TY - JOUR
T1 - Interferometric mapping of magnetic fields
T2 - The ALMA view of the massive star-forming clump W43-MM1
AU - Cortes, Paulo C.
AU - Girart, Josep M.
AU - Hull, Charles L.H.
AU - Sridharan, Tirupati K.
AU - Louvet, Fabien
AU - Plambeck, Richard
AU - Li, Zhi Yun
AU - Crutcher, Richard M.
AU - Lai, Shih Ping
N1 - Funding Information:
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO. ALMA#2013.1.00725.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. P.C.C. would like to thank Ed Fomalont for very helpful and enlighten discussion about polarization data analysis. J.M.G. acknowledges support from MICINN AYA2014- 57369-C3-P and the MECD PRX15/00435 grants (Spain). Z.Y.L. is supported in part by NASA NNX14AB38G and NSF AST-1313083. S.P.L. thanks the support of the Ministry of Science and Technology (MoST) of Taiwan through grants NSC 98-2112- M-007-007-MY3, NSC 101-2119-M-007-004, and MoST 102- 2119-M-007-004-MY3.
Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/7/1
Y1 - 2016/7/1
N2 - Here, we present the first results from ALMA observations of 1 mm polarized dust emission toward the W43-MM1 high-mass star-forming clump. We have detected a highly fragmented filament with source masses ranging from 14 M⊙ to 312 M⊙, where the largest fragment, source A, is believed to be one of the most massive in our Galaxy. We found a smooth, ordered, and detailed polarization pattern throughout the filament, which we used to derived magnetic field morphologies and strengths for 12 out of the 15 fragments detected ranging from 0.2 to 9 mG. The dynamical equilibrium of each fragment was evaluated finding that all the fragments are in a super-critical state that is consistent with previously detected infalling motions toward W43-MM1. Moreover, there are indications suggesting that the field is being dragged by gravity as the whole filament is collapsing.
AB - Here, we present the first results from ALMA observations of 1 mm polarized dust emission toward the W43-MM1 high-mass star-forming clump. We have detected a highly fragmented filament with source masses ranging from 14 M⊙ to 312 M⊙, where the largest fragment, source A, is believed to be one of the most massive in our Galaxy. We found a smooth, ordered, and detailed polarization pattern throughout the filament, which we used to derived magnetic field morphologies and strengths for 12 out of the 15 fragments detected ranging from 0.2 to 9 mG. The dynamical equilibrium of each fragment was evaluated finding that all the fragments are in a super-critical state that is consistent with previously detected infalling motions toward W43-MM1. Moreover, there are indications suggesting that the field is being dragged by gravity as the whole filament is collapsing.
KW - ISM: clouds
KW - ISM: kinematics and dynamics
KW - ISM: magnetic fields
UR - http://www.scopus.com/inward/record.url?scp=84978481296&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84978481296&partnerID=8YFLogxK
U2 - 10.3847/2041-8205/825/1/L15
DO - 10.3847/2041-8205/825/1/L15
M3 - Article
AN - SCOPUS:84978481296
SN - 2041-8205
VL - 825
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L15
ER -