Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Centro Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, and observations collected at the European Southern Observatory, Chile, using FEROS spectrograph at 1.5 m telescope (proposal ID: 69.D-0338).

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http://feros.lsw.uni-heidelberg.de/docu/ferosDB/search.html

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... emission

Actually, we expect that our values of R^'_HK contain systematic errors due to stellar rotation. Lines of some of our calibrators are indeed significantly broadened by rotation; however the values of R'(HK) we derived for these stars do not differ systematically by more than 0.05 dex from the average calibration of Fig. 2.

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...1998)

Note that the [Fe/H] values given in Paper I may be slightly overestimated, due to the choice of a very low value for the microturbulent velocity.

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... HD 219542 A

The measurement of lithium of HD 219542 A of Paper I was confirmed by the independent analysis by Reddy et al. (2002).

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... data

The measurements were weighted according to their errors, when available, and assigning errors of 0.2 arcsec and 2 deg for $\rho$ and $\theta$ measurements respectively for those stars without errors bars.

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... IRAF

IRAF is distributed by the National Optical Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Fundation.

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... velocities

Comparison between pairs of observations obtained consecutively in both components suggest that the errors given by this procedure may be overestimated by about 25%, possibly because individual chunks consistently deviates by similar amounts in spectra acquired on the same night.

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... solution

The fitting was performed using the program Orbitsolver (R.E.M. Griffin, priv. comm.) that adjusts all the elements of the orbit simultaneously in a least-squares solution (Griffin & Cornell 1998).

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... confirmation

We cannot then at present confirm at a high level of confidence the announcement of a planet that some of us (the Italian part of the group) gave as a press release in November 2002.

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... observations

The second peak in Fig. 12 is at 18.5 days (a reasonable rotational period for the star). While the season 2002 data can be fitted fairly well by a sinusoidal variation with this period, the 2001 data cannot.

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...

Note that our R_HK measurement was obtained in the season for which a larger radial velocity scatter is present.

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... companion

If the planet around HD 219542 B does exist, the upper limit to the jitter estimated from residuals from the best fitting orbit, is 4.2 m s^-1, similar to HD 219542 A.

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... periods

This upper limit is justified on the basis on the detection of a planet with e= 0.93 (HD80606b, Naef et al. 2001).

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... 16 Cyg

To our knowledge, a high precision differential chemical composition analysis was not performed for HD 178911, but this would be complicated by the double line spectroscopic binarity of the primary.

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