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We study the origin of the interstellar object 1I/2017 U1 'Oumuamua byjuxtaposing estimates based on the observations with simulations. We speculatethat objects like 'Oumuamua are formed in the debris disc as left over from thestar and planet formation process, and subsequently liberated. The liberationprocess is mediated either by interaction with other stars in the parentalstar-cluster, by resonant interactions within the planetesimal disc or by therelatively sudden mass loss when the host star becomes a compact object.Integrating backward in time in the Galactic potential together with stars fromthe Gaia-TGAS catalogue we find that about 1.3Myr ago 'Oumuamua passed thenearby star HIP 17288 within a mean distance of $1.3$pc. By comparing nearbyobserved L-dwarfs with simulations of the Galaxy we conclude that thekinematics of 'Oumuamua is consistent with relatively young objects of$1.1$--$1.7$Gyr. We just met 'Oumuamua by chance, and with a derived meanGalactic density of $\sim 3\times 10^{5}$ similarly sized objects within100\,au from the Sun or $\sim 10^{14}$ per cubic parsec we expect about 2 to 12such visitors per year within 1au from the Sun.

The origin of interstellar asteroidal objects like 1I/2017 U1 'Oumuamua