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Table 7

WISE flux densities for the DGS sample.

Source F 3.4 F 4.6 F 12 F 22 Aperture radius
[mJy] [mJy] [mJy] [mJy] [′′]

Haro11 17.9 ± 1.9 32.6 ± 3.4 353. ± 19. 2054. ± 148. 45a, 90b
Haro2 24.5 ± 2.6 16.5 ± 1.7 152. ± 8. 760. ± 55. 50a, 65b
Haro3 25.8 ± 2.7 17.7 ± 1.9 162. ± 9. 766. ± 56. 60a
He2-10 133. ± 17. 92.7 ± 11.2 996. ± 53. 5018. ± 362. 81b
HS0017+1055 0.16 ± 0.03 0.25 ± 0.04 3.83 ± 0.49 11.7 ± 2.0 12a, 25b
HS0052+2536 0.65 ± 0.08 0.52 ± 0.07 3.71 ± 0.40 16.2 ± 2.3 17a, 23a
HS0822+3542 0.106 ± 0.009c 0.082 ± 0.008c 0.47c 3.85c
HS1222+3741 0.15 ± 0.03 0.15 ± 0.03 1.0 ± 0.2c 5.94 ± 0.73c 14a, –
HS1236+3937 0.22 ± 0.05 0.16 ± 0.04 0.65 2.72 15a
HS1304+3529 0.4 ± 0.1 0.43 ± 0.09 1.78 ± 0.21c 10.5 ± 0.9c 18a, –
HS1319+3224 0.06 ± 0.02 0.07 ± 0.02 0.70c 1.93c 12b, –
HS1330+3651 0.51 ± 0.07 0.36 ± 0.07 1.23 ± 0.26 5.31 ± 1.26 20a
HS1442+4250 1.20 ± 0.14 0.8 ± 0.1 1.54 ± 0.33 9.40 32b
HS2352+2733 0.15 ± 0.04 0.13 ± 0.04 1.03c 2.98c 15a, –
IZw18 0.33 ± 0.07 0.39 ± 0.07 0.8 ± 0.3 4.64 ± 1.19 23b
IC 10 1454. ± 154. 917. ± 98. 3521. ± 191. 9991. ± 728. 205 × 150b, 230b
IIZw40 18.6 ± 2.0 19.3 ± 2.1 335. ± 18. 1540. ± 112. 45 × 33a, 90b
Mrk 1089 19.0 ± 2.3 13.9 ± 3.1 102. ± 6. 453. ± 34. 75a
Mrk 1450 1.10 ± 0.12 0.73 ± 0.09 8.00 ± 0.74 49.3 ± 4.8 20a, 40b
Mrk 153 2.03 ± 0.23 1.34 ± 0.17 4.61 ± 0.41 28.1 ± 3.9 25a
Mrk 209 2.61 ± 0.39 1.70 ± 0.31 7.30 ± 0.85 46.4 ± 5.4 39a
Mrk 930 2.61 ± 0.30 2.26 ± 0.27 25.8 ± 2.6 170. ± 14. 34b, 60a
NGC 1140 32.7 ± 3.5 21.6 ± 2.3 94.9 ± 5.5 367. ± 28. 118a
NGC 1569 359. ± 24. 240. ± 47. 1021. ± 116. 6971. ± 503. 120b
NGC 1705 25.7 ± 2.7 16.1 ± 1.7 20.3 ± 1.5 46.2 ± 6.1 75 × 46b, 72a
NGC 2366 75.8 ± 5.7 39.4 ± 6.2 121. ± 12. 612. ± 65. 260 × 125b, 150a
NGC 4214 294. ± 31. 184. ± 19. 546. ± 29. 1830. ± 133. 181a
NGC 4449 483. ± 50. 307. ± 32. 1323.8 ± 70.0 3119. ± 227. 190 × 170a, 250a
NGC 4861 18.1 ± 1.1 10.1 ± 1.9 52.8 ± 5.7 330. ± 26. 120 × 50b, 120a
NGC 5253 212. ± 22. 255. ± 27. 2002. ± 105. 10345. ± 746. 120 × 80b, 120a
NGC 625 106. ± 11. 64.7 ± 6.8 194. ± 11. 797. ± 59. 200 × 75
NGC 6822d
Pox186 0.34 0.44 2.67 ± 0.33 11.2 ± 1.4 25b
SBS0335-052 0.45 ± 0.05 1.45 ± 0.16 23.4 ± 1.4 67.8 ± 5.8 14b, 35b
SBS1159+545 0.09 0.11 1.0 ± 0.3 4.44 ± 1.38 12a, 25b
SBS1211+540 0.133 ± 0.009 0.10 ± 0.03 0.80 3.60 15a
SBS1249+493 0.05c 0.07c 1.17 3.76 -, 20b
SBS1415+437 0.8 ± 0.1 0.53 ± 0.08 2.30 ± 0.55 15.5 ± 2.8 28 × 15b, 34a
SBS1533+574 1.52 ± 0.19 1.28 ± 0.17 9.76 ± 0.84 53.3 ± 4.7 30a, 50b
Tol0618-402 2.33 ± 0.33 1.32 ± 0.21 0.71 1.73 18a
Tol1214-277 0.13 0.14 0.8 ± 0.2c 6.89c 12a, –
UGC 4483 1.12 ± 0.26 1.01 2.30 12.72 43 × 24
UGCA 20 0.26 ± 0.08 0.24 0.74 3.27 20a
UM133 10.83 6.74 1.49 6.70 26a
UM311 48.5 ± 3.0 29.1 ± 3.5 120. ± 7. 292. ± 25. 115a
UM448 15.4 ± 1.6 11.7 ± 1.3 103. ± 6. 552. ± 40. 64a
UM461 0.58 ± 0.07 0.52 ± 0.07 5.98 ± 1.02 29.4 ± 4.9 17a, 35b
VIIZw403 2.59 ± 0.29 1.89 ± 0.23 4.54 ± 0.61 26.3 ± 3.6 40a

Notes. In the aperture column, a single value indicates that only one aperture has been used for the four wavelengths. Two values separated by a comma indicate that a different aperture has been used for WISE1 and WISE2 on one side (first value), and WISE3 and WISE4 on the other side (second value, see text for details). For several galaxies elliptical apertures were used to match the morphology of the source and are indicated by semi-major axis × semi-minor axis. A dash indicates that we take the profile fit photometry from the All WISE database.

(a)

The aperture is the same as that used for IRAC or Herschel photometry.

(b)

The aperture has been adapted to match the peculiar morphology of the source in the NIR/MIR or to avoid a contaminating source.

(c)

This galaxy is not resolved at these wavelengths and we thus use the profile fit photometry provided by the WISE database.

(d)

The WISE map does not cover the full galaxy. Thus we do not report flux densities for this source.

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