All Tables
- Table 1:
Selected XMM-Newton energy bands.
- Table 2:
Correlation coefficients of the CCD contamination rates as defined
in Sect. 5 vs. the observation parameters listed in the left column of the
table. The last row shows the critical value of a the statistical test for the significance of the correlation coefficient of the sample at a 95% confidence
level adopted from Crow et al. (1960). We shown the 99% confidence level value in parenthesis. Note that the zero correlation is only rejected with the values of the CCD2 column.
- Table 3:
Summary of the observations extracted from the XMM-Newton Science Archive for our investigation of the XMM-data reduction. This table shows observations performed with the thin filter. The fourth column shows the total column densities derived from the newest all-sky stray-radiation corrected 21-cm line surveys (Kalberla et al., submitted). The
columns show the total integration time of the observation for the MOS and pn instruments. The
columns show the effective time after proton flare filtering (see Sect. 3.2) for each observation in MOS1, MOS2 and pn as indicated. The accumulated integration time of the thin filter sample is
for MOS and
for pn. The accumulated effective time amounts to
for MOS and
for pn.
- Table 4:
Like Table 3 for the case of the observations with the medium filter. The accumulated integration time of this sample is
for MOS and
for pn. The accumulated effective time amounts to
for MOS and
for pn.
- Table 5:
Like Table 3 for the case of the observations with the thick filter. The accumulated integration time of this sample is
for MOS and
for pn. The accumulated effective time amounts to
for MOS and
for pn.
- Table 6:
Summary of of our sample of pointings performed with XMM-Newton (see also Table 3). The directions of the pointings have been specifically selected to study the contribution of the SXRB as seen by XMM-Newton.