Constraints on the gas content of the Fomalhaut debris belt - Can gas-dust interactions explain the belt’s morphology?

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Volume 574 (February 2015)

A&A, 574 (2015) L1

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Table 2

Upper limits on the total gas mass (and corresponding lower limits on the gas-to-dust ratio), the C mass and the O mass.

Abundances	M_gas	ϵ^a	M_C	M_O	e^- density		H density		N_max^d (C⁺)	N_max^d (O)
					min	max	min	max
	(M_⊕)		(M_⊕)	(M_⊕)	(cm^-3)		(cm^-3)		(cm^-2)	(cm^-2)

solar^b	< 5.0 × 10^-3	> 3.4	< 1.2 × 10^-5	< 3.2 × 10^-5	2	10	5 × 10³	5 × 10⁴	8 × 10¹⁴	2 × 10¹⁵
β Pic^c	< 5.7 × 10^-5	>298	< 1.6 × 10^-5	< 4.1 × 10^-5	6	12	8 × 10^-2	2 × 10^-1	1 × 10¹⁵	3 × 10¹⁵

Notes. The gas masses are calculated from 99% confidence level upper limits on the C ii and O i flux. We also list the range of collision partner densities and maximum column densities occurring in the models.

^(a)

Dust-to-gas ratio, using the mm dust mass M_mm = 0.017 M_⊕ derived by B12.

^(b)

Assuming solar elemental abundances.

^(c)

Assuming elemental abundances similar to the β Pic gas disc.

^(d)

Assuming a typical line width of ~2 km s^-1, the corresponding optical depths are below 10^-2.

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