XMM-Newton/MOS1 (left column) and MOS2 (right column) images of Sgr A* on 2014 Mar. 10. The energy range is 2–10 keV. The field of view is 20″ × 20″, the pixel size is . The same linear color-scale is used for panels a)–f) and g)–h). In all panels, the black circle in the right-bottom corner is the instrument angular-resolution (FWHM); the crosses are the positions of SGR J1745-2900 (Bower et al. 2015b) and Sgr A* (Petrov et al. 2011), surrounded by a circle giving the absolute-astrometry uncertainty of EPIC (; Guainazzi 2013). Panels a) and b): count numbers observed during the flaring period. Panels c) and d): count numbers observed during the non-flaring period scaled-down to the flaring-period exposure. The contour map shows count numbers smoothed on four pixels with a Gaussian, starting from 2 counts with step of 1 count. Panels e) and f): count excesses during the flaring period. Panels g) and h): statistically significant count excesses (≥ 3σ; computed on the boxed-pixel area with the Bayesian method of Kraft et al. 1991), the diamond is the corresponding count-weighted barycenter of these detections.