Extended Data Fig. 1: Diffuse Galactic Centre X-ray emission at different scales. | Nature

Extended Data Fig. 1: Diffuse Galactic Centre X-ray emission at different scales.

From: An X-ray chimney extending hundreds of parsecs above and below the Galactic Centre

Extended Data Fig. 1

a, ROSAT (0.9–2-keV energy band) large-scale map of the Galactic Centre. The X-ray counterparts of the Fermi bubbles are strong X-ray emitters. The edges (white ellipses) are clearly detected on scales of several degrees, whereas they become confused (because of the short exposure of 200–300 s and soft X-ray energy band) close to the plane. The red dashed line indicates the XMM-Newton area covered by our survey. b, XMM-Newton map zooming into the central degrees of the Milky Way. The magenta dashed line intersects both chimneys, passing through Sgr A*. The map shows the X-ray emissivity within the 1.5–2.6-keV energy band (see Extended Data Fig. 2). c, Schematic view of the main diffuse X-ray-emitting features within the central 500 pc or so from Sgr A*. The red star and the yellow ellipses indicate the position of Sgr A* and of Sgr A’s ±15-pc bipolar lobes. The large violet ellipses indicate the location and extension of the X-ray counterpart of the Galactic Centre lobe with shell-like morphology (the northern chimney), of its eastern protrusion and of its roughly symmetric southern counterpart (the southern chimney). The orange filled ellipse, the two red circles and the red ellipse indicate the location of the Arc super-bubble (SB), the Quintuplet and Arches clusters and the super-bubble candidate G359.77–0.09 (ref. 8). The pink regions indicate the location of the edges to the Fermi bubbles. The dotted circles and solid ellipses indicate the position of bright X-ray sources with intense dust-scattering halos (DSH) and known supernova remnants (SNR). d, Chandra RGB map zooming into the central tens of parsecs of the Galaxy. The ±15-pc lobes are clearly visible (orange). The dashed circles have radii of 1 pc, 5 pc and 15 pc.