Left panel: 0.3–5 keV Chandra image of the J2055 field. The image has been smoothed with a Gaussian filter. Central panel: graphical representation of the results of the imaging analysis presented in Sect. 3.4. Each box has a count distribution that varies significantly (3σ) from the adjacent distributions. The box thickness contains 95% of the background counts, as from Gaussian describing the distribution. The box intensity is the best-fitted (background-subtracted) counts density within the box. The pulsar position is indicated by a cyan X. We also report a sample of the distributions described in Table 1, where the distance orthogonal to the main axis of the nebula is on the x-axis and on the background-subtracted nebular counts is on the y-axis. Right panel: graphical representation of the results of the MRHT analysis presented in Sect. 3. Each cyan vector is the best-fitted maximum of a distribution significantly (3σ) different from the adjacent distributions. Dotted green lines show the 1σ error on the associated vector. The pulsar position is denoted by a cyan X. As for the central panel, we report a sample of the distributions described in Table 1, where the angle of significant segments from MRHT is on the y-axis.