ALMA Observations of polarization from dust scattering in the IM lup protoplanetary disk
Author
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Hull, Charles L. H.
Author
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Yang, Haifeng
Author
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Li, Zhi-Yun
Author
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Kataoka, Akimasa
Author
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Stephens, Ian W.
Author
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Andrews, Sean
Author
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Bai, Xuening
Author
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Cleeves, L. Ilsedore
Author
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Hughes, A. Meredith
Author
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Looney, Leslie
Author
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Pérez, L. M.
Author
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Wilner, David
Admission date
dc.date.accessioned
2018-10-24T21:18:37Z
Available date
dc.date.available
2018-10-24T21:18:37Z
Publication date
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2018-06-10
Cita de ítem
dc.identifier.citation
Astrophysical Journal Volumen: 860 Número: 1 Número de artículo: 82
es_ES
Identifier
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10.3847/1538-4357/aabfeb
Identifier
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https://repositorio.uchile.cl/handle/2250/152233
Abstract
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We present 870 mu m ALMA observations of polarized dust emission toward the Class II protoplanetary disk IM. Lup. We find that the orientation of the polarized emission is along the minor axis of the disk, and that the value of the polarization fraction increases steadily toward the center of the disk, reaching a peak value of similar to 1.1%. All of these characteristics are consistent with models of self-scattering of submillimeter-wave emission from an optically thin inclined disk. The distribution of the polarization position angles across the disk reveals that, while the average orientation is along the minor axis, the polarization orientations show a significant spread in angles; this can also be explained by models of pure scattering. We compare the polarization with that of the Class I/II source HL. Tau. A comparison of cuts of the polarization fraction across the major and minor axes of both sources reveals that IM. Lup has a substantially higher polarization fraction than HL. Tau toward the center of the disk. This enhanced polarization fraction could be due a number of factors, including higher optical depth in HL. Tau, or scattering by larger dust grains in the more evolved IM. Lup disk. However, models yield similar maximum grain sizes for both HL. Tau (72 mu m) and IM. Lup (61 mu m, this work). This reveals continued tension between grain-size estimates from scattering models and from models of the dust emission spectrum, which find that the bulk of the (unpolarized) emission in disks is most likely due to millimeter-sized (or even centimeter-sized) grains.
es_ES
Patrocinador
dc.description.sponsorship
SOS award from NRAO
NASA
NNX 14AB38G
NAS 5-26555
NSF
AST-1313083
1716259
NASA through Hubble Fellowship grant - Space Telescope Science Institute
HST-HF2-51356.001-A