All Tables

Table 1: Basic cluster parameters.
Table 2: Observation log.
Table 3: Boundaries between the shells. For each shell nr., the lower and upper radius (in arcmin) are listed.
Table 4: Spectral binning. Number of bins of 1/3 FWHM taken together in intervals E₁-E₂, in the rest frame of the cluster.
Table 5: Spectral fit results for a single-temperature model. The # indicates the shell number (cf. Table 3).
Table 6: Spectral fit results for the multi-temperature model. The temperature is the temperature of the hottest component, T₁; the emission measures Y₁ to Y₅ have been renormalised to 1 for Y₁. The # indicates the shell number. A "C" in the last column indicates consistency with an isobaric cooling flow spectrum, an "I" consistency with an isothermal spectrum.
Table 7: Spectral fit results for the multi-temperature model (continued). Same notation as Table 6.
Table 8: Constraints for the isobaric cooling flow model. The lower limit, best-fit value and upper limit are given for both $T_{\min}$ (in keV) and $T_{\min}/T_{\max}$ . Only shells with a cooling time less than 30 Gyr (as determined from the single temperature fits) are listed. No entries are listed whenever the data cannot constrain the ratio $T_{\min}/T_{\max}$ (i.e., any value between 0-1 is statistically allowed). The # indicates the shell number.
Table 9: Spectral fit results with the wdem model.
Table 10: Weighted average temperature $T_{\max}$ of the hot gas in the region with cooling time between 10-100 Gyr, and weighted average value for $1/\alpha$ for the full cluster (average is dominated by the cooling cluster core).
Table 11: Characteristic temperatures and cooling times. $T_{\rm h}$ is the temperature outside the cooling region, $T_{\rm c}$ the temperature in the center of the cluster as determined from a single temperature fit; $r_{\rm c}$ is the characteristic radius of the temperature profile (see Eq. (10); $r_{{\rm cool}}$ is the cooling radius for a cooling time of 15 Gyr and a is the power law index of the scaling of $r_{{\rm cool}}$ with cooling time (see text for details).
Table 12: Radio fluxes of the central galaxies in clusters. S_1.4 is the flux (mJy) at 1.4 GHz, $L_{\nu }$ the intrinsic luminosity at the same frequency, $\alpha$ is the radio spectral index ( $L_{\nu }\sim \nu ^{\alpha }$ ). $L_{\rm X}$ is the total 0.2-10 keV luminosity within the cooling radius $r_{{\rm cool}}$ as given in Table 11.
Table 13: Emission measure distributions for the Aschwanden & Schrijver (2002) models. $T_{\rm a}$ (keV) is the maximum temperature at the loop apex. $\Gamma$ is the loop cross section ratio between the loop apex and the photosphere. L is the loop half length (kpc), and $s_{\rm H}$ the heating scale height. M₁₃ is the cluster mass in $10^{13}~M_{\hbox{$\odot$ }}$ within the radius R (kpc) where the loop is located. Y₁-Y₅ are the emission measures Y_i (in m^-3 of the temperature components 1-5. The corresponding temperatures are T_i = T₁ / 2^i-1. The density at the loop apex is $n_{\rm a}$ (given in units of 10⁴ m^-3) and the average density over the loop volume is $\overline {n}$ . The mass of an individual loop is M_l (in $10^{10}~M_{\hbox{$\odot$ }}$ ). Finally, N is the maximum number of loops per scale height, defined by $N\equiv 4\pi R^3/V$ with V the volume of an individual loop. All calculations are done for loops with a cross-sectional radius at the foot points (r₀) of 10 kpc. For other values of r₀, the following scaling applies: $Y_i\sim r_0^2$ , $M_l\sim r_0^2$ and $N\sim r_0^{-2}$ .
Table 14: Application of the coronal loop models of Aschwanden & Schrijver (2002) to the innermost three shells of 2A 0335+096. M₁₃ is the total cluster mass in $10^{13}~M_{\hbox{$\odot$ }}$ within the radius R (kpc), for which we take the average radius of the shell. $\overline {\rho _l}/\rho _{{\rm tot}}$ is the average mass density of the loops divided by the total mass density of the cluster (including dark matter etc.). The total mass density profile was taken from Ettori et al. (2002). In this table, f is the volume filling factor of the loops.
Table A.1: Distribution of the observed flux, expressed as a percentage of the original flux emitted in a given annulus. Calculation applies to the MOS1 data of A 1795. The observed flux is corrected for vignetting, psf and exposure map. The column o labels the observed annulus number, the row ethe emitting annulus.