dc.contributor.advisor Mundy, Lee G en_US dc.contributor.author Storm, Shaye en_US dc.date.accessioned 2016-02-06T06:35:01Z dc.date.available 2016-02-06T06:35:01Z dc.date.issued 2015 en_US dc.identifier https://doi.org/10.13016/M26X4B dc.identifier.uri http://hdl.handle.net/1903/17236 dc.description.abstract This thesis utilizes new observations of dense gas in molecular clouds to develop an empirical framework for how clouds form structures which evolve into young cores and stars. Previous observations show the general turbulent and hierarchical nature of clouds. However, current understanding of the star formation pathway is limited by existing data that do not combine angular resolution needed to resolve individual cores with area coverage required to capture entire star-forming regions and with tracers that can resolve gas motions. The original contributions of this thesis to astrophysical research are the creation and analysis of the largest-area high-angular-resolution maps of dense gas in molecular clouds to-date, and the development of a non-binary dendrogram algorithm to quantify the hierarchical nature and three-dimensional morphology of cloud structure. I first describe the CARMA Large Area Star Formation Survey, which provides spectrally imaged \NtwoH{}, \HCO{}, and HCN ($J=1\rightarrow0$) emission across diverse regions of the Perseus and Serpens Molecular Clouds. I then present a detailed analysis of the Barnard~1 and L1451 regions in Perseus. A non-binary dendrogram analysis of Barnard~1 \NtwoH{} emission and all L1451 emission shows that the most hierarchically complex gas corresponds with sub-regions actively forming young stars. I estimate the typical depth of molecular emission in each region using the spatial and kinematic properties of dendrogram-identified structures. Barnard~1 appears to be a sheet-like region at the largest scales with filamentary substructure, while the L1451 region is composed of more spatially distinct ellipsoidal structures. I then do a uniform comparison of the hierarchical structure and young stellar content of all five regions. The more evolved regions with the most young stellar objects (YSOs) and strongest emission have formed the most hierarchical levels. However, all regions show similar mean branching properties at each level, suggesting that dense gas fragmentation proceeds in a hierarchically similar way from earlier to later stages of star formation. Compared to the more evolved YSOs, the youngest YSOs are preferentially forming within leaves and at high-level locations in dendrogram hierarchies, indicating that dense gas in molecular clouds must reach a state of hierarchical complexity before young stars form efficiently. en_US dc.language.iso en en_US dc.title High-Resolution Imaging of Dense Gas Structure and Kinematics in Nearby Molecular Clouds with the CARMA Large Area Star Formation Survey en_US dc.type Dissertation en_US dc.contributor.publisher Digital Repository at the University of Maryland en_US dc.contributor.publisher University of Maryland (College Park, Md.) en_US dc.contributor.department Astronomy en_US dc.subject.pqcontrolled Astronomy en_US dc.subject.pquncontrolled Dendrograms en_US dc.subject.pquncontrolled ISM Kinematics en_US dc.subject.pquncontrolled ISM Structure en_US dc.subject.pquncontrolled Molecular Clouds en_US dc.subject.pquncontrolled Perseus Molecular Cloud en_US dc.subject.pquncontrolled Star Formation en_US
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