2024-03-28T14:04:22Zhttp://digital.csic.es/dspace-oai/requestoai:digital.csic.es:10261/2141282022-11-07T11:14:43Zcom_10261_97com_10261_4com_10261_45col_10261_350col_10261_298
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Girart, Josep Miquel
author
Fernández-López, M.
author
Li, Z. -Y.
author
Yang, H.
author
Estalella, R.
author
Anglada-Escudé, Guillem
author
Áñez-López, N.
author
Busquet, G.
author
Carrasco-González, C.
author
Curiel, S.
author
Galván-Madrid, R.
author
Gómez Rivero, José Francisco
author
de Gregorio-Monsalvo, Itziar
author
Jiménez-Serra, I.
author
Krasnopolsky, R.
author
Martí, Josep
author
Osorio, Mayra
author
Padovani, Marco
author
Rao, R.
author
Rodríguez, L. F.
author
Torrelles, José María
author
2018
Here 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..
Astrophysical Journal Letters 856(2): L27 (2018)
http://hdl.handle.net/10261/214128
10.3847/2041-8213/aab76b
http://dx.doi.org/10.13039/501100003329
http://dx.doi.org/10.13039/501100000780
http://dx.doi.org/10.13039/501100005739
http://dx.doi.org/10.13039/501100003141
http://dx.doi.org/10.13039/100000104
http://dx.doi.org/10.13039/100000001
http://dx.doi.org/10.13039/501100000271
Accretion, accretion disks
ISM:individual objects (GGD27, HH 80-81, IRAS 18162-2048)
Stars:formation
Resolving the Polarized Dust Emission of the Disk around the Massive Star Powering the HH 80-81 Radio Jet