Astronomy and Astrophysics, volume 620A, 26-26 (2018/12-1)
Dust spectrum and polarisation at 850 µm in the massive IRDC G035.39-00.33.
JUVELA M., GUILLET V., LIU T., RISTORCELLI I., PELKONEN V.-M., ALINA D., BRONFMAN L., EDEN D.J., KIM K.T., KOCH P.M., KWON W., LEE C.W., MALINEN J., MICELOTTA E., MONTILLAUD J., RAWLINGS M.G., SANHUEZA P., SOAM A., TRAFICANTE A., YSARD N. and ZHANG C.-P.
Abstract (from CDS):
Context. The sub-millimetre polarisation of dust emission from star-forming clouds carries information on grain properties and on the effects that magnetic fields have on cloud evolution.
Aims. Using observations of a dense filamentary cloud G035.39-00.33, we aim to characterise the dust emission properties and the variations of the polarisation fraction.
Methods. JCMT SCUBA-2/POL-2 observations at 850µm were combined with Planck 850µm (353GHz) data to map polarisation fraction at small and large scales. With previous total intensity SCUBA-2 observations (450 and 850µm) and Herschel data, the column densities were determined via modified black-body fits and via radiative transfer modelling. Models were constructed to examine how the observed polarisation angles and fractions depend on potential magnetic field geometries and grain alignment processes.
Results. POL-2 data show clear changes in the magnetic field orientation. These are not in contradiction with the uniform orientation and almost constant polarisation fraction seen by Planck, because of the difference in the beam sizes and the POL-2 data being affected by spatial filtering. The filament has a peak column density of N(H2)∼7x1022cm–2, a minimum dust temperature of T∼12K, and a mass of ∼4300M☉ for the area N(H2)>5x1021cm–2. The estimated average value of the dust opacity spectral index is β∼1.9. The ratio of sub-millimetre and J-band optical depths is τ (250µm)/τ(J)∼2.5x10–3, more than four times the typical values for diffuse medium. The polarisation fraction decreases as a function of column density to p∼1% in the central filament. Because of noise, the observed decrease of p(N) is significant only at N(H2)>2x1022cm–2. The observations suggest that the grain alignment is not constant. Although the data can be explained with a complete loss of alignment at densities above ∼104cm–3 or using the predictions of radiative torques alignment, the uncertainty of the field geometry and the spatial filtering of the SCUBA-2 data prevent strong conclusions.
Conclusions. The G035.39-00.33 filament shows strong signs of dust evolution and the low polarisation fraction is suggestive of a loss of polarised emission from its densest parts.
© ESO 2018
ISM: clouds - infrared: ISM - submillimeter: ISM - dust, extinction - stars: formation - stars: protostars
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