With a hyperbolic trajectory around the Sun , ‘ Oumuamua is the first confirmed interstellar object . However , its origin is poorly known . By simulating the orbits of 0.23 million local stars , we find 109 encounters with periastron less than 5 pc . ‘ Oumuamua ’ s low peculiar velocity is suggestive of its origin from a young stellar association with similar velocity . In particular , we find that ’ Oumuamua would have had slow encounters with at least five young stars belonging to the Local Association thus suggesting these as plausible sites for formation and ejection . In addition to an extremely elongated shape , the available observational data for ‘Oumuamua indicates a red colour suggestive of a potentially organic-rich and activity-free surface . These characteristics seem consistent with formation through energetic collisions between planets and debris objects in the middle part of a young stellar system . We estimate an abundance of at least 6.0 \times 10 ^ { -3 } au ^ { -3 } for such interstellar objects with mean diameter larger than 100 m and find that it is likely that most of them will be ejected into the Galactic halo . Our Bayesian analysis of the available light curves indicates a rotation period of 6.96 _ { -0.39 } ^ { +1.45 } h which is consistent with the estimation by [ ] and shorter than other literature . The codes and results are available on \href https : //github.com/phillippro/OumuamuaGitHub .