The early evolution of young massive clusters: The kinematic history of NGC6611 / M16

In the first few Myr massive stars dynamically interact, produce runaways and affect initial binary population. Observing interpreting dynamics of young clusters is key to our understanding star formation process predicting outcome stellar evolution. We have studied NGC6611 in Eagle Nebula (M16), a cluster hosting 19 O stars. used Gaia EDR3 data determine membership, age, kinematics including runaways. The membership analysis yields 137 members located at mean distance 1706 $\pm$ 7 pc. colour - absolute magnitude diagram reveals blue red population pre-main-sequence stars, consistent with two distinct populations line earlier studies, youngest has extinction $A_V$ = 3.6 0.1 mag an age 1.3 0.2 Myr, while older 2.0 7.5 0.4 Myr. latter more spatially extended than younger generation argue that most OB belong identify 8 originating from center NGC6611, dynamical ejection scenario. show ~ 50% velocities comparable or greater escape velocity. These can be traced back kinematic ages ranging 0 2 This suggests interactions played important role early evolution which surprising considering low current density. Comparing this simulations clusters, required radius 0.1-0.5 pc not NGC6611. could initially formed wide binaries possibly harden through interactions.