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Table 6

Spitzer IRAC flux densities for the DGS sample.

Source F 3.6 F 4.5 F 5.8 F 8.0 Aperture radius Aper corr ?
[mJy] [mJy] [mJy] [mJy] [′′]
Haro11 22.4 ± 3.2 32.3 ± 4.6 77.1 ± 10.9 164. ± 23. 45a yes
Haro2 24.7 ± 3.5 18.2 ± 2.6 49.3 ± 7.0 257. ± 36. 50a yes
Haro3 28.2 ± 4.0 21.5 ± 3.1 43.9 ± 6.3 116. ± 16. 60a yes
He2-10 134. ± 19. 99.2 ± 14.1 296. ± 42. 836. ± 118. 108a yes
HS0017+1055 0.17 ± 0.02 0.31 ± 0.03 0.76 ± 0.08 1.53 ± 0.16 12b
HS0052+2536 0.7 ± 0.1 0.32 ± 0.09 0.7 ± 0.2 3.17 ± 0.46 17c yes
HS0822+3542 0.12 ± 0.01 0.10 ± 0.01 0.10 ± 0.02 0.09 ± 0.02 5b yes
HS1222+3741 0.25 ± 0.03 0.19 ± 0.02 0.27 ± 0.05 0.57 ± 0.07 14a
HS1236+3937 ≤0.56 ≤0.38 ≤0.66 ≤0.32 15a
HS1304+3529 0.38 ± 0.08 0.41 ± 0.09 ≤0.78 0.6 ± 0.1 18a
HS1319+3224 0.061 ± 0.010 0.051 ± 0.008 0.10 ± 0.02 0.12 ± 0.02 8a
HS1330+3651 0.56 ± 0.09 0.5 ± 0.1 ≤0.80 1.0 ± 0.2 20a
HS1442+4250 – 1.24 ± 0.21 – 1.59 ± 0.25 51a yes
HS2352+2733 ≤0.04 ≤0.04 ≤0.13 ≤0.11 15a
IZw18 0.36 ± 0.05 0.35 ± 0.05 0.39 ± 0.07 0.53 ± 0.08 12b yes
IC 10f – – – – – –
IIZw40 18.1 ± 4.3 19.9 ± 3.5 39.8 ± 5.7 105. ± 15. 45 × 33c yes
Mrk 1089 20.4 ± 2.9 15.5 ± 2.2 31.4 ± 4.4 82.2 ± 11.6 75a yes
Mrk 1450 1.22 ± 0.17 1.01 ± 0.14 0.9 ± 0.1 2.06 ± 0.29 20a yes
Mrk 153 2.29 ± 0.33 1.70 ± 0.24 1.76 ± 0.25 2.75 ± 0.39 25b yes
Mrk 209 2.90 ± 0.41 2.21 ± 0.32 1.78 ± 0.27 2.20 ± 0.32 39d yes
Mrk 930 2.66 ± 0.38 2.73 ± 0.39 4.17 ± 0.59 10. ± 1. 13b yes
NGC 1140 32.8 ± 4.8 23.3 ± 3.4 41.0 ± 5.8 93.9 ± 13.3 118a yes
NGC 1569 312. ± 45. 244. ± 35. 324. ± 46. 533. ± 75. 150a yes
NGC 1705 25.5 ± 5.9 18.3 ± 4.2 15.0 ± 2.8 17.5 ± 2.6 72a yes
NGC 2366 61.5 ± 12.4 45.7 ± 10.4 35.8 ± 7.6 52.8 ± 8.1 200d yes
NGC 4214 334. ± 47. 253. ± 36. 280. ± 40. 748. ± 106. 205 × 160c yes
NGC 4449 472. ± 67. 342. ± 48. 709. ± 100. 1622. ± 229. 190 × 170c yes
NGC 4861 18.3 ± 2.6 13.8 ± 2.0 16.8 ± 2.5 17.7 ± 2.5 100 × 50c yes
NGC 5253 235. ± 34. 252. ± 36. 458. ± 65. 812. ± 115. 120a yes
NGC 625 110. ± 16. 79.7 ± 11.4 71.3 ± 10.1 147. ± 21. 170a yes
NGC 6822 1780. ± 272. 1240. ± 196. 951. ± 141. 1226. ± 175. 440a yes
Pox186 0.18 ± 0.02 0.18 ± 0.02 0.14 ± 0.03 0.64 ± 0.07 9b
SBS0335-052 0.78 ± 0.08 1.64 ± 0.17 4.50 ± 0.45 12.3 ± 1.2 10a
SBS1159+545 0.11 ± 0.01 0.10 ± 0.01 0.12 ± 0.03 0.59 ± 0.07 12d
SBS1211+540 0.16 ± 0.02 0.08 ± 0.01 ≤0.12 0.30 ± 0.05 15a
SBS1249+493 0.08 ± 0.02 0.07 ± 0.02 ≤0.20 0.26 ± 0.04 5b
SBS1415+437 – 0.8 ± 0.1 – 0.50 ± 0.08 34a yes
SBS1533+574 2.09 ± 0.34 1.52 ± 0.24 2.26 ± 0.33 3.32 ± 0.48 30a yes
Tol0618-402 2.68 ± 0.38 1.64 ± 0.23 1.13 ± 0.16 0.9 ± 0.1 18a yes
Tol1214-277 0.076 ± 0.009 0.09 ± 0.01 0.15 ± 0.03 0.25 ± 0.03 8b
UGC 4483 1.69 ± 0.25 1.02 ± 0.15 ≤0.62 0.9 ± 0.1 43 × 24c yes
UGCA 20 ≤0.85 ≤0.60 ≤1.07 ≤0.46 20a
UM133 0.39 ± 0.08 0.28 ± 0.06 ≤0.46 ≤0.27 8a
UM311 – 33.4 ± 4.7 – 114. ± 16. 115e yes
UM448 17.7 ± 2.5 13.2 ± 1.9 34.1 ± 4.8 83.0 ± 11.7 53 × 31c yes
UM461 0.8 ± 0.1 0.61 ± 0.09 0.8 ± 0.1 1.58 ± 0.29 17a yes
VIIZw403 2.86 ± 0.41 2.23 ± 0.32 1.69 ± 0.25 2.56 ± 0.37 40a yes

Notes.

(a)

The aperture is the same as the one used for Herschel.

(b)

The Herschel aperture has been shorten to avoid a contaminating source.

(c)

The Herschel aperture has been adapted to match the peculiar morphology of the source in the NIR.

(d)

The Herschel aperture has been enlarged to encompass all of the NIR emission.

(e)

The IRAC map is smaller than the Herschel aperture. The aperture thus had to be shorten.

(f)

The IRAC maps do not cover the full galaxy. Thus we do not report flux densities for this source.

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