Journal
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
Volume 213, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0067-0049/213/1/13
Keywords
ISM: magnetic fields; magnetic fields; polarization; stars: formation; stars: magnetic field; stars: protostars
Categories
Funding
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1139950, 1140063] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1007713, 1140019, 1140031, 1139998] Funding Source: National Science Foundation
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We present lambda 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 similar to 2 ''.5 resolution TADPOL maps with similar to 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 (similar to 20 '') and small (similar to 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 similar to 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 similar to 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.
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