Velocity Structure of the Orion A Integral Shaped Filament
Star formation is fundamental for the processes of planet formation and galaxy evolution. Here we present an analysis of the gas kinematics of the ISF, a massive filament hosting a young embedded cluster, in the Orion A cloud through observations of different molecular transitions. We derive kinemat...
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| Tipo de recurso: | tesis de maestría |
| Estado: | Versión publicada |
| Fecha de publicación: | 2019 |
| País: | Chile |
| OAI Identifier: | oai:repositorio.anid.cl:10533/237599 |
| Acceso en línea: | https://hdl.handle.net/10533/237599 |
| Access Level: | acceso abierto |
| Palabra clave: | Ciencias Naturales Ciencias Físicas Astronomía |
| Sumario: | Star formation is fundamental for the processes of planet formation and galaxy evolution. Here we present an analysis of the gas kinematics of the ISF, a massive filament hosting a young embedded cluster, in the Orion A cloud through observations of different molecular transitions. We derive kinematic parameters to construct intensity-weighted position-velocity diagrams and non-thermal velocity dispersion radial profiles of the filament. The radial velocity structure of the filament presents a velocity gradient that terminates with a blue-shifted velocity peak near the center of the cluster. The global velocity structure is consistent with the wave-like appearance of the filament, and we also report the presence of small velocity fluctuations along the filament reminiscent of torsional waves. From the velocity dispersion radial profiles we find supersonic velocities that depend on each molecular tracer. We estimated the specific kinetic energy and compared to the gravitational potential, showing that the filament is gravitationally bound. This suggests that either the filament is collapsing or that other forces are required to provide support against gravity. Our analysis indicate that the cluster formation scenario is more complex that previously thought. We propose to study the influence of magnetic fields more carefully through numerical simulations and combining Zeeman with polarization observations. |
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