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

Soam, Archana; Liu, Tie; Andersson, B. G.; Lee, Chang-Won; Liu, Junhao; Juvela, M.; Li, Pak Shing; Goldsmith, Paul F.; Zhang, Qizhou; Koch, Patrick M.; Kim, Kee-Tae; Qiu, Keping; Evans, N. J.; Johnstone, Doug; Thompson, M. A.; Ward-Thompson, Derek; Francesco, James Di; Tang, Ya-Wen; Montillaud, J.; Kim, Gwanjeong; Mairs, Steve; Sanhueza, Patricio; Kim, Shinyoung; Berry, D. S.; Gordon, Michael S.; Tatematsu, Ken’ichi; Liu, Sheng-Yuan; Pattle, Kate; Eden, David; McGehee, P.; Wang, Ke; Ristorcelli, I.; Graves, Sarah; Alina, D.; Lacaille, Kevin; Montier, L.; Park, Geumsook; Kwon, Woojin; Chung, Eun Jung; Pelkonen, Veli-Matti; Micelotta, Elisabetta R.; Saajasto, Mika; Fuller, G. A.

doi:10.3847/1538-4357/ab39dd

Cited by 51 publications

(39 citation statements)

References 75 publications

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“…Previous studies concluded that the B-fields are observed to be mostly perpendicular to the main axis of dense filaments (e.g., Planck Collaboration et al 2016a, 2016b, 2016cPattle et al 2017;Soler et al 2017;Ward-Thompson et al 2017;Liu et al 2018;Fissel et al 2019;Soam et al 2019). Three filaments in NGC 1333 (#7, #13, and #18b) show perpendicular B-field orientations, which is consistent with those studies.…”

Section: Local B-field Alignment To Filamentssupporting

confidence: 88%

“…The angle γ is an inclination angle of the B-field with respect to the POS. Ward-Thompson et al 2017;Liu et al 2018;Fissel et al 2019;Soam et al 2019). Thus, our model, where we assume that a filament and the B-field are orthogonal in a 3D space, can successfully reproduce these observational results.…”

Section: Probability Distribution Of Offset Angle Projected To the Posmentioning

confidence: 54%

“…For example, some studies based on Planck and BLASTPol observations (e.g., Planck Collaboration et al 2016aCollaboration et al , 2016bCollaboration et al , 2016cSoler et al 2017;Fissel et al 2019) conclude that B-fields are observed to be mostly perpendicular to the long axes of dense filaments. Several ground-based polarimetry studies support these conclusions (Pattle et al 2017;Ward-Thompson et al 2017;Liu et al 2018;Soam et al 2019).…”

Section: Introductionmentioning

confidence: 75%

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The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

Doi¹,

Hasegawa

Furuya

et al. 2020

ApJ

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We present new observations of the active star formation region NGC 1333 in the Perseus molecular cloud complex from the James Clerk Maxwell Telescope B-Fields In Star-forming Region Observations (BISTRO) survey with the POL-2 instrument. The BISTRO data cover the entire NGC 1333 complex (∼1.5 pc×2 pc) at 0.02 pc resolution and spatially resolve the polarized emission from individual filamentary structures for the first time. The inferred magnetic field structure is complex as a whole, with each individual filament aligned at different position angles relative to the local field orientation. We combine the BISTRO data with low-and high-resolution data derived from Planck and interferometers to study the multiscale magnetic field structure in this region. The magnetic field morphology drastically changes below a scale of ∼1 pc and remains continuous from the scales of filaments (∼0.1 pc) to that of protostellar envelopes (∼0.005 pc or ∼1000 au). Finally, we construct simple models in which we assume that the magnetic field is always perpendicular to the long axis of the filaments. We demonstrate that the observed variation of the relative orientation between the filament axes and the magnetic field angles are well reproduced by this model, taking into account the projection effects of the magnetic field and filaments relative to the plane of the sky. These projection effects may explain the apparent complexity of the magnetic field structure observed at the resolution of BISTRO data toward the filament network.

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Section: Local B-field Alignment To Filamentssupporting

confidence: 88%

Section: Probability Distribution Of Offset Angle Projected To the Posmentioning

confidence: 54%

Section: Introductionmentioning

confidence: 75%

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The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

Doi¹,

Hasegawa

Furuya

et al. 2020

ApJ

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“…. This shows that the magnetic field required for the additional support against gravitational collapse could then be more than achieved if these cores follow the Crutcher et al (2010) relation, which is broadly consistent with the typical magnetic field strengths observed within molecular clouds (Pillai et al 2015(Pillai et al , 2016Soam et al 2019;Tang et al 2019).…”

Section: Thermal Turbulence and Magnetic Supportsupporting

confidence: 77%

“…We use the mean line-of-sight results from the PPMAP project shown in Figure 2 (Marsh et al 2016(Marsh et al , 2017. To check the fidelity of the PPMAP column density and temperature maps, where possible, we compare to the corresponding maps from Nguyen Luong et al (2011), Lim et al (2016, Zhang et al (2017), and Soam et al (2019). These authors independently produced column density and temperature maps following a more conventional far-infrared SED fitting routine, whilst accounting for the background in Herschel observations.…”

Section: Physical Propertiesmentioning

confidence: 99%

ALMA–IRDC: dense gas mass distribution from cloud to core scales

Barnes

Henshaw

Fontani

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Infrared dark clouds (IRDCs) are potential hosts of the elusive early phases of high-mass star formation (HMSF). Here we conduct an in-depth analysis of the fragmentation properties of a sample of 10 IRDCs, which have been highlighted as some of the best candidates to study HMSF within the Milky Way. To do so, we have obtained a set of large mosaics covering these IRDCs with ALMA at band 3 (or 3 mm). These observations have a high angular resolution (∼ 3″; ∼ 0.05 pc), and high continuum and spectral line sensitivity (∼ 0.15 mJy beam−1 and ∼ 0.2 K per 0.1 km s−1 channel at the N2H+ (1 − 0) transition). From the dust continuum emission, we identify 96 cores ranging from low- to high-mass (M = 3.4 − 50.9M⊙) that are gravitationally bound (αvir = 0.3 − 1.3) and which would require magnetic field strengths of B = 0.3 − 1.0 mG to be in virial equilibrium. We combine these results with a homogenised catalogue of literature cores to recover the hierarchical structure within these clouds over four orders of magnitude in spatial scale (0.01 pc – 10 pc). Using supplementary observations at an even higher angular resolution, we find that the smallest fragments (< 0.02 pc) within this hierarchy do not currently have the mass and/or the density required to form high-mass stars. Nonetheless, the new ALMA observations presented in this paper have facilitated the identification of 19 (6 quiescent and 13 star-forming) cores that retain >16 M⊙ without further fragmentation. These high-mass cores contain trans-sonic non-thermal motions, are kinematically sub-virial, and require moderate magnetic field strengths for support against collapse. The identification of these potential sites of high-mass star formation represents a key step in allowing us to test the predictions from high-mass star and cluster formation theories.

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Characterization of dense Planck clumps observed with Herschel and SCUBA-2

Mannfors

Juvela

Bronfman

et al. 2021

A&A

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Context. Although the basic processes of star formation (SF) are known, more research is needed on SF across multiple scales and environments. The Planck all-sky survey provided a large catalog of Galactic cold clouds and clumps that have been the target of several follow-up surveys. Aims. We aim to characterize a diverse selection of dense, potentially star-forming cores, clumps, and clouds within the Milky Way in terms of their dust emission and SF activity. Methods. We studied 53 fields that have been observed in the JCMT SCUBA-2 continuum survey SCOPE and have been mapped with Herschel. We estimated dust properties by fitting Herschel observations with modified blackbody functions, studied the relationship between dust temperature and dust opacity spectral index β, and estimated column densities. We extracted clumps from the SCUBA-2 850 µm maps with the FellWalker algorithm and examined their masses and sizes. Clumps are associated with young stellar objects found in several catalogs. We estimated the gravitational stability of the clumps with virial analysis. The clumps are categorized as unbound starless, prestellar, or protostellar. Results. We find 529 dense clumps, typically with high column densities from (0.3-4.8)×10 22 cm −2 , with a mean of (1.5±0.04)×10 22 cm −2 , low temperatures (T ∼10 -20 K), and estimated submillimeter β=1.7±0.1. We detect a slight increase in opacity spectral index toward millimeter wavelengths. Masses of the sources range from 0.04 M to 4259 M . Mass, linear size, and temperature are correlated with distance. Furthermore, the estimated gravitational stability is dependent on distance, and more distant clumps appear more virially bound. Finally, we present a catalog of properties of the clumps. Conclusions. Our sources present a large array of SF regions, from high-latitude, nearby diffuse clouds to large SF complexes near the Galactic center. Analysis of these regions will continue with the addition of molecular line data, which will allow us to study the densest regions of the clumps in more detail.

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

Cited by 51 publications

References 75 publications

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

The JCMT BISTRO Survey: Magnetic Fields Associated with a Network of Filaments in NGC 1333

ALMA–IRDC: dense gas mass distribution from cloud to core scales

Characterization of dense Planck clumps observed with Herschel and SCUBA-2

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