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Table 2

Best-fit model parameters (cf. Sect. 4).

Sourcesa Modelb χ2 /d.o.f. (mJy)c α 6 d Spectral indexe τ 6 f Additional features

IRAS F00235+1024 A 238/75 86 ± 5 0.982 ± 0.002 0.8 2.57 ± 0.06 ...
B 218/74 >1.0 ...
IRAS 07380-2342 A 22/76 213 ± 12 0.988 ± 0.006 0.8 0.49 ± 0.05 ...
B 16/75 0.990 ± 0.009 < 0.3 ...
IRAS 09104+4109* A 44/69 176 ± 3 0.995 ± 0.002 0.8 0.69 ± 0.02 [NeVI] emission line g
B 26/68 104 ± 11 0.996 ± 0.004 1.65 ± 0.17 0.16 ± 0.10 [NeVI] emission lineg
IRAS F10026+4949 A 19/88 >0.988 0.8 ...
B 19/87 150 ± 60 >0.992 ...
IRAS F12509+3122 A 51/85 0.8 0.04 ...
B 51/84 25 ± 6 < 0.2 ...
IRAS 12514+1027 A 116/73 57.4 ± 1.0 0.958 ± 0.003 0.8 0.02 [NeVI] emission line g
B 114/72 57 ± 7 0.956 ± 0.004 < 0.12 [NeVI] emission lineg
IRAS 14026+4341 A 33/75 75 ± 2 0.977 ± 0.004 0.8 0.06 ± 0.02 ...
B 31/74 0.978 ± 0.004 < 0.18 ...
IRAS F15307+3252 A 238/84 38 ± 2 0.981 ± 0.004 0.8 0.64 ± 0.04 ...
B 173/83 0.975 ± 0.006 >1.4 ...
IRAS F16124+3241 A 38/78 6.6 ± 1.3 0.8 1.3 ± 0.2 ...
B 38/77 7 ± 4 ...
ELAIS J1640+41 A 33/88 17.3 ± 1.1 0.993 ± 0.006 0.8 0.13 ± 0.06 ...
B 32/87 >0.988 < 0.4 ...
IRAS 18216+6418 A 117/77 >0.999 0.8 < 0.001 ...
A 18/76 0.4 0.17 ...
(a)

Sources where our model is not reliable are marked with *.

(b)

HLIRG emission model (A: AGN power law slope fixed at 0.8; B: AGN power law slope allowed to vary between 0.2 and 1.8). See Sect. 4.1 for a complete discussion of the adopted model. The best-fit model is shown in boldface.

(c)

Intrinsic flux at 6 μm (corrected by dust absorption).

(d)

Relative contribution of the AGN component at 6 μm.

(e)

Spectral index of the AGN power law.

(f)

Optical depth at 6 μm of the obscuring material.

(g)

Emission line at 7.65 μm. See Sect 4.2 for a discussion about these spectral features.

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