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tokens: et al. 2005 ; Helder et al. 2011 , 2013 ), although Shimoda et al. ( 2015 ) suggested the measured efficiency could be higher than reality. It is noteworthy that the thermal and nonthermal emission in this SNR is not uniform and has different morphology, which makes this SNR a suitable laboratory to test a possible relation between the acceleration efficiency and the environment. In this paper, we present the systematic analysis of spatially resolved spectra obtained with the X-ray Imaging Spectrometer (XIS: Koyama et al. 2007 ) on board Suzaku (Mitsuda et al. 2007 ). Unless otherwise noted the uncertainty is given at the 90% confidence interval. 2. OBSERVATION AND DATA REDUCTION The entire region of RCW 86 is covered by six observations with Suzaku . The observation log is summarized in Table 1 . The fields of views (FoVs) are shown in Figure 1 with the dashed squares. Figure 1. The XIS image of RCW 86 in a logarithmic scale. Red and blue, respectively, show emission from 0.5–2.0 keV (soft) and 3.0–5.5 keV (hard). The FoVs of XIS are indicated by the dashed squares. They are EAST (cyan), SE (green), SOUTH (blue), SW (orange), WEST (magenta), and NORTH (red). The solid-white shapes are source regions, while the dashed-white shapes are background regions in each FoV. The white and black numbers in the SW region represent SW-A and SW-B regions, as shown in the main text. Table 1 Suzaku Observations of RCW 86 The XIS consists of four X-ray CCD cameras, which observe in 0.2–12.0 keV with X-ray telescopes (XRT: Serlemitsos et al. 2007 ). Three of them (XIS 0, 2, and 3) are front-illuminated (FI) CCDs, and the other (XIS 1) is a back-illuminated (BI) CCD. The FI CCDs have larger effective area in the hard X-ray band while the BI CCD is in the soft band. A pre-flight energy resolution is ∼130 eV (full width at half maximum, FWHM) at 5.9 keV (Koyama et al. 2007 ). After 2006 November 9, the XIS 2 was out of operation. The others (XIS 0, 1, and 3) use spaced-row charge injection (SCI: Nakajima et al. 2008 ; Uchiyama et al. 2009 ) to recover the charge transfer efficiency and improve the energy resolution after 2006 October. Each XRT accumulates X-rays with the effective area of 250 cm 2 at 8.0 keV to make an image over an FoV with angular resolutions of – in the half-power diameter. Thanks to the low-Earth orbit, the non-X-ray background (NXB) is fairly low and stable. Thus, Suzaku is very suitable for RCW 86, with its large extent and low surface brightness in some regions. We reprocessed the data using the xispi software and the recent calibration database released on 2012 May 9. The data were reduced in accordance with the standard screening criteria. 6 6 see ( http://heasarc.nasa.gov/docs/suzaku/processing/criteria_xis.html ). Grades 0, 2, 3, 4, and 6 events were used in the following analysis. We removed events during the South Atlantic Anomaly passages, Earth elevation angles below 5°, and Earth day-time elevation angles below 20°. We also