Table 1
Dust SED, ν Iν, and its uncertainty, σ(ν Iν), for the Diffuse High Galactic Latitude (DHGL) medium.
| Instrument | DIRBE | DIRBE | DIRBE | DIRBE | DIRBE | DIRBE | DIRBE | DIRBE | WMAP | WMAP |
| λ (μm) | 3.5 | 4.9 | 12 | 25 | 60 | 100 | 140 | 240 | 3200 | 4900 |
|
|
||||||||||
| ν Iν | 8.4 | 9.5 | 61.6 | 30.7 | 47.6 | 160.6 | 216.6 | 99.2 | 4.0 × 10-3 | 8.2 × 10-4 |
| σ(ν Iν) | 1.0 | 1.1 | 7.3 | 3.6 | 1.1 | 19.0 | 18.8 | 8.9 | 1.5 × 10-4 | 4.9 × 10-5 |
|
|
||||||||||
| Instrument | PACS | SPIRE | SPIRE | SPIRE | HFI | HFI | HFI | |||
| λ (μm) | 160 | 250 | 350 | 500 | 350 | 550 | 850 | |||
|
|
||||||||||
| ν Iν | 217.0 | 100.0 | 37.3 | 11.6 | 36.0 | 8.3 | 1.4 | |||
| σ(ν Iν) | 34.7 | 9.3 | 3.3 | 1.5 | 3.2 | 1.4 | 0.3 | |||
Notes. Unit is 10-30 W sr-1 H-1. The DIRBE and WMAP values were obtained by correlation of the measured intensities with H I emission data and corrected to account for the contributions of the diffuse ionized medium and the diffuse molecular gas (see Sect. 4.1). The Herschel PACS, SPIRE and Planck/HFI values were derived by integrating the FIRAS spectrum (see Sect. 4.1) considering the instrument transmission and color correction.
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