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Table 1.
Bands used for the SED modelling.
| Telescope/Filter (a) | λ | FWHM(b) | Number of galaxies |
|---|---|---|---|
| (μm) | (arcsec) | ||
| 2MASS/J | 1.25 | 2.5 | 732 |
| 2MASS/H | 1.65 | 2.5 | 708 |
| 2MASS/Ks | 2.17 | 2.5 | 729 |
| WISE/W1 | 3.4 | 8.4 | 715 |
| WISE/W2 | 4.6 | 9.2 | 715 |
| Spitzer/IRAC | 8.0 | 2.0 | 99 |
| WISE/W3 | 12 | 11.4 | 735 |
| WISE/W4 | 22 | 18.6 | 740 |
| Herschel/PACS | 70 | 5.8 | 125 |
| Herschel/PACS | 100 | 7.1 | 501 |
| Herschel/PACS | 160 | 11.2 | 522 |
| Herschel/SPIRE | 250 | 18.2 | 698 |
| Planck/HFI | 350 | 260.0 | 360 |
| Herschel/SPIRE | 350 | 25.0 | 698 |
| Herschel/SPIRE | 500 | 36.4 | 692 |
| Planck/HFI | 550 | 281.0 | 251 |
| Planck/HFI | 850 | 290.0 | 181 |
Notes.
(a)
Filter here is defined to mean either the instrument used, or the camera used, or the filter used, depending on the telescope facility.
(b)
References for FWHM – these are the same as in Lianou et al. (2014), while for Planck/HFI this is given in Planck Collaboration VII (2014).
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