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Table 3

SFR and AGN relative contributions to the IR output, along with IR luminosities (in cgs units).

Sourcesa SFR b α IR c L IR d e
[M⊙   yr-1] [× 1046] [× 1046]
IRAS F00235+1024 0.68 ± 0.12 20 ± 8 6 ± 4
IRAS 07380-2342 <700 14.2 ± 0.6 3 ± 2
IRAS 09104+4109* <600 13.8 ± 1.3
IRAS F10026+4949 <500 >0.8 140 ± 40 <20
IRAS F12509+3122 2000 ± 1400 36 ± 13 18 ± 8
IRAS 12514+1027 400 ± 300 3.7 ± 0.4
IRAS 14026+4341 400 ± 300 6.2 ± 0.5
IRAS F15307+3252 3000 ± 2000 52 ± 17
IRAS F16124+3241 16 ± 6
ELAIS J1640+41 <1200 <120 <20
IRAS 18216+6418 8.0 ± 1.4
(a)

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

(b)

Star formation rates estimated through PAH intensity (see Sect. 5.1).

(c)

AGN contribution to the total IR luminosity (see Sect. 5.2).

(d)

Total IR luminosity (8−1000 μm), estimated through IRAS fluxes.

(e)

IR luminosity (8−1000 μm) of the SB component (see Sect. 5.1).

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