All Tables

Table 1: Summary of the observations taken during 4-13 July, 2002 in Hawaii, San Pedro Màrtir, Loiano and from 9-17 July, 2001 in La Palma (by B03).
Table 2: The observing window relative to the July 2002 observations. The last line shows the total number of observing hours for each site.
Table 3: The observing window relative to the July 2001 observations.
Table 4: Adopted parameters for the BLS algorithm: nf is the number of frequency steps adopted, fmin is the minimum frequency considered, df is the increasing frequency step, nb is the number of bins in the folded time series at any test frequency, qmi and qma are the minimum and maximum fractional transit length to be tested, as explained in the text.
Table 5: The different cases in which the data-sets analysis was splitted into. The notation in the first column is explained in the text, the second column shows the number of stars in each case and the third column refers to the DSP values assumed, correspondent to a FAR = $0.1\%$ .
Table 6: The candidates found in the two cases discussed in Sect. 8. The case of the whole data-sets put together is indicated with ALL (1st column), that one for the onlyCFHT data-set is indicated with CFHT (2nd column). A cross (x) indicates that the candidate was found in that case, a trait (-) that it is absent. In the 3rd column, the ID of the stars taken from S03 is shown. Follow the V calibrated magnitude, the (B-V) color, the right ascension, ( $\alpha$ ), and the declination, ( $\delta$ ), of the stars.
Table 7: The Table shows the results of our simulations on the expected number of detectable transiting planets for the whole data-set (all the cases of Table 5) as explained in Sect. 10.3. $N_{\rm geom}$ indicates planets with favorable inclination for transits, N₁₊, and N₁, planets that transit respectively at least one time and only one time inside the observing window. R¹, R², R³, indicate the expected number of detectable transiting planets inside our observing window, for the three assumed planetary radii distributions, (see Sect. 7.3.2).
Table 8: The same as Table 7, but for the case of the only CFHT data as explained in Sect. 10.2.
Table 9: Number of nights and hours which have been devoted to the study of NGC 6791 as a function of the diameter of the telescope used for the survey. We adopted a mean of 5 hours of observations per night.