Combination of radio (MeerKAT; 1.3 GHz, red) and X-ray (Chandra; 2.3−8 keV, Log scale, smoothed with σ = 0.5″ Gaussian, green) images of the G0.13−0.11 region in Galactic coordinates. The cyan lines show the constraints on the polarization angle (PA) of the G0.13−0.11 emission derived from the IXPE data (best-fitting value ±1σ error; i.e., 21 ± 9°). The prominent red vertical threads on the left side of the image belong to the NTFs of the Radio Arc. G0.13−0.11 is the green feature to the east of a sequence of fainter NTFs near the center of the image. G0.13−0.11 consists of (i) a compact core (the bright green dot at the center of the figure; presumably the pulsar itself and its PWN); (ii) a pair of bright “wings”; and (iii) a more diffuse (possibly structured) X-ray glow to the left of the “wings” (at higher Galactic longitude). The polarization direction is approximately perpendicular to the X-ray “wings” and the nearest NTFs. Coupled with the large polarization degree, this proves that X-rays are produced by synchrotron emission of ∼TeV electrons.