tokens: 0.2 and 10.0 . Although one of the main problems of this survey was the poor and sparse sampling and the small number of observations per star, which complicates the statistical analysis and increases the uncertainty on the frequency of Jupiters in our survey, we find a total occurrence rate of Jupiter-mass planets in the M 67 sample of 18.0% (precisely 15.8% for the MS stars and 23.0% for the evolved stars). It is worth noting that on average we need a minimum number of 20 observations per star to exclude Jupiter-mass planets at high confidence when a periodogram analysis is applied. The Jupiter-mass planets in our sample imply that our results are consistent with the planet frequency of much larger surveys carried out for field star samples. For example, from the ELODIE survey, Naef et al. (2005) estimated that a fraction of 7.5 1.5% stars host giant planets with periods shorter than 10 yr, while Cumming et al. (2008) derived a frequency of 12 1.6% from the Keck survey and Mayor et al. (2011) 13.9 1.7% from the HARPS/CORALIE survey. As a general conclusion, our simulation study seems to confirm the recent finding ( Meibom et al. 2013 ) that the frequency of massive planets around stars of open clusters agrees with the frequency of these planets around field stars. However, we note that when we only investigate the frequency of hot Jupiters around MS stars of our survey, we find a hot Jupiter occurrence rate (5.7%) that is substantially higher than what is observed in field stars (see also Brucalassi et al. 2016 ). We have shown that the search for planets in open clusters is a powerful test benchmark for the theory of planet formation and stellar evolution. The new generation of spectrographs such as ESPRESSO ( Pasquini et al. 2009 ) will extend this search more effectively. It is clear, however, that to efficiently perform a planet search survey in star clusters, a multi-object capability, even with relatively low multiplex (10–50), is desirable. Unfortunately, no such facility is currently planned. Appendix A: Accompanying plots and table Table A.1 Observed targets in M 67. Notes. Object name, basic stellar parameters, number of observations for each instrument (H: HARPS, S: SOPHIE, C: CORALE, HET: HRS at Het, H-N: HARPS-N), total number of observations, mean stellar RV, average measurements error, average corrected measurements error, observed RV dispersion. Binary candidates are indicated in bold face. Fig. A.1 Contours of the planet detection efficiency for the MS stars in the domains of 1–1000 days for planet period and 0.2–10 for planet mass. A 0.01 FAP level has been used as detection planet threshold in the periodogram analysis. A filled circle indicates the planet position. Fig. A.2 Contours of the planet detection efficiency for the evolved stars in the domains of 1–1000 days for planet period and 0.2–10 for planet mass. A 0.01 FAP level has been used as detection planet threshold in the periodogram analysis. A filled circle
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