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450 years after the explosion of the Type Ia SN1572, the dynamics of theTycho supernova remnant can give us keys to understand the explosion mechanismand the interaction of the remnant with the interstellar medium. To probe theasymmetries and the evolution of the SNR, we track the ejecta dynamics usingnew methods applied to the deep X-ray observations available in the Chandraspace telescope archive. For the line of sight velocity measurement Vz, we usethe Doppler effect focused on the bright Si line in the 1.6-2.1 keV band. Usingthe component separation tool General Morphological Component Analysis (GMCA),we successfully disentangle the red and blueshifted Si ejecta emission. Thisallows us to reconstruct a map of the peak energy of the Si line with a totalcoverage of the SNR at a 2'' resolution and a proxy of the velocity in the lineof sight. For the proper motions in the plane of the sky Vxy, we develop a newmethod, named Poisson Optical Flow, to measure the displacement of 2D featuresbetween the observations of 2003 and 2009. The result is a field of 1700velocity vectors covering the entire SNR. These exhaustive 3D velocitymeasurements reveal the complex and patchy dynamics of the SNR. At thelarge-scale, an asymmetry with the North being dominantly blueshifted and theSouth redshifted is observed. The proper motion vector field Vxy highlightsdifferent dynamics between the East and the West parts of the SNR. The easternvelocity field is more disturbed by external inhomogeneities and the South-Eastejecta knot. In particular, a slow-down is observed in the North-East whichcould be due to the interaction with higher densities as seen in otherwavelengths. The vector field is also used to backtrace the center of theexplosion which is then compared with potential stellar progenitors distancesfrom the latest Gaia DR3, leaving only stars B and E as possible candidates.

A fresh perspective on the 3-D dynamics of Tycho's supernova remnant: ejecta asymmetries in X-rays