Alma Science Verification Data: Millimeter Continuum Polarimetry of the Bright Radio Quasar 3c 286

Nagai, Hiroshi; Nakanishi, Koichiro; Paladino, R.; Hull, Charles L. H.; Cortés, Paulo C.; Moellenbrock, G.; Fomalont, Ed; Asada, Keiichi; Hada, Kazuhiro

doi:10.3847/0004-637x/824/2/132

Cited by 53 publications

(65 citation statements)

References 27 publications

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“…The details of all four data sets are summarized in Table 2. The ALMA results we present here are among the first results from the ALMA full-polarization system, which has already led to publications on magnetized low- ) and high-mass star formation (Cortes et al 2016); quasar polarization (Nagai et al 2016); and protostellar disk polarization (Kataoka et al 2016b).…”

Section: Introductionmentioning

confidence: 90%

ALMA Observations of Dust Polarization and Molecular Line Emission from the Class 0 Protostellar Source Serpens SMM1

Hull

Girart

Tychoniec

et al. 2017

ApJ

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113

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We present high angular resolution dust polarization and molecular line observations carried out with the Atacama Large Millimeter/submillimeter Array (ALMA) toward the Class 0 protostar Serpens SMM1. By complementing these observations with new polarization observations from the Submillimeter Array (SMA) and archival data from the Combined Array for Research in Millimeter-wave Astronomy (CARMA) and the James Clerk Maxwell Telescopes (JCMT), we can compare the magnetic field orientations at different spatial scales. We find major changes in the magnetic field orientation between large (∼0.1 pc) scales-where the magnetic field is oriented E-W, perpendicular to the major axis of the dusty filament where SMM1 is embedded-and the intermediate and small scales probed by CARMA (∼1000 au resolution), the SMA (∼350 au resolution), and ALMA (∼140 au resolution). The ALMA maps reveal that the redshifted lobe of the bipolar outflow is shaping the magnetic field in SMM1 on the southeast side of the source; however, on the northwestern side and elsewhere in the source, lowvelocity shocks may be causing the observed chaotic magnetic field pattern. High-spatial-resolution continuum and spectral-line observations also reveal a tight (∼130 au) protobinary system in SMM1-b, the eastern component of which is launching an extremely high-velocity, one-sided jet visible in both =  (J CO 2 1) and =  (J SiO 5 4); however, that jet does not appear to be shaping the magnetic field. These observations show that with the sensitivity and resolution of ALMA, we can now begin to understand the role that feedback (e.g., from protostellar outflows) plays in shaping the magnetic field in very young, star-forming sources like SMM1.

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Section: Introductionmentioning

confidence: 90%

ALMA Observations of Dust Polarization and Molecular Line Emission from the Class 0 Protostellar Source Serpens SMM1

Hull

Girart

Tychoniec

et al. 2017

ApJ

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113

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“…The instrumental polarization contamination of the ALMA interferometers is the polarization fraction of 0.1 % for a point source in the center of the field or 0.3 % within up to the inner 1/3 of the FWHM (see the technical handbook of ALMA. More discussion is found in Nagai et al 2016). The derived polarization fraction of the integrated flux corresponds to the case of the point source.…”

Section: Introductionmentioning

confidence: 99%

The Evidence of Radio Polarization Induced by the Radiative Grain Alignment and Self-scattering of Dust Grains in a Protoplanetary Disk

Kataoka

Tsukagoshi

Pohl

et al. 2017

ApJL

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146

192

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The mechanisms causing millimeter-wave polarization in protoplanetary disks are under debate. To disentangle the polarization mechanisms, we observe the protoplanetary disk around HL Tau at 3.1 mm with the Atacama Large Millimeter/submillimeter Array (ALMA), which had polarization detected with CARMA at 1.3 mm. We successfully detect the ring-like azimuthal polarized emission at 3.1 mm. This indicates that dust grains are aligned with the major axis being in the azimuthal direction, which is consistent with the theory of radiative alignment of elongated dust grains, where the major axis of dust grains is perpendicular to the radiation flux. Furthermore, the morphology of the polarization vectors at 3.1 mm is completely different from those at 1.3 mm. We interpret that the polarization at 3.1 mm to be dominated by the grain alignment with the radiative flux producing azimuthal polarization vectors, while the self-scattering dominates at 1.3 mm and produces the polarization vectors parallel to the minor axis of the disk. By modeling the total polarization fraction with a single grain population model, the maximum grain size is constrained to be 100 µm, which is smaller than the previous predictions based on the spectral index between ALMA at 3 mm and VLA at 7 mm.

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“…POL-2 with SCUBA-2 on JCMT is a facility that can map the B-field within cold dense cores and filaments on scales of ∼1000-2000au in nearby star-forming regions, such as those in the Gould Belt. As such, it can provide a link between the B-field measured on arcminute scales by Planck (Planck Collaboration et al 2015) and BLASTPol (e.g., Matthews et al 2014) with measurements made on arcsecond scales by interferometers such as the Submillimeter Array (SMA; e.g., Girart et al 2006;Tang et al 2010;Chen et al 2012), Combined Array for Research in Millimeter-wave Astronomy (CARMA; e.g., Hull et al 2013Hull et al , 2014, and the Atacama Large Millimeter/submillimeter Array (ALMA; e.g., Cortes et al 2016;Nagai et al 2016). This intermediate-size scale is crucial to testing theoretical models of star formation.…”

Section: Theoretical Modelsmentioning

confidence: 99%

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

Ward-Thompson

Pattle

Bastien

et al. 2017

ApJ

106

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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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Alma Science Verification Data: Millimeter Continuum Polarimetry of the Bright Radio Quasar 3c 286

Cited by 53 publications

References 27 publications

ALMA Observations of Dust Polarization and Molecular Line Emission from the Class 0 Protostellar Source Serpens SMM1

ALMA Observations of Dust Polarization and Molecular Line Emission from the Class 0 Protostellar Source Serpens SMM1

The Evidence of Radio Polarization Induced by the Radiative Grain Alignment and Self-scattering of Dust Grains in a Protoplanetary Disk

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

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