All Tables

Table 1: Residuals between datasets from different sources. These are given as X₂-X₁ where X is the studied variable from the data sources 1 and 2.
Table 2: "Inside correlations'' between gradients from various sources, used in the estimation of probable errors in each dataset. The impartial correlation Y=pX+a is given.
Table 3: Estimated mean errors in UBVRI gradients for various datasets.
Table 4: Parameters of the colour gradients distributions.
Table 5: "Inside correlations'' between gradients from new and merged data. The relation Y=pX+a is given (taking errors in account).
Table 6: Relative gradients, observed and calculated: $\Delta _{BV}$ is taken as unit.
Table 7: Comparison of average values of colour gradients for our full sample and for the Pec subsample of morphologically peculiar objects (Michard & Prugniel 2004). Among Pec objects we distinguish the YP family with evidence for the presence of some young stars and the NP family with no such evidence.
Table 8: Mean colour gradients for the subtypes of ellipticals, respectively diE and boE. The unE are always intermediate. The S0 NGC 5866 was rejected.
Table 9: Comparison of average values of colour gradients for the subsample IR₀ of objects with zero IRAS 100 $\mu$ flux and the subsample IR₁ of objects with non zero flux (Knapp et al. 1989).
Table 10: Estimates of the diffuse dust content in the Tau(V) scale defined by models in Witt et al. (1992, Wal92), using the correlations $\Delta _{VK}-\Delta _{UB}$ , $\Delta _{VJ}-\Delta _{UB}$ , $\Delta _{VK}-\Delta _{BV}$ , and $\Delta _{VJ}-\Delta _{BV}$ (see Sect. 4.2). Doubtfull cases are noted with a colon.