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Our recent advances in the visualization and characterization of
complex molecular line emission maps allow us to scrutinize
star-forming regions with previously unattained stringency and
oversight. In a first study, we apply these methods to 13CO maps of
the L1448 region in the Perseus molecular cloud. Specifically, using
an innovative structure identification approach geared at hierarchical
objects like molecular clouds, we extract and physically characterize
(e.g., in terms of mass) features across the full range of spatial
scales covered (i.e., 0.1 to 4 pc). Subsequent analysis shows that
dense cores preferentially exist in regions of high pressure and
density. Interestingly, gravity seems to be of lesser relevance
though. Also, using our open source 3D data visualization tools (see
http://am.iic.harvard.edu), we also identify filamentary features that
seem to influence the aggregation of cores. The formation of cores is
possibly triggered by collisions of larger clumps. Finally, our
observations indicate that, even in a region as quiescent as L1448,
the global impact of stellar winds, radiation, and Hii regions cannot
be ignored. If the latter was true, present numerical simulations of
molecular clouds do probably miss an important agent of cloud
evolution.
The above discussion thus also highlights how extensive legacy-style
datasets, like our COMPLETE survey, will in future change the way
in which research is conducted. Beyond this, it illustrates that these
data need to be matched with appropriate software tools, like our 3D
visualization suite. Unfortunately, the tools needed are often too
complex to be built by astronomers. Our project, which collaborates
with medical 3D imaging communities via an interdisciplinary research
institute, illustrates a path out of these emerging dilemmas.
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