All Tables

Table 1: Observing log for the programme clusters. All clusters were observed on one night by O. I. Pintado (OIP), M. Netopil (MN), H. M. Maitzen (HMM) and I. Kh. Iliev (IKI).
Table 2: Summary of results; the age, distance modulus, reddening and thus the distance from the Sun was derived by fitting isochrones to the $\Delta a$ photometry. R_V was set to 3.1. For the distance of the Sun from the galactic center, a value of 8.5 kpc was used, the Trumpler classification was taken from Lyngå (1987) and the errors in the final digits of the corresponding quantity are given in parenthesis. Questionable peculiar stars are marked by asterisks (see the corresponding cluster result section for details). All photometric values are in units of mmags.
Table 3: Comparison of our results (bold face) with already published cluster parameters. The errors of the last digit are given in parentheses if available. If interstellar extinction was given in other photometric systems (* RGU, ** uvby) they were transformed to E(B-V) as described in Sect. 3. The following references, sorted by cluster and year, are given in the last column: (1) Jackson, Fitzgerald & Moffat (1980); (2) Yadav & Sagar (2002); (3) Yilmaz (1970); (4) Wramdemark (1978); (5) Fitzsimmons (1993); (6) Vogt & Moffat (1972); (7) Peterson & Fitzgerald (1988); (8) Vázquez et al. (2003); (9) Kharchenko et al. (2005); (10) Lindoff (1967); (11) Moffat & Vogt (1975); (12) Fenkart & Binggeli (1979); (13) Topatkas (1981); (14) Piatti et al. (1999); (15) Rohlfs et al. (1959); (16) Eggen (1961); (17) Talbert (1965); (18) Vleeming (1974); (19) Schneider (1985); (20) Johnson (1961); (21) Fünfschilling (1967); (22) Moffat (1972); (23) Piatti et al. (2000).
Table 4: The regression coefficients for the transformations and normality lines. The absolute values and errors vary due to the inhomogeneous "standard'' observations (photographic, photoelectric and CCD) found in the literature as well as the dependence on the magnitude range in common, i.e. a broader range guarantees a small error. The offsets are due to the four different telescopes and thus instruments as well as CCD used (Table 1), the deviating results for the slopes are discussed in the beginning of Sect. 3. The errors in the final digits of the corresponding quantity are given in parentheses.