Searching for the signatures of terrestrial planets in F-, G-type main-sequence stars

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Volume 552 (April 2013)

A&A, 552 (2013) A6

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Table 1

Spectroscopic observations.

Spectrograph	Telescope	Spectral range	λ/δλ	Binning	N_stars^a	\|S/N\|^b	δ \|S/N\|^c	ΔS/N^d

		[Å]		[Å/pixel]

HARPS	3.6 m-ESO	3800–6900	110 000	0.010	50	877	429	265–2015
UVES	8 m-VLT	4800–6800	85 000	0.016	7	722	150	510–940
UES	4.2 m-WHT	4150–7950	65 000	0.029	4	643	180	520–850

Notes.Details of the spectroscopic data used in this work. The UVES and UES stars are all planet hosts. Three of the UVES stars were observed with a slit of 0.3″ providing a resolving power λ/δλ ~ 110 000.

^(a)

Total number of stars including those with and without known planets.

^(b)

Mean signal-to-noise ratio, at λ = 6070 Å, of the spectroscopic data used in this work.

^(c)

Standard deviation from the mean signal-to-noise ratio.

^(d)

Signal-to-noise range of the spectroscopic data.

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