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Resolving the Polarized Dust Emission of the Disk around the Massive Star Powering the HH 80-81 Radio Jet

AuthorsGirart, J. M.; Fernández-López, M.; Li, Z. -Y.; Yang, H.; Estalella, R.; Anglada, Guillem ; Áñez-López, N.; Busquet, G.; Carrasco-González, C.; Curiel, S.; Galvan-Madrid, R.; Gómez Rivero, José Francisco ; de Gregorio-Monsalvo, I.; Jiménez-Serra, I.; Krasnopolsky, R.; Martí, Josep; Osorio, Mayra ; Padovani, M.; Rao, R.; Rodríguez, L. F.; Torrelles, José María
KeywordsAccretion, accretion disks
ISM:individual objects (GGD27, HH 80-81, IRAS 18162-2048)
Issue Date2018
PublisherIOP Publishing
CitationAstrophysical Journal Letters 856(2): L27 (2018)
AbstractHere we present deep (16 μJy beam), very high (40 mas) angular resolution 1.14 mm, polarimetric, Atacama Large Millimeter/submillimeter Array (ALMA) observations toward the massive protostar driving the HH 80-81 radio jet. The observations clearly resolve the disk oriented perpendicularly to the radio jet, with a radius of ≃0.″171 (∼291 au at 1.7 kpc distance). The continuum brightness temperature, the intensity profile, and the polarization properties clearly indicate that the disk is optically thick for a radius of R ≲ 170 au. The linear polarization of the dust emission is detected almost all along the disk, and its properties suggest that dust polarization is produced mainly by self-scattering. However, the polarization pattern presents a clear differentiation between the inner (optically thick) part of the disk and the outer (optically thin) region of the disk, with a sharp transition that occurs at a radius of ∼0.″1 (∼170 au). The polarization characteristics of the inner disk suggest that dust settling has not occurred yet with a maximum dust grain size between 50 and 500 μm. The outer part of the disk has a clear azimuthal pattern but with a significantly higher polarization fraction compared to the inner disk. This pattern is broadly consistent with the self-scattering of a radiation field that is beamed radially outward, as expected in the optically thin outer region, although contribution from non-spherical grains aligned with respect to the radiative flux cannot be excluded.© 2018. The American Astronomical Society. All rights reserved..
Publisher version (URL)http://dx.doi.org/10.3847/2041-8213/aab76b
Identifiersdoi: 10.3847/2041-8213/aab76b
issn: 2041-8213
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