Table 2
Results of the spectral fits for the extended emission of the 5 sources with the highest number of counts.
| Name | Model name | Model parameters | Nuclear component |  (d.o.f.) |
F(0.5–2 keV) |
|
|
|||||
| 3C 171 | pha(mekal+zpha(po)) |  [keV]  |
Γ = 1.7fix zNh = 8.8e22 [cm-2] fix | 1.25(4) | 1.19e–14 |
| ab = 0.3 fix | 1.83(5) | ||||
| ab = 0.5 fix | 2.26(5) | ||||
| pha(pow+zpha(po)) |
|
Γ = 1.7fix zNh = 8.8e22 [cm-2] fix | 1.26(5) | 1.33e-14 | |
| Γ = 1.7 fix | 4.76(6) | ||||
| pha(xstar+zpha(po)) |  e21 [cm-2]  |
Γ = 1.7fix zNh = 8.8e22 [cm-2] fix | 0.94(4) | 1.89e-14 | |
|
|
|||||
| 3C 305 | pha(mekal) | kT = 1.06 ± 0.1 [keV] ab = 0.3 fix | 4.17e-14 | ||
| pha(po) | Γ = 2.5 ± 0.2 | 4.62e-14 | |||
| pha(xstar) | N = (2.17 ± 0.09)e21 [cm-2] log ξ = 5.0 ± 1.0 | 4.07e-14 | |||
|
|
|||||
| 3C 403 | pha(mekal+zpha(po)) | kT = 0.38 ± 0.05 [keV] ab = 0.00 ± 0.01 | Γ = 1.7fix zNh = (19.7 ± 5.2) e22 [cm-2] | 9.12e-15 | |
| pha(pow+zpha(po)) | Γ = 3.9 ± 0.3 | Γ = 1.7fix zNh = (24.1 ± 7.1) e22 [cm-2] | 8.97e-15 | ||
| pha(xstar+zpha(po)) | N = (8.3 ± 12.0)e23 [cm-2] log ξ = 5.0 ± 3.3 | Γ = 1.7fix zN = (18.8 ± 6.8)e22 [cm-2] | 1.25e-14 | ||
|
|
|||||
| 3C 433 | pha(mekal+zpha(po)) | kT = 0.7 ± 0.1 [keV] ab = 0.1 ± 0.09 | Γ = 1.7fix zNh = (8.6 ± 2.1)e22 [cm-2] | 1.04e-14 | |
| pha(pow+zpha(po)) | Γ = 3.5 ± 0.5 | Γ = 1.7fix zNh = (10.3 ± 2.8)e22 [cm-2] | 1.03e-14 | ||
| pha(xstar+zpha(po)) | N = (9.9 ± 2.7)e21 [cm-2] Log ξ = 3.9 ± 1.2 | Γ = 1.7fix zNh = (12.1 ± 3.4)e22 [cm-2] | 1.15e-14 | ||
|
|
|||||
| 3C 445 | pha(mekal+zpha(po)) | kT = 0.39 ± 0.05 [keV] ab = 0.00 ± 0.01 | Γ = 1.7fix zNh = (11.0 ± 6.5)e22 [cm-2] | 0.85(4) | 1.46e-14 |
| ab = 0.3 fix | 2.84(5) | ||||
| ab = 0.5 fix | 2.91(5) | ||||
| pha(pow+zpha(po)) | Γ = 3.7 ± 0.2 | Γ = 1.7 fix zNh = (14.7 ± 7.9)e22 [cm-2] | 1.22(5) | 1.03e-14 | |
| Γ = 1.7 fix | 10.89(6) | ||||
| pha(xstar+zpha(po)) | N = (1.1 ± 0.1)e22 [cm-2] Logξ = 5.0 ± 3.4 | Γ = 1.7fix zNh = (15.9 ± 8.6)e22 [cm-2] | 2.45(4) | 1.59e-14 | |
Notes. For 3C 305, 3C 403, and 3C 433 the spectrum is grouped to at least 10 counts/bin and we apply a Poissonian statistic (cstat). The fluxes reported in the table are corrected for Galactic absorption. For 3C 171 and 3C 445 the spectrum is grouped by at least 20 counts/bin (χ2 statistic). In four cases we add in the models a power-law component to fit the emission observed in the hard band. Notes. 3C 171: in all the models, we fixed the nuclear component parameters at Γ = 1.7 and NH = 8.8 × 1022 cm-2 (see Hardcastle et al. 2010); 3C 305: the spectrum do not require a nuclear related component. We do not report in table the flux measurement if the model is not representative of the spectrum (according to the χ2 value).
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