The Simons Observatory: assessing the impact of dust complexity on the recovery of primordial B-modes

We investigate how dust foreground complexity can affect measurements of the tensor-to-scalar ratio,r, in the context of the Simons Observatory, using a cross-spectrum component separation analysis. Employing a suite of simulations with realistic Galactic dust emission, we find that spatial variation in the dust frequency spectrum, parametrized by β_d, can bias the estimate forrwhen modeled using a low-order moment expansion to capture this spatial variation. While this approach performs well across a broad range of dust complexity, the bias increases with more extreme spatial variation in dust frequency spectrum, reaching as high asr∼ 0.03 for simulations with no primordial tensors and a spatial dispersion of σ (β_d) ≃ 0.3 — the most extreme case considered, yet still consistent with current observational constraints. This bias is driven by changes in the ℓ-dependence of the dust power spectrum as a function of frequency that can mimic a primordialB-mode tensor signal. Although low-order moment expansions fail to capture the full effect when the spatial variations of β_d become large and highly non-Gaussian, our results show that extended parametric methods can still recover unbiased estimates ofrunder a wide range of dust complexities. We further find that the bias inr, at the highest degrees of dust complexity, is largely insensitive to the spatial structure of the dust amplitude and is instead dominated by spatial correlations between β_d and dust amplitude, particularly at higher orders. If β_d does spatially vary at the highest levels investigated here, we would expect to use more flexible foreground models to achieve an unbiased constraint onrfor the noise levels anticipated from the Simons Observatory.