All Tables

Table 1: $\ensuremath{\langle B_z\rangle}$ measurements of the V=6.1 Ap star HD 94660 = KQ Vel. Date, UT, and signal to noise ratio (SNR) are calculated as explained in the caption of Table A.3. Observations obtained in P66 had been already published by Bagnulo et al. (2002).
Table 2: List of open clusters observed in this survey, with approximate ages (Col. 4) and distance moduli $d = \vert M - m \vert$ (Col. 5) extracted from WEBDA. Column 6 gives the number of candidate peculiar stars and Col. 7 the number of non chemically peculiar A and B stars that we observed in each cluster.
Table 3: Log of the various observing runs with FORS1 at the ESO VLT, dedicated to the open cluster survey.
Table A.1: List of Ap star candidate open cluster members. Magnitude and spectral types are taken from the General catalogue of Ap and Am stars by Renson et al. (1992), and/or from SIMBAD. In Col. 6 we report a flag about peculiarity confidence from the same catalogue. Symbol * means ``well knonw Ap star'', symbol ``?'' means ``doubtful nature''; we indicate with ``-'' the cases in which the star is not included in the Renson et al's catalogue (in which case spectral type is taken from SIMBAD or specific literature). The star's actual membership and peculiarity will be discussed in Paper II.
Table A.2: List of the observed normal cluster A and B-type stars. Actual membership has not been checked. Spectral types reported between square brackets were estimated from the star's colour indices, and should be taken with caution.
Table A.3: $\ensuremath{\langle B_z\rangle}$ measurements for chemically peculiar stars. Columns 2 and 3 give the date and UT at mid-exposure of the observation, respectively. Columns 4-6 report the $\ensuremath{\langle B_z\rangle}$ measurement from the Balmer lines, the metal lines, and the full spectrum, as explained in the text. Column 7 reports the flag for the $\ensuremath{\langle B_z\rangle}$ detection obtained from Balmer, metal lines, and full spectrum. The meaning of ``D'', ``d'', and ``n'' is explained in the text, in Sect. 7. Column 8 reports the signal to noise ratio (SNR) per Å calculated, for stars observed with grism 600B, in the wavelength interval 4975-5025Å (close to the red wing of H $\beta$ ). For stars observed with grism 600R, the SNR was calculated in the wavelength interval 6640-6690Å (i.e., close to the red wing of H $\alpha$ ). Column 9 is used to report flags and notes. Unless otherwise marked, the star was observed with grism 600B.
Table A.4: $\ensuremath{\langle B_z\rangle}$ measurements for stars not known to be chemically peculiar stars. Unless otherwise stated in the notes, the observations have been obtained with grism 600B.
Table A.5: $\ensuremath{\langle B_z\rangle}$ measurements for stars not of early spectral type.