Table 3. Open in new tab Comparison of...

				Dust scattering^‡
Paβ/Hα	<3.5 × 10⁻² (Main southwest)	7.6 × 10⁻²	5.7 × 10⁻²	(3.0 ± 0.3) × 10⁻²	(5.2 ± 0.4) × 10⁻²

				Dust scattering^‡
Paβ/Hα	<3.5 × 10⁻² (Main southwest)	7.6 × 10⁻²	5.7 × 10⁻²	(3.0 ± 0.3) × 10⁻²	(5.2 ± 0.4) × 10⁻²

Table 3.

Comparison of the observed and model-predicted Paβ/Hα ratios.

				Dust scattering^‡
	Observed 3 σ upper limit	Case A*	Case B^†	Silicate	Graphite
Paβ/Hα	<3.5 × 10⁻² (Main southwest)	7.6 × 10⁻²	5.7 × 10⁻²	(3.0 ± 0.3) × 10⁻²	(5.2 ± 0.4) × 10⁻²

				Dust scattering^‡
	Observed 3 σ upper limit	Case A*	Case B^†	Silicate	Graphite
Paβ/Hα	<3.5 × 10⁻² (Main southwest)	7.6 × 10⁻²	5.7 × 10⁻²	(3.0 ± 0.3) × 10⁻²	(5.2 ± 0.4) × 10⁻²

Low density limit, |$T_{\rm e}=10^4\rm \, K$| (Osterbrock & Ferland 2006).

†

|$n_{\rm e} = 10^2\rm \, cm^{-3}$|⁠, |$T_{\rm e} = 10^4\rm \, K$| (Osterbrock & Ferland 2006).

‡

Scattering efficiency from Laor and Draine (1993). A single dust size of 0.35 μm is assumed. The scattered Paβ/Hα photons originate from the Case B recombination lines from the host galaxy.

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