Magnetic Fields in the Infrared Dark Cloud G34.43+0.24

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dc.contributor.authorSoam, Archana
dc.contributor.authorLiu, Tie
dc.contributor.authorAndersson, B-G
dc.contributor.authorLee, Chang Won
dc.contributor.authorLiu, Junhao
dc.contributor.authorJuvela, Mika
dc.contributor.authorLi, Pak Shing
dc.contributor.authorGoldsmith, Paul F.
dc.contributor.authorZhang, Qizhou
dc.contributor.authorKoch, Patrick M.
dc.contributor.authorKim, Kee-Tae
dc.contributor.authorQiu, Keping
dc.contributor.authorEvans, Neal J., II
dc.contributor.authorJohnstone, Doug
dc.contributor.authorThompson, Mark
dc.contributor.authorWard-Thompson, Derek
dc.contributor.authorDi Francesco, James
dc.contributor.authorTang, Ya-Wen
dc.contributor.authorMontillaud, Julien
dc.contributor.authorKim, Gwanjeong
dc.contributor.authorMairs, Steve
dc.contributor.authorSanhueza, Patricio
dc.contributor.authorKim, Shinyoung
dc.contributor.authorBerry, David
dc.contributor.authorGordon, Michael S.
dc.contributor.authorTatematsu, Ken'ichi
dc.contributor.authorLiu, Sheng-Yuan
dc.contributor.authorPattle, Kate
dc.contributor.authorEden, David
dc.contributor.authorMcGehee, Peregrine M.
dc.contributor.authorWang, Ke
dc.contributor.authorRistorcelli, I.
dc.contributor.authorGraves, Sarah F.
dc.contributor.authorAlina, Dana
dc.contributor.authorLacaille, Kevin M.
dc.contributor.authorMontier, Ludovic
dc.contributor.authorPark, Geumsook
dc.contributor.authorKwon, Woojin
dc.contributor.authorChung, Eun Jun
dc.contributor.authorPelkonen, Veli-Matti
dc.contributor.authorMicelotta, Elisabetta R.
dc.contributor.authorSaajasto, Mika
dc.contributor.authorFuller, Gary
dc.date.accessioned2019-12-12T05:27:50Z
dc.date.available2019-12-12T05:27:50Z
dc.date.issued2019-09-24
dc.description.abstractWe present the B-fields mapped in IRDC G34.43+0.24 using 850 mu m polarized dust emission observed with the POL-2 instrument at the James Clerk Maxwell telescope. We examine the magnetic field geometries and strengths in the northern, central, and southern regions of the filament. The overall field geometry is ordered and aligned closely perpendicular to the filament's main axis, particularly in regions containing the central clumps MM1 and MM2, whereas MM3 in the north has field orientations aligned with its major axis. The overall field orientations are uniform at large (POL-2 at 14 '' and SHARP at 10 '') to small scales (TADPOL at 2 ''.5 and SMA at 1 ''.5) in the MM1 and MM2 regions. SHARP/CSO observations in MM3 at 350 mu m from Tang et al. show a similar trend as seen in our POL-2 observations. TADPOL observations demonstrate a well-defined field geometry in MM1/MM2 consistent with MHD simulations of accreting filaments. We obtained a plane-of-sky magnetic field strength of 470 +/- 190 mu G, 100 +/- 40 mu G, and 60 +/- 34 mu G in the central, northern, and southern regions of G34, respectively, using the updated Davis-Chandrasekhar-Fermi relation. The estimated value of field strength, combined with column density and velocity dispersion values available in the literature, suggests G34 to be marginally critical with criticality parameter lambda values 0.8 +/- 0.4, 1.1 +/- 0.8, and 0.9 +/- 0.5 in the central, northern, and southern regions, respectively. The turbulent motions in G34 are sub-AlfvEnic with Alfvenic Mach numbers of 0.34 +/- 0.13, 0.53 +/- 0.30, and 0.49 +/- 0.26 in the three regions. The observed aligned B-fields in G34.43+0.24 are consistent with theoretical models suggesting that B-fields play an important role in guiding the contraction of the cloud driven by gravity.en_US
dc.identifier.citationSoam, A., Liu, T., Andersson, B. G., Lee, C. W., Liu, J., Juvela, M., ... & Kim, K. T. (2019). Magnetic fields in the infrared dark cloud G34. 43+ 0.24. The Astrophysical Journal, 883(1), 95en_US
dc.identifier.urihttp://nur.nu.edu.kz/handle/123456789/4421
dc.language.isoenen_US
dc.publisherIOP PUBLISHINGen_US
dc.rightsAttribution-NonCommercial-ShareAlike 3.0 United States*
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/3.0/us/*
dc.titleMagnetic Fields in the Infrared Dark Cloud G34.43+0.24en_US
dc.typeArticleen_US
workflow.import.sourcescience

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