Table 2
Dust emission flux densities in Magellanic Bridge A North and South.
| Source | Rap | S100 μm | S160 μm | S250 μm | S350 μm | S500 μm |  |
 |
|---|---|---|---|---|---|---|---|---|
| (′′) | (mJy) | (mJy) | (mJy) | (mJy) | (mJy) | (mJy) | (mJy) | |
| MagB. A(*) | 50 | 952 ± 95 ± 151 | 1565 ± 313 ± 511 | 856 ± 68 ± 48 | 422 ± 34 ± 33 | 187 ± 15 ± 23 | 257 ± 52 ± 28 | <16 |
| North(**) | 11 | 131 ± 13 ± 49 | 305 ± 61 ± 120 | 139 ± 11 ± 12 | … | … | 46 ± 9 ± 5 | <7 |
| South(**) | 11 | 678 ± 68 ± 48 | 838 ± 168 ± 120 | 449 ± 36 ± 13 | … | … | 56 ± 11 ± 5 | <7 |
Notes. We express the errors on our measurements with the flux calibration error first (Herschel errors obtained from Meixner et al. 2013) and the photometric error last. (†)Flux at 870 μm has the free–free emission and CO(3−2) line contributions subtracted. (‡) Flux at 1.3 mm has the free–free emission contribution subtracted. (*)In Magellanic Bridge A, all images are convolved to a common resolution of 43′′. (**) In the North and South sources all images are convolved to a common resolution of 22′′.
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