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The Perseus molecular cloud is a nearby star-forming region in
which both low and intermediate mass stars are forming. A wealth
of data at a variety of wavelengths exists over a large extent of the
cloud. Analysis of the column density distribution has placed strong
observational constraints on models of star-formation and cloud support
(see the presentation in this conference by Johnstone). Here, we
present results from an IRAM survey of the dense cores within Perseus,
in order to place similar constraints on the kinematics of the region.
We observed over 150 candidate objects, ranging from starless cores
to protostars, in N2H+, a good dense gas tracer. The previous column
density analysis revealed large moderate extinction regions (Av > ~5)
in which all of the major star-formation occurs (e.g., NGC 1333, IC 348,
B1, etc). Our dense core observations span all of these extinction
regions. We measure both the internal kinematics (internal level of
turbulence of each core) as well as the kinematic properties of the
group of independent cores over each extinction region and the cloud
as a whole. These measures are compared with predictions from turbulent
simulations.
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