All Tables

Table 1: Results from the spectral fitting in concentric annular regions in the [0.4/0.9-10.0] keV energy range (MOS/pn) and in the [1.0-10.0] keV energy range. Temperatures (kT) are in keV, metallicities (Z) in solar units and [2-10] keV luminosities ( $L_{\rm X}$ ) in units of $10^{44}~\mbox{erg~s}^{-1}$ . The total $\chi ^2$ values and numbers of degrees of freedom (d.o.f.) in the fits are also listed. Error bars are at the 90% confidence levels on a single parameter of interest.
Table 2: The best-fit parameter values and 90% confidence limits from the spectral analysis in the central $0\hbox {$.\mkern -4mu^\prime $ }6$ region. Temperatures (kT) are in keV, metallicities (Z) as a fraction of the solar value and normalizations in units of $10^{-14} n_{\rm e} n_{\rm p} V / 4 \pi [D_{\rm A} (1+z)]^2$ as done in XSPEC (for the MKCFLOW model the normalization is parameterized in terms of the mass deposition rate $\dot{M}$ , in ${M}_{\odot}~\mbox{ yr}^{-1}$ ).
Table 3: Characteristics of the co-added WFI images. The limiting magnitudes quoted in Col. 4 are defined in the Vega system via $m_{\rm lim}=ZP-2.5\log(\sqrt{N_{\rm pix}}\cdot 3\cdot\sigma)$ , where ZP is the magnitude zeropoint, $N_{\rm pix}$ is the number of image pixels in a circle with radius $2\hbox{$.\!\!^{\prime\prime}$ }0$ and $\sigma$ the sky background noise. The seeing in Col. 5 was measured with the SExtractor FWHM_IMAGE parameter. The groups in Bonn (B) and Innsbruck (I) observed Z3146 with an offset of about $5\hbox {$.\mkern -4mu^\prime $ }0$ In Ra and $8\hbox {$.\mkern -4mu^\prime $ }0$ in Dec. The exact layout is given in Fig. 8. For the R band we created, besides the individual stacks, a deep mosaic in the common area (A). We note that the Innsbruck R band has nearly double the exposure time of the Bonn image but about the same limiting magnitude as it was observed during less favourable moon phases. The quality of our photometric calibration is crosschecked in Fig. 9.
Table 4: Table of the arc candidates shown in Fig.19. "cc'' denotes the cluster centre, the length-to-width ratio l/w is calculated with the help of $\lambda _1$ , and $\lambda _2$ (the second order moments of the light distribution) and is measured on the WFPC2 images as it is not affected by atmospheric blurring. A value of =0.75 was chosen for both, the DETECT_THRESH and ANALYSIS_THRESH due to the shallowness of the image. The magnitudes are instrumental WFI magnitudes in the Vega system. All objects are photometrised using SExtractor'sMAG_AUTO.
Table 5: Photometric properties of the arc candidates and their possible counter images. See Sect. 5.2.4 for more details and discussions.
Table 6: Details of the catalogues, K-corrections values and the Schechter function parameters $\phi ^*$ , $\alpha$ and M^* for the three WFI filters. F is the fraction of light which is missing due to the limiting magnitudes $M_{\rm lim\it }$ of the catalogue given in Table 3. For the R band we used the limiting magnitude for region A (see Table 3). See text for more details. The Luminosity distance is 1.5 Gpc (distance modulus m-M=40.88 at z=0.2906).