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We present the first results of applying Gaussian Mixture Models in thestellar kinematic space of normalized angular momentum and binding energy onNIHAO high resolution galaxies to separate the stars into multiple components.We exemplify this method using a simulated Milky Way analogue, whose stellarcomponent hosts: thin and thick discs, classical and pseudo bulges, and astellar halo. The properties of these stellar structures are in good agreementwith observational expectations in terms of sizes, shapes and rotationalsupport. Interestingly, the two kinematic discs show surface mass densityprofiles more centrally concentrated than exponentials, while the bulges andthe stellar halo are purely exponential. We trace back in time the Lagrangianmass of each component separately to study their formation history. Between z~3and the end of halo virialization, z~1.3, all components lose a fraction oftheir angular momentum. The classical bulge loses the most (~95%) and the thindisc the least (~60%). Both bulges formed their stars in-situ at high redshift,while the thin disc formed ~98% in-situ, but with a constantSFR~1.5M$_{\rm\odot}$/yr$^{\rm-1}$ over the last ~11 Gyr. Accreted stars (6% oftotal stellar mass) are mainly incorporated to the thick disc or the stellarhalo, which formed ex-situ 8% and 45% of their respective masses. Our analysispipeline is freely available at https://github.com/aobr/gsf.

Introducing galactic structure finder: the multiple stellar kinematic structures of a simulated Milky Way mass galaxy