Far‐infrared and Submillimeter Polarization of OMC‐1: Evidence for Magnetically Regulated Star Formation

Schleuning, D. A.

doi:10.1086/305139

Cited by 163 publications

(183 citation statements)

References 44 publications

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“…It traces a magnetic field of which the sky-plane projection is actually along the Bar, in disagreement with the suggestion by Schleuning (1998). It is uncertain whether this result confirms the conjecture of Houde et al (2004) corroborating the H 2 excitation study of Shaw et al (2009).…”

Section: Omc1contrasting

confidence: 71%

“…He confirmed the relatively weak linear polarization and its position angle measured by Hildebrand et al (1984) towards the Kleinman-Low nebula (Orion KL) which is thought to be powered by an explosive event (Zapata et al 2011), while the neighboring high mass star-forming region Orion-South and the envelope of Orion KL exhibit a stronger polarization. Schleuning (1998) explains the depolarization in Orion KL by the rising dust opacity towards the far-infrared, while the low polarization in the Orion Bar, a photon-dominated region seen edge-on (Tielens & Hollenbach 1985), is attributed to a magnetic field pointing to the observer. Vaillancourt et al (2008) studied the polarization spectrum of OMC-1 and conclude that a polarization minimum occurs between λ100 µm and λ350 µm while Houde et al (2004), investigating the large scale structure of the magnetic field in Orion A, confirmed the relatively smooth polarization angle structure towards OMC1 and interprete the weak polarization levels in the Orion bar with the lower dust temperature in that region.…”

Section: Omc1mentioning

confidence: 94%

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Submillimeter polarimetry with PolKa, a reflection-type modulator for the APEX telescope

Wiesemeyer

Hezareh

Kreysa

et al. 2014

2014 39th International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz)

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Imaging polarimetry is an important tool for the study of cosmic magnetic fields. In our Galaxy, polarization levels of a few up to ∼10% are measured in the submillimeter dust emission from molecular clouds and in the synchrotron emission from supernova remnants. Only few techniques exist to image the distribution of polarization angles, as a means of tracing the plane-of-sky projection of the magnetic field orientation. At submillimeter wavelengths, polarization is either measured as the differential total power of polarization-sensitive bolometer elements, or by modulating the polarization of the signal. Bolometer arrays such as LABOCA at the APEX telescope are used to observe the continuum emission from fields as large as ∼ 0.• 2 in diameter. Here we present PolKa, a polarimeter for LABOCA with a reflection-type waveplate of at least 90% efficiency.The modulation efficiency depends mainly on the sampling and on the angular velocity of the waveplate. For the data analysis the concept of generalized synchronous demodulation is introduced. The instrumental polarization towards a point source is at the level of ∼ 0.1%, increasing to a few percent at the −10db contour of the main beam. A method to correct for its effect in observations of extended sources is presented. Our map of the polarized synchrotron emission from the Crab nebula is in agreement with structures observed at radio and optical wavelengths. The linear polarization measured in OMC1 agrees with results from previous studies, while the high sensitivity of LABOCA enables us to also map the polarized emission of the Orion Bar, a prototypical photon-dominated region.

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Section: Omc1contrasting

confidence: 71%

Section: Omc1mentioning

confidence: 94%

Submillimeter polarimetry with PolKa, a reflection-type modulator for the APEX telescope

Wiesemeyer

Hezareh

Kreysa

et al. 2014

2014 39th International Conference on Infrared, Millimeter, and Terahertz Waves (IRMMW-THz)

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“…In the southern half of the filament, the field appears to curve to the south, forming an inverted U-shape. This so-called "hourglass" morphology was first noted by Schleuning (1998) at much lower resolution and signal-to-noise ratio, observing at 100 and 350 μm with the Kuiper Airborne Observatory (KAO) and the Caltech Submillimeter Observatory, respectively. However, we note a far higher degree of curvature of the field lines than was seen by Schleuning (1998).…”

Section: First Data From the Surveymentioning

confidence: 93%

First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt

Ward-Thompson

Pattle

Bastien

et al. 2017

ApJ

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We present the first results from the B-fields In STar-forming Region Observations (BISTRO) survey, using the Sub-millimetre Common-User Bolometer Array2 camera, with its associated polarimeter (POL-2), on the James Clerk Maxwell Telescope in Hawaii. We discuss the survey's aims and objectives. We describe the rationale behind the survey, and the questions thatthe survey will aim to answer. The most important of these is the role of magnetic fields in the star formation process on the scale of individual filaments and cores in dense regions. We describe the data acquisition and reduction processes for POL-2, demonstrating both repeatability and consistency with previous data. We present a first-look analysis of the first results from the BISTRO survey in the OMC1 region. We see that the magnetic field lies approximately perpendicular to the famous "integral filament" in the densest regions of that filament. Furthermore, we see an "hourglass" magnetic field morphology extending beyond the densest region of the integral filament into the less-dense surrounding material, and discuss possible causes for this. We also discuss the more complex morphology seen along the Orion Bar region. We examine the morphology of the field along the lower-density northeastern filament. We find consistency with previous theoretical models that predict magnetic fields lying parallel to low-density, non-self-gravitating filaments, and perpendicular to higher-density, self-gravitating filaments.

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“…Therefore our knowledge of cloud magnetic fields has been mostly concentrated on cloud cores, using field morphologies (e.g. Schleuning 1998;Girart, Rao, & Marrone 2006), Chandrasekhar-Fermi method (e.g. Crutcher et al 2004) and Zeeman measurements (e.g.…”

Section: Introductionmentioning

confidence: 99%

Anchoring Magnetic Field in Turbulent Molecular Clouds

Dowell

Goodman

et al. 2009

ApJ

100

118

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One of the key problems in star formation research is to determine the role of magnetic fields. Starting from the atomic inter-cloud medium (ICM) which has density n H ~ 1 cm −3 , gas must accumulate from a volume several hundred pc across in order to form a typical molecular cloud. Star formation usually occurs in cloud cores, which have linear sizes below 1 pc and densities n H2 > 10 5 cm −3 . With current technologies, it is hard to probe magnetic fields at scales lying between the accumulation length and the size of cloud cores, a range corresponds to many levels of turbulent eddy cascade, and many orders of magnitude of density amplification. For field directions detected from the two extremes, however, we show here that a significant correlation is found. Comparing this result with molecular cloud simulations, only the sub-Alfvénic cases result in field orientations consistent with our observations.

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Far‐infrared and Submillimeter Polarization of OMC‐1: Evidence for Magnetically Regulated Star Formation

Cited by 163 publications

References 44 publications

Submillimeter polarimetry with PolKa, a reflection-type modulator for the APEX telescope

Submillimeter polarimetry with PolKa, a reflection-type modulator for the APEX telescope

First Results from BISTRO: A SCUBA-2 Polarimeter Survey of the Gould Belt

Anchoring Magnetic Field in Turbulent Molecular Clouds

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