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Table 2: Count rates for extended sources in three energy bands calculated assuming an average luminosity ( $L_{[2{-}10]\,{\rm keV}}=2.8~10^{44}$ erg/s, $T_{\rm X}=5$ keV) $\beta-$profile cluster of galaxies with a Raymond-Smith spectrum, $N_{\rm H}=5~10^{20}$ cm-2 and spectral response functions for the three EPIC detectors with thin filters
z Core radius Count-rate, photons/s
  arcsec [0.4-4] keV [0.5-2] keV [2-10] keV
0.6 32.8 0.1687 0.1316 0.0362
0.7 31.3 0.1238 0.0963 0.0253
0.8 30.4 0.0942 0.0734 0.0185
0.9 29.7 0.0737 0.0577 0.0139
1.0 29.3 0.0593 0.0465 0.0107
1.1 29.1 0.0486 0.0382 0.0085
1.2 29.0 0.0406 0.0319 0.0068
1.3 29.0 0.0343 0.0270 0.0055
1.4 29.1 0.0293 0.0231 0.0046
1.5 29.2 0.0253 0.0200 0.0038
1.6 29.4 0.0220 0.0175 0.0032
1.7 29.6 0.0193 0.0154 0.0027
1.8 29.9 0.0171 0.0137 0.0023
1.9 30.2 0.0152 0.0122 0.0020
2.0 30.5 0.0137 0.0109 0.0018



  \begin{figure*}
\mbox{\includegraphics[width=7cm,clip]{MS10417f2a.eps} \include...
...10417f2c.eps} \includegraphics[width=7cm,clip]{MS10417f2d.eps} }
\end{figure*} Figure 2: Test 1. The raw X-ray photon image with object counts for 10 ks exposure time (upper left). There are three sets of two columns of objects at separations of $15\hbox {$^{\prime \prime }$ }$ (HEW of the PSF), $30\hbox {$^{\prime \prime }$ }$ and $60\hbox {$^{\prime \prime }$ }$. The Gaussian convolution with $FWHM=12\hbox {$^{\prime \prime }$ }$ (upper right), MR/1 wavelet filtering (lower left) and WAVDETECT detection image (lower right) both with a significance threshold of 10-4 are shown


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