Table 3
Power indices of the power spectrum and Δ-variance slopes computed from maps of dust/gas tracers.
| Optical | FIR | MIR | Planck radiance | NH I | |
|---|---|---|---|---|---|
| γ | −2.88 ± 0.01 | −2.82 ± 0.01 | −3.00 ± 0.01 | −2.98 ± 0.09 | −3.00 ± 0.05 |
| β | −0.08 ± 0.02 | −0.84 ± 0.02 | −0.25 ± 0.05 | − | − |
| α | 0.84 ± 0.03 | 0.70 ± 0.01 | 0.93 ± 0.02 | 0.72 ± 0.04 | 0.94 ± 0.03 |
Notes. γ describes the power term of the radiation from dust/gas, while β describes the contribution from all other astrophysical sources and sky noise. α characterizes the Δ-variance spectrum. See Eqs. (5) and (7). Theoretically, Δ-variance slopes should be related to power indices via α = −γ − 2. The listed uncertainties are from the model fitting and do not include systematic errors.
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