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CARMA Large Area Star-formation SurveY
Completing observations of 5 regions of 120-200 square arcminutes with 7” angular resolution in the J=1-0 transitions of HCO+, HCN, and N2H+
Regions are in the Perseus and Serpens molecular clouds – covered by the c2d Spitzer Legacy project which characterized the young stellar population
Using CARMA to get interferometric and single-dish data to make maps of the full emission
Completed last week: 600 hours total array time
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NGC 1333High-Activity
~100 sq. arcmin.
Barnard 1Moderate-Activity
~150 sq. arcmin. (focus of this paper)
L1451Low-Activity
~150 sq. arcmin
~3.5 pc
~5.5 pc
Composite Herschel250, 350, 500 μm view
Approximate CARMA mapping areas
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N2H+ Emission Velocity Field HCN Emission
NGC 1333 SVS -13 Region HCO+ Emission
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NGC 1333 SVS-13 Herschel 350 microns versus N2H+
N2H+ emission tracks the structure in the long wavelength continuum….
The bright region to the northeast is a heated area associated with a reflection nebula.
N2H+ traces gas >105 per cc and give velocity information.
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Provides resolution to study individual objects in the context of the large scale cloud.
Beam size in above three maps
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Perseus B1 Region
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main core
central filaments
southern clumps
N2H+
HCN HCO+
Herschel 250 μm
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Cloudprops(best for sparse fields)
Object Identification Methods
Molecular Cloud structure is mostly hierarchical … dendrograms avoid small-scale segmentation and
naturally capture large-scales in addition to the small-scales
vs. Dendrograms
(best for dense/blended fields)
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Capturing Large and Small Scales with Dendrogram Approach
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Moment Zero Maps of Leaves and Branches
How do larger-scale gas structures compare to smaller-scale structures?
Facilitates an investigation of the turbulent properties of dense gas at different scales in a way that clumpfind-like segmentation would not allow
LeafBranch
IRAS 2 region of NGC 1333
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Integrated Intensity Maps
0.04 pc
Results: Non-Binary Dendrogramof NGC 1333 N2H+ (1-0)
How do larger-scale gas structures compare to smaller-scale structures?
We evaluated the size and kinematics of each identified gas structure
Turbulence … across different spatial scales within a single cloud… across different clouds at different stages of evolution?
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Fitted Line Dispersion Maps
How do larger-scale gas structures compare to smaller-scale structures?
Results: Non-Binary Dendrogramof NGC 1333 N2H+ (1-0)
We evaluated the size and kinematics of each identified gas structure
Turbulence … across different spatial scales within a single cloud… across different clouds at different stages of evolution?
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Results: Line Dispersion vs. Sizein NGC 1333 Gas Structures
Capturing mean internal turbulence
- - - - H2 thermal dispersion N2H+ thermal dispersion … at 11 K and 25 K
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Results: Non-Binary Dendrogram Structure
of Barnard 1 N2H+ (1-0)
Spitzer IRAC+ N2H+ outline
black = nearby protostellar outflowsred = further from outflow activity
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Results: Cross-Cloud ComparisonBarnard 1
- - - - H2 thermal dispersion N2H+ thermal dispersion … at 9 K and 12 K
vs.
NGC 1333
- - - - H2 thermal dispersion N2H+ thermal dispersion … at 11 K and 25 K
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Results: Cross-Cloud ComparisonBarnard 1
- - - - H2 thermal dispersion N2H+ thermal dispersion … at 9 K and 12 K
vs.
NGC 1333
- - - - H2 thermal dispersion N2H+ thermal dispersion … at 11 K and 25 K
Observe supersonic turbulence at ~0.01 – 0.5 pc scales near active
young stars
Indication that outflows are an important turbulent driver of the dense
gas at these scales
not an outflow
N2H+ moment 0HCO+ outflows
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Results: Cross-Cloud ComparisonBarnard 1
- - - - H2 thermal dispersion N2H+ thermal dispersion … at 9 K and 12 K
vs.
NGC 1333
- - - - H2 thermal dispersion N2H+ thermal dispersion … at 11 K and 25 K
Observe subsonic turbulence in filamentary regions yet to form young, active stars
… expected if these dense gas filaments formed from supersonic turbulence
Next step to probe even larger scales and make connection to lower density gas
not an outflow
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• Wealth of kinematics on ~1000s of AU size scale– fully sampled spatial scales •Dendrograms used to decompose dense gas emission and explore kinematics of structures in CLASSy clouds
• Compared turbulent linewidths of NGC 1333 and B1 gas structures:• Star formation feedback correlates with supersonic turbulence at the ~0.01 – 0.5 pc scale
• B1 filament is a great region to probe turbulence driven star formation theories
Summary
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Smaller Scale Magnetic Field
Simultaneously observed CO outflow
Hull et al. 2013
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Smaller Scale Magnetic FieldInferred magnetic fields are more consistent with random or anti-aligned with the outflow axis.
Maybe good news for young disks (Vorobyov 2010, Joos et al. 2012, Li et al. 2013)
Hull et al. 2013
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Disks? What about magnetic braking?TADPOL results for L1527 and VLA 1623– coupled with no disk
detection of L1157— interesting trend
Hul
l et a
l. 20
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