Most stars are born in clustered environments, and the Solar system was probably not an exception. There is considerable evidence supporting this argument, including the high abundance of 26-Aluminum in short-lived radionuclides, the existence of Sedna-similar asteroids, retrograde orbiting TNOs, the tilting of the Ecliptic, and the scarred outer edge of the Kuiper belt. Some sibling cluster members may still be in the Sun's vicinity. But if our neighboring stars so strongly influenced the early Solar system, why do we have an Oort cloud? The parent cluster dissolved in the Galactic tidal field long ago, but can we find our siblings back based on their orbits in the Galactic potential or chemical composition? Those unable to attend the colloquium in person are invited to participate online through Zoom (Meeting ID: 942 0262 2849, passcode 792771) using the link: https://zoom.us/j/94202622849?pwd=dGlPQXBiUytzY1M2UE5oUDRhbzNOZz09 Prof. Portegies Zwart will be based at the ITA institute for his visit to Heidelberg and will be available for meetings by arrangement with his host, Ralf Klessen (klessen@uni-heidelberg.de).