Disc kinematics and stability in high-mass star formation - Linking simulations and observations

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Table 1

Details of synthetic observations.

Interferometer	Distance	Synthesised beam	Linear resolution	Continuum rms^(a)	Line rms^(b)
	(pc)	(′′×′′, PA)	(au)	(mJy beam⁻¹)	(mJy beam⁻¹)
ALMA	800	0.09′′× 0.06′′, 88°	60	0.25	0.17
ALMA	2000	0.07′′× 0.06′′, 90°	130	0.06	0.04

NOEMA	800	0.44′′× 0.34′′, 44°	312	0.60	1.08
NOEMA	2000	0.44′′× 0.34′′, 44°	780	0.54	0.78

Notes. Values are averages for 10°, 30°, 60°, and 80° inclinations. ^(a) The rms noise in the emission-free region. ^(b)The rms noise in the emission-free region in the channel that has the peak of emission for CH₃ CN (12₄−11₄); therefore, the unit is per 0.35 km s⁻¹ channel.

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