios for the 8–27 Å RGS cooling flow model. The flux and significance of each line were measured with accurate local fits (see Sect. 3.1). Line fluxes are in photons m-2 s-1. Starred fluxes
are those maximizing both O vii(r,f) detections. UV O vi detections and cooling rates (with typical ≳30% uncertainties) are taken from Bregman et al. (2005, see also Table 1).
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