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TADPOL: A 1.3 mm Survey of Dust Polarization in Star-forming Cores and Regions

Hull, Charles L. H. and Plambeck, Richard L. and Kwon, Woojin and Bower, Geoffrey C. and Carpenter, John M. and Crutcher, Richard M. and Fiege, Jason D. and Franzmann, Erica and Hakobian, Nicholas S. and Heiles, Carl and Houde, Martin and Hughes, A. Meredith and Lamb, James W. and Looney, Leslie W. and Marrone, Daniel P. and Matthews, Brenda C. and Pillai, Thushara and Pound, Marc W. and Rahman, Nurur and Sandell, Göran and Stephens, Ian W. and Tobin, John J. and Vaillancourt, John E. and Volgenau, N. H. and Wright, Melvin C. H. (2014) TADPOL: A 1.3 mm Survey of Dust Polarization in Star-forming Cores and Regions. Astrophysical Journal Supplement Series, 213 (1). Art. No. 13. ISSN 0067-0049.

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We present λ 1.3 mm Combined Array for Research in Millimeter-wave Astronomy observations of dust polarization toward 30 star-forming cores and eight star-forming regions from the TADPOL survey. We show maps of all sources, and compare the ~2".5 resolution TADPOL maps with ~20" resolution polarization maps from single-dish submillimeter telescopes. Here we do not attempt to interpret the detailed B-field morphology of each object. Rather, we use average B-field orientations to derive conclusions in a statistical sense from the ensemble of sources, bearing in mind that these average orientations can be quite uncertain. We discuss three main findings. (1) A subset of the sources have consistent magnetic field (B-field) orientations between large (~20") and small (~2".5) scales. Those same sources also tend to have higher fractional polarizations than the sources with inconsistent large-to-small-scale fields. We interpret this to mean that in at least some cases B-fields play a role in regulating the infall of material all the way down to the ~1000 AU scales of protostellar envelopes. (2) Outflows appear to be randomly aligned with B-fields; although, in sources with low polarization fractions there is a hint that outflows are preferentially perpendicular to small-scale B-fields, which suggests that in these sources the fields have been wrapped up by envelope rotation. (3) Finally, even at ~2".5 resolution we see the so-called polarization hole effect, where the fractional polarization drops significantly near the total intensity peak. All data are publicly available in the electronic edition of this article.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Bower, Geoffrey C.0000-0003-4056-9982
Carpenter, John M.0000-0003-2251-0602
Marrone, Daniel P.0000-0002-2367-1080
Tobin, John J.0000-0002-6195-0152
Additional Information:© 2014 The American Astronomical Society. Received 2013 October 24; accepted 2014 March 11; published 2014 July 3. We thank the referee for thorough and insightful comments, which improved the paper significantly. C.L.H.H. acknowledges the advice and guidance of the members of the Berkeley Radio Astronomy Laboratory and the Berkeley Astronomy Department. In particular he thanks James Gao and James McBride, as well as the authors of the APLpy plotting package, for helping make the Python plots of TADPOL sources a reality. He would also like to thank Nicholas Chapman for helping to compile the SHARP data. C.L.H.H. acknowledges support from an NSF Graduate Fellowship and from a Ford Foundation Dissertation Fellowship. J.D.F. acknowledges support from an NSERC Discovery grant. J.J.T. acknowledges support provided by NASA through Hubble Fellowship grant no. HST-HF-51300.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. N.R. acknowledges support from South Africa Square Kilometer Array (SKA) Postdoctoral Fellowship program. Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities.
Funding AgencyGrant Number
NSF Graduate FellowshipUNSPECIFIED
Ford FoundationUNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
NASA Hubble FellowshipHST-HF-51300.01-A
NASANAS 5-26555
Subject Keywords:ISM: magnetic fields; magnetic fields; polarization; stars: formation; stars: magnetic field; stars: protostars
Issue or Number:1
Record Number:CaltechAUTHORS:20140815-092108964
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Official Citation:TADPOL: A 1.3 mm Survey of Dust Polarization in Star-forming Cores and Regions Charles L. H. Hull et al. 2014 ApJS 213 13
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:48594
Deposited By: Jason Perez
Deposited On:15 Aug 2014 20:53
Last Modified:09 Mar 2020 13:19

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