Evidence for disks at an early stage in class 0 protostars?

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Volume 606 (October 2017)

A&A, 606 (2017) A35

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Table 2

Analytical fits and physical structure.

	B1b-S		B1b-N

Size^a (′′)	0.45 × 0.43 ± 0.05		0.42 ± 0.4
PA^a (°)	25 ± 10		170 ± 10

F₀, F₁^b (mJy/beam)	66 ± 2	1.1 ± 0.4	15.3 ± 0.6	0.8 ± 0.1
r₀, r₁^b (′′)	0.34 ± 0.005	1.06 ± 0.22	0.21 ± 0.005	2.3 ± 0.5
α₀, α₁^b	6	2	4	2

n₀^c (H₂ cm^-3)	0.9 × 10¹⁰		1.0 × 10¹⁰
ρ_g^c (g cm^-3)	3.9 × 10^-14		4.3 × 10^-14
T_c^d (K)	56		41
T₀ (K)	12		12
M(r < 0.3′′) (M_⊙)	0.093		0.11
M(r < 1.0′′) (M_⊙)	0.42		0.36
M(r < 2.0′′) (M_⊙)	0.67		0.72

Notes.

^(a)

From Gaussian fitting of the ALMA images.

^(b)

The fitting formula of the circularly averaged specific distribution for B1b-S and for B1b-N uses two modified power laws: . For isothermal optically thin dust emission, the slope of the density distribution is α + 1.

^(c)

Assuming optically thin emission at 350 GHz.

^(d)

Deduced from the specific intensity assuming optically thick emission.

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