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