Planetary detection limits taking into account stellar noise - I. Observational strategies to reduce stellar oscillation and granulation effects

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Table 1

Properties of our sample stars.

Star	M_V	Mass [M_⊙]^a	T_eff [K]^a	[Fe/H] ^a	log g^a	log()	ST	# meas.	# nights/span [days]	T_exp [s]

β Hyi	2.8	1.10	5872	–0.11	3.95	–	G2lV	2766^b	6/6	40 to 50^b
μ Ara	5.2	1.08	5780	0.30	4.27	–5.20	G3IV-V	2104^d	8/8	100^d
α Cen A	0.0	1.09	5623	0.22	4.22	–5.07	G2V	4959^c	5/5	2 to 10^c
τ Ceti	3.5	0.63	5310	–0.52	4.44	–4.93	G8V	1962^e	5/6	23 to 40^e
α Cen B	1.3	0.91	5248	0.26	4.55	–4.98	K1V	783	8/8	13

Notes. For each star, the dead time due to CCD readout is 31 s, ST is for spectral type and T_exp for exposure time.

^(a)

Sousa et al. (2008);

^(b)

Bedding et al. (2007);

^(c)

Bazot et al. (2007);

^(d)

Bouchy et al. (2005);

^(e)

Teixeira et al. (2009).

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