| DOI | Trouver le DOI : https://doi.org/10.1088/0067-0049/213/1/13 |
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| Auteur | Rechercher : Hull, Charles L. H.; Rechercher : Plambeck, Richard L.; Rechercher : Kwon, Woojin; Rechercher : Bower, Geoffrey C.; Rechercher : Carpenter, John M.; Rechercher : Crutcher, Richard M.; Rechercher : Fiege, Jason D.; Rechercher : Franzmann, Erica; Rechercher : Hakobian, Nicholas S.; Rechercher : Heiles, Carl; Rechercher : Houde, Martin; Rechercher : Hughes, A. Meredith; Rechercher : Lamb, James W.; Rechercher : Looney, Leslie W.; Rechercher : Marrone, Daniel P.; Rechercher : Matthews, Brenda C.1; Rechercher : Pillai, Thushara; Rechercher : Pound, Marc W.; Rechercher : Rahman, Nurur; Rechercher : Sandell, Goran; Rechercher : Stephens, Ian W.; Rechercher : Tobin, John J.; Rechercher : Vaillancourt, John E.; Rechercher : Volgenau, N. H.; Rechercher : Wright, Melvin C. H. |
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| Affiliation | - Conseil national de recherches du Canada. Infrastructure scientifique nationale
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| Format | Texte, Article |
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| Sujet | ISM: magnetic fields; magnetic fields; polarization; stars: formation; stars: magnetic field; stars: protostars |
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| Résumé | 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. |
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| Date de publication | 2014-07-03 |
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| Dans | |
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| Langue | anglais |
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| Publications évaluées par des pairs | Oui |
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| Numéro NPARC | 21272764 |
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| Exporter la notice | Exporter en format RIS |
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| Signaler une correction | Signaler une correction (s'ouvre dans un nouvel onglet) |
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| Identificateur de l’enregistrement | e343aa6d-1a31-4d7a-b7c2-792ba5e89114 |
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| Enregistrement créé | 2014-12-03 |
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| Enregistrement modifié | 2020-04-22 |
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