All Tables

Table 1: Journal of observations. Phases $\phi$ refer to the ephemeris of WR20a (Rauw et al. 2007).
Table 2: Properties of candidate late-O stars. The last two lines reproduces the data of two eclipsing binaries (from Rauw et al. 2007).
Table 3: Properties of the early-type stars in the optical and X-ray domains. Background- and exposure-corrected source fluxes (in 10^-5 photons cm^-2 s^-1) are estimated for each observation from the fluxed images in a region of radius r (in px) and for the 0.3-10. keV band. The last columns give the average hardness ratios and dereddened X-ray luminosity in 10³² erg s^-1 and for the 0.5-10. keV energy band (see text for details). A colon (:) indicates an uncertain value.
Table 4: Best-fitting models and X-ray fluxes at Earth for the brightest early-type stars in Westerlund 2. For each parameter, the lower and upper limits of the 90% confidence interval (derived from the ERROR command under XSPEC) are noted as indices and exponents, respectively. The normalisation factors are defined as $10^{-14}\int n_{\rm e} n_{\rm H} {\rm d}V/4\pi D^2$ , where D, $n_{\rm e}$ and $n_{\rm H}$ are respectively the distance to the source (8 kpc), the electron and proton density of the emitting plasma. Abundances were fixed to solar except for the WR stars (for more details, see text).
Table 5: Spectral analysis of the flaring PMS candidates, ordered by RA. Columns 2 and 3 yield the coordinates (J2000) of the sources, whilst the fourth column indicates the number of the observation during which the flare occured. Columns 5-9 list the best fit parameters of the spectral fits with a wabs $\times$ mekal model. For each parameter, the lower and upper limits of the 90% confidence interval are noted as indices and exponents, respectively. Finally, Col. 10 yields the 1/e decay time of the flare; $kT_{\rm max}$ is the maximum plasma temperature during the flare (derived from the fitted ${\it kT}$ ) and l is the loop half-length.