Nulling interferometry: impact of exozodiacal clouds on the performance of future life-finding space missions

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Volume 509 (January 2010)

A&A, 509 (2010) A9

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Table 3:

Detailed view of the various contributors to the noise budget, given in photo-electrons persecond over the 6-20 $\mu$ m wavelength range for D ARWIN/TPF in the Emma X-array configuration.
	M0V - 05pc	K0V - 10 pc	G2V - 15 pc	F0V - 20 pc
Optimum baseline [m]	25	22	22	11
Planetary modulation efficiency	0.57	0.58	0.58	0.58
Planetary coupling efficiency	0.76	0.76	0.76	0.75
Stellar signal [e-/s]	$2.6 \times 10^7$	$2.1 \times 10^7$	$1.3 \times 10^7$	$2.1 \times 10^7$
Planetary signal [e-/s]	5.52	1.39	0.62	0.35
Photon noise [e-/s]	0.459	0.388	0.358	0.365
- Geometric leakage [e-/s]	0.304	0.179	0.101	0.078
- Null-floor leakage [e-/s]	0.019	0.017	0.013	0.017
- 3-zodi signal [e-/s]	0.077	0.078	0.075	0.121
- Local zodiacal signal [e-/s]	0.260	0.260	0.260	0.260
- Detected thermal [e-/s]	0.101	0.101	0.101	0.101
- Detected stray light [e-/s]	0.166	0.166	0.166	0.166
Dark current [e-/s]	0.063	0.063	0.063	0.063
Detector noise [e-/s]	0.063	0.063	0.063	0.063
Instability noise [e-/s]	0.025	0.014	0.008	0.012
- First order phase term [e-/s]	0.021	0.008	0.002	0.001
- Second order phase-amplitude [e-/s]	0.014	0.012	0.007	0.012
Total noise [e-/s]	0.460	0.388	0.358	0.365
Integrated SNR (one rotation)	16.0	4.4	2.1	1.1
Integration time for SNR = 5 [h]	1.36	17.9	81.8	285

The final SNRs are computed over a single rotation of 50 000 s and for four targets representative of the target catalogue (see main text for further information).

Source LaTeX | All tables | In the text

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