A potential new phase of massive star formation - A luminous outflow cavity centred on an infrared quiet core

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Table 5

Input parameters that were used for the grid of radiative transfer simulations (Bontemps et al. 2010; Palau et al. 2013; Beuther et al. 2015a; Beltrán & de Wit 2016), subdivided based on the three different model setups.

Model	Plummer core			Passive flared disc (PFD)			Cavities

		r_0,x (AU)		n₀ (cm⁻³)	r₀ (AU)	h₀	Size (AU)
Model 1	[1, 3, 6] × 10⁶	[1.5, 4.0, 10] × 10³	0.2, 0.6, 1				10⁵	[10⁰, 10², 10⁴]
Model 2	[10², 10⁴]	5 × 10⁴	1	[0.2, 0.6, 1] × 10⁷	[0.1, 0.4, 1] × 10⁴	[0.1, 0.3]
Model 3	3 × 10⁶	[0.1, 0.4, 1] × 10⁴	0.7	[0.2, 0.6, 1] × 10⁷	[0.1, 0.4, 1] × 10⁴	[0.1, 0.3]	10⁵	[10⁰, 10², 10⁴]

Notes. A combination of all of these input parameters were run. In Model 3, r_0,x of the Plummer core and r₀ of the PFD are fixed to be the same.

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