Astronomy & Astrophysics

All Tables

Table 1: Description of the used photometric data sets. The filter name, the number of exposures and the total integration time (in seconds) are given.
Table 2: The photometric data for the twelve most isolated white dwarfs in NGC 6752 in the Vega-based HST flight system.
Table 4: Fitting the photometry of the twelve most isolated white dwarfs in NGC 6752 with ${T_{\rm eff}}$ and $\log~{g}$ as free parameters, (m-M)₀ fixed at $\rm 13\hbox{$.\!\!^{\rm m}$ }05$ and $\rm 13\hbox{$.\!\!^{\rm m}$ }20$ . E_B-V assumed as $\rm 0\hbox{$.\!\!^{\rm m}$ }04$ .
Table 5: Fitting the white dwarf spectra in NGC 6752 with $\log~{g}$ held fixed at 7.84. ${T_{\rm eff,ph}}$ is the result from the photometry for (m-M)₀ = $\rm 13\hbox{$.\!\!^{\rm m}$ }20$ .
Table 6: Fitting the white dwarf spectra in NGC 6397 with $\log~{g}$ held fixed at 7.84. ${T_{\rm eff,ph}}$ is the effective temperature estimated from VI photometry by Moehler et al. (2000). We also give M_V from the model fit (assuming a thick hydrogen layer), the observed V corrected for a reddening of E_B-V = $\rm 0\hbox{$.\!\!^{\rm m}$ }18$ , and the derived distance modulus.
Table 7: Results for the brightest object in NGC 6397 with $\log~{g}$ as free parameter. We also give M_V from the model fit (assuming a thick hydrogen layer), the observed V corrected for a reddening of E_B-V = $\rm 0\hbox{$.\!\!^{\rm m}$ }18$ , and the derived distance modulus.
Table 3: Observational parameters for the spectroscopic data. On August 10, 2001, the seeing monitor did not work and the seeing was estimated from the acquisition and through-slit images.