Table A.1:

Limiting rms OPD values computed for a G2V star located at 15 pc such that shot noise dominates instability noise by a factor 5.

[nm]	2-m apertures						4-m apertures
			m		m				m			m
		DCB	X-ar2	X-ar6	DCB	X-ar2	X-ar6	DCB	X-ar2	X-ar6	DCB	X-ar2	X-ar6
White noisea	0.01%	>50	>50	>50	>50	>50	>50	>50	>50	>50	>50	>50	>50
	0.05%	16	9.5	9.5	>50	>50	>50	6.5	4.6	4.6	23	16	16
	0.10%	2.4	1.0	1.0	5.3	4.8	4.8	0.8	0.5	0.5	3.7	2.9	2.9
1/f noiseb	0.01%	0.7	2.6	4.2	2.8	13	19	0.4	1.1	1.9	1.1	3.6	5.6
	0.05%	0.7	0.9	1.5	2.0	2.9	4.1	0.3	0.4	0.6	0.8	0.9	1.4
	0.10%	0.5	0.5	0.7	1.5	1.6	2.0	0.3	0.3	0.3	0.5	0.5	0.6

^a rms values is defined on the [0-10 Hz] wavelength range; ^b rms values is defined on the [1/ -10⁴ Hz] wavelength range. The results are given at 7 m and 10 m, assuming a spectral resolution of 20, for different rms amplitude mismatches and shapes of the instability noise power spectrum. Three configurations are shown, the X-array with an aspect ratio of 2 (X-ar2), the X-array with an aspect ratio of 6 (X-ar6) and the Dual Chopped Bracewell (DCB, configuration used in Lay 2004).