tokens: value, as many of our fitting regions do not have enough counts to constrain either or abundance. 3. TEMPERATURE MAPS Temperature maps shown in Figure 2 were derived following the method described in Markevitch et al. ( 2000 ). We extracted six narrow-band flux images between 0.8 and 9 keV, excluding the 1.7–1.9 keV edge and 7.3–7.6 keV (possibly affected by poor subtraction of the instrumental lines). Both flux and error images were smoothed prior to deriving the temperature map. A single-temperature MEKAL model was then fitted to a set of six flux values from each pixel of the image, resulting in a smoothed temperature map. The absorption column and metal abundance were fixed to the cluster best-fit values. Two smoothing methods were used, as described below. Figure 2. (a) Variable smoothing temperature map with X-ray contours. The holes in the map are masked point sources. (b) Wavelet temperature map. The fitted images were reconstructed from component wavelet scales of 6.6, 13, 26, 53, 105, and 210 kpc. 3.1. Smoothing with the Variable-width Gaussian Kernel For this approach, the narrow-band images were smoothed using a Gaussian kernel for which the width at each image pixel is determined by surface brightness in the 0.8–4 keV band, with the goal of preserving detail in bright regions. As a reference for this smoothing method, but also as a high-quality X-ray image that shows the cluster structure on all scales and omits point sources, we used wavelet reconstruction of the 0.8–4 keV image, as described in Vikhlinin et al. ( 1994 , 1998 ). We extracted wavelet components (with the atrous kernel and scales increasing in geometric progression) on scales of 53, 105, 210, and 420 kpc (or 157, 315, 630, and 126′′). Point sources are contained in wavelet components on smaller scales than the first scale above, thus not included. These image components were then co-added with the residual image smoothed by the 840 kpc scale wavelet. This procedure retains most of the statistically significant extended structures on various angular scales. The resulting image is shown in Figure 1 (b) next to the original unsmoothed image; we will use it as a reference when discussing various features in this cluster. Based on this reference image, the narrow-band images and their corresponding error images (with point sources excised) were identically smoothed by a variable-width Gaussian. By inspecting the error in the derived temperature map, we determined that using the Gaussian smoothing radius ∝ flux, and smoothing radius between 13 and 200 kpc, achieved a balance between revealing the temperature variations and suppressing noise. The resulting temperature map is shown in Figure 2 (a). To check the validity of values shown in the map, we extracted the proper spectra in a few hot spots and a cooler spot (regions T1–T4 and T5 in Figure 2 (a), respectively) and fitted their projected temperatures in XSPEC. For T1, we obtain keV; for T2, keV; for T3, we
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