Mass assembly from clouds to clusters

The process by which stars within clusters assemble their mass is incredibly important but currently not very well understood.  While recent surveys of the Galactic Plane have identified a large number of dense, massive clouds where the next generation of cluster formation will likely occur, progress in understanding the process by which clusters form has been limited primarily due to the lack of angular resolution and sensitivity of the observations.

Only with observations of the natal gas and dust in a cluster-forming clump well before the onset of star formation can we begin to understand the process by which the material is transferred from the large reservoir within a cloud onto protostellar cores and ultimately the stars. Fortunately, by combining the revolutionary capabilities of ALMA with new and existing facilities such as Mopra, LMT, GBT, CARMA, SMA, PdBI and the JVLA, we can obtain the necessary observations, allowing us to observe the small-scale processes and, for the first time, test cluster formation scenarios. To achieve and make progress we need to bring together theorists and observers to coordinate our efforts to achieve our common goals.

This will be a small workshop (~40 people) on the topic of Galactic cluster formation. This meeting is timely: results already coming from ALMA and those expected in the next 12 months are revolutionizing the field of Galactic cluster formation. We are poised to make significant progress in this field in the next decade. As such, one of the key outcomes of this meeting is to identify the most important science questions related to cluster formation that both theory and observations can answer. To help achieve this goal, we will dedicate at least one day to a discussion of analysis tools that can turn the simulations into observable quantities that we can directly compare to data.

Key topics

1. Observations of the large scale mass assembly: formation and early evolution of protocluster clouds
2. Observations of the small scale mass assembly: infall, outflow, and feedback
3. Current theory and simulations of cluster formation
4a. Techniques and tools for directly comparing simulations with observations
4b. ALMA for theorists
5. Focusing and coordinating our efforts: identifying the big questions