Multiwavelength Polarimetry of the Filamentary Cloud IC 5146. II. Magnetic Field Structures

被引：19

作者：

Wang, Jia-Wei ^{[1
,2
,3
]}

Lai, Shih-Ping ^{[1
,2
]}

Clemens, Dan P. ^{[4
]}

Koch, Patrick M. ^{[3
]}

Eswaraiah, Chakali ^{[5
,6
]}

Chen, Wen-Ping ^{[7
]}

Pandey, Anil K. ^{[8
]}

机构：

[1] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan

[2] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan

[3] Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan

[4] Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA

[5] Chinese Acad Sci, NAOC, CAS Key Lab FAST, Beijing 100101, Peoples R China

[6] Chinese Acad Sci, Natl Astron Observ, Datun Rd, Beijing 100101, Peoples R China

[7] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan

[8] Aryabhatta Res Inst Observat Sci ARIES, Naini Tal 263001, India

来源：

ASTROPHYSICAL JOURNAL | 2020年 / 888卷 / 01期

基金：

国家重点研发计划;

关键词：

STAR-FORMATION; INTERSTELLAR CLOUDS; AMBIPOLAR DIFFUSION; MOLECULAR CLOUDS; POLARIZATION; CONTRACTION; STRENGTHS; COLLAPSE; CORES; MODEL;

D O I：

10.3847/1538-4357/ab5c1c

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The IC 5146 cloud is a nearby star-forming region in Cygnus, consisting of molecular gas filaments in a variety of evolutionary stages. We used optical and near-infrared polarization data toward the IC 5146 cloud, reported in the first paper of this series, to reveal the magnetic fields in this cloud. Using the newly released Gaia data, we found that the IC 5146 cloud may contain two separate clouds: a first cloud, including the densest main filament at a distance of similar to 600 pc, and a second cloud, associated with the Cocoon Nebula at a distance of similar to 800 pc. The spatially averaged H-band polarization map revealed a well-ordered magnetic field morphology, with the polarization segments perpendicular to the main filament but parallel to the nearby subfilaments, consistent with models assuming that the magnetic field is regulating cloud evolution. We estimated the magnetic field strength using the Davis-Chandrasekhar-Fermi method and found that the magnetic field strength scales with volume density with a power-law index of similar to 0.5 in the density range from <CDATA<i to 3000 cm(-3), which indicates an anisotropic cloud contraction with a preferred direction along the magnetic field. In addition, the mass-to-flux ratio of the cloud gradually changes from subcritical to supercritical from the cloud envelope to the deep regions. These features are consistent with strong magnetic field star formation models and suggest that the magnetic field is important in regulating the evolution of the IC 5146 cloud.

引用

页数：19

共 72 条

[1] Planck intermediate results XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds [J].

Ade, P. A. R. ;

Aghanim, N. ;

Alves, M. I. R. ;

Arnaud, M. ;

Arzoumanian, D. ;

Ashdown, M. ;

Aumont, J. ;

Baccigalupi, C. ;

Banday, A. J. ;

Barreiro, R. B. ;

Bartolo, N. ;

Battaner, E. ;

Benabed, K. ;

Benoit, A. ;

Benoit-Levy, A. ;

Bernard, J-P. ;

Bersanelli, M. ;

Bielewicz, P. ;

Bock, J. J. ;

Bonavera, L. ;

Bond, J. R. ;

Borrill, J. ;

Bouchet, F. R. ;

Boulanger, F. ;

Bracco, A. ;

Burigana, C. ;

Calabrese, E. ;

Cardoso, J. -F. ;

Catalano, A. ;

Chiang, H. C. ;

Christensen, P. R. ;

Colombo, L. P. L. ;

Combet, C. ;

Couchot, F. ;

Crill, B. P. ;

Curto, A. ;

Cuttaia, F. ;

Danese, L. ;

Davies, R. D. ;

Davis, R. J. ;

de Bernardis, P. ;

de Rosa, A. ;

de Zotti, G. ;

Delabrouille, J. ;

Dickinson, C. ;

Diego, J. M. ;

Dole, H. ;

Donzelli, S. ;

Dore, O. ;

Douspis, M. .

ASTRONOMY & ASTROPHYSICS, 2016, 586

[2] NEW LOOK AT STATISTICAL-MODEL IDENTIFICATION [J].

AKAIKE, H .

IEEE TRANSACTIONS ON AUTOMATIC CONTROL, 1974, AC19 (06) :716-723

[3]

Andre P., 2014 PROTOSTARS PLAN

[4] From filamentary clouds to prestellar cores to the stellar IMF: Initial highlights from the Herschel Gould Belt Survey [J].

Andre, Ph. ;

Men'shchikov, A. ;

Bontemps, S. ;

Koenyves, V. ;

Motte, F. ;

Schneider, N. ;

Didelon, P. ;

Minier, V. ;

Saraceno, P. ;

Ward-Thompson, D. ;

Di Francesco, J. ;

White, G. ;

Molinari, S. ;

Testi, L. ;

Abergel, A. ;

Griffin, M. ;

Henning, Th. ;

Royer, P. ;

Merin, B. ;

Vavrek, R. ;

Attard, M. ;

Arzoumanian, D. ;

Wilson, C. D. ;

Ade, P. ;

Aussel, H. ;

Baluteau, J. -P. ;

Benedettini, M. ;

Bernard, J. -Ph. ;

Blommaert, J. A. D. L. ;

Cambresy, L. ;

Cox, P. ;

Di Giorgio, A. ;

Hargrave, P. ;

Hennemann, M. ;

Huang, M. ;

Kirk, J. ;

Krause, O. ;

Launhardt, R. ;

Leeks, S. ;

Le Pennec, J. ;

Li, J. Z. ;

Martin, P. G. ;

Maury, A. ;

Olofsson, G. ;

Omont, A. ;

Peretto, N. ;

Pezzuto, S. ;

Prusti, T. ;

Roussel, H. ;

Russeil, D. .

ASTRONOMY & ASTROPHYSICS, 2010, 518

[5] Formation and evolution of interstellar filaments Hints from velocity dispersion measurements [J].

Arzoumanian, D. ;

Andre, Ph ;

Peretto, N. ;

Koenyves, V. .

ASTRONOMY & ASTROPHYSICS, 2013, 553

[6] Characterizing interstellar filaments with Herschel in IC 5146 [J].

Arzoumanian, D. ;

Andre, Ph. ;

Didelon, P. ;

Koenyves, V. ;

Schneider, N. ;

Men'shchikov, A. ;

Sousbie, T. ;

Zavagno, A. ;

Bontemps, S. ;

Di Francesco, J. ;

Griffin, M. ;

Hennemann, M. ;

Hill, T. ;

Kirk, J. ;

Martin, P. ;

Minier, V. ;

Molinari, S. ;

Motte, F. ;

Peretto, N. ;

Pezzuto, S. ;

Spinoglio, L. ;

Ward-Thompson, D. ;

White, G. ;

Wilson, C. D. .

ASTRONOMY & ASTROPHYSICS, 2011, 529

[7]

Brown A.G.A., 2018, Astron. & Astrophys, V616, pA1, DOI [DOI 10.1051/0004-6361/201833051, 10.1051/0004-6361/201833051]

[8] MAGNETIC FIELDS IN SPIRAL ARMS [J].

CHANDRASEKHAR, S ;

FERMI, E .

ASTROPHYSICAL JOURNAL, 1953, 118 (01) :113-115

[9] Magnetic Fields in Molecular Clouds [J].

Crutcher, Richard M. .

ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS, VOL 50, 2012, 50 :29-63

[10] MAGNETIC FIELDS IN INTERSTELLAR CLOUDS FROM ZEEMAN OBSERVATIONS: INFERENCE OF TOTAL FIELD STRENGTHS BY BAYESIAN ANALYSIS [J].

Crutcher, Richard M. ;

Wandelt, Benjamin ;

Heiles, Carl ;

Falgarone, Edith ;

Troland, Thomas H. .

ASTROPHYSICAL JOURNAL, 2010, 725 (01) :466-479

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