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SUMMARY:Visibility Plane Forward Modeling of Young Massive Clusters within
  the Nuclear Ring of NGC 3351
DTSTART;VALUE=DATE-TIME:20261028T174500Z
DTEND;VALUE=DATE-TIME:20261028T175500Z
DTSTAMP;VALUE=DATE-TIME:20261026T031946Z
UID:indico-contribution-3650@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Peter Knowlton (University of Victoria)\nUsing high-
 resolution ALMA millimeter observations\, we investigate the formation of 
 massive star clusters within the nuclear ring in NGC 3351\, a nearby Milky
  Way analog galaxy. The dense\, high-pressure conditions within nuclear ri
 ngs are among the most extreme star-forming settings in the local universe
 \, providing the ideal conditions for massive cluster formation. Neverthel
 ess\, the mechanisms driving massive cluster formation and the impact of e
 nvironmental conditions remain poorly understood. They are distinct from l
 ower-mass clusters in that they form quickly and convert gas to stars effi
 ciently\, doing so before the significant onset of stellar feedback from n
 ewly formed stars. To study the full conditions of massive cluster formati
 on\, we must observe their short\, infant stages when they are actively st
 ar-forming and newborn stars remain deeply embedded in gas and dust. This 
 phase is best traced by (sub-)millimeter observations. We perform our anal
 ysis directly in the raw visibility plane using the GALARIO package to con
 vert forward models of the region into model visibilities sampled at the s
 ame baselines as our observations. This approach avoids image-plane-based 
 reconstruction methods that produce artifacts and correlated noise\, and i
 t preserves the full data resolution\, allowing us to better constrain the
  intrinsic radial profiles of the young massive clusters and the physics o
 f their star formation. Furthermore\, we can derive higher-fidelity estima
 tes and uncertainties of the shared morphology of the ring and clusters\, 
 contributing to our understanding of how gas accretion onto the nuclear ri
 ng drives massive cluster formation along its structure.\n\nhttps://nyx.ph
 ysics.mcgill.ca/event/587/contributions/3650/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3650/
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