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A Face-on Accretion System in High Mass Star-Formation: Possible Dusty Infall Streams within 100 Astronomical Unit

Published online by Cambridge University Press:  16 July 2018

Kazuhito Motogi ,
Tomoya Hirota ,
Kazuo Sorai ,
Yoshinori Yonekura ,
Koichiro Sugiyama ,
Mareki Honma ,
Kotaro Niinuma ,
Kazuya Hachisuka ,
Kenta Fujisawa  and
Andrew J. Walsh
Kazuhito Motogi
Affiliation:
Graduate School of Sciences and Technology for Innovation, Yamaguchi University, Yoshida 1677-1, Yamaguchi 753-8512, Japan email: kmotogi@yamaguchi-u.ac.jp
Tomoya Hirota
Affiliation:
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan Department of Astronomical Sciences, SOKENDAI (The Graduate University for Advanced Studies), Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
Kazuo Sorai
Affiliation:
Department of Physics, Faculty of Science, Hokkaido University, Sapporo 060-0810, Japan Department of Cosmosciences, Graduate School of Science, Hokkaido University, Sapporo 060-0810, Japan
Yoshinori Yonekura
Affiliation:
Center for Astronomy, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan
Koichiro Sugiyama
Affiliation:
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan
Mareki Honma
Affiliation:
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Hoshigaoka 2-12, Mizusawa, Oshu, Iwate 023-0861, Japan
Kotaro Niinuma
Affiliation:
Graduate School of Sciences and Technology for Innovation, Yamaguchi University, Yoshida 1677-1, Yamaguchi 753-8512, Japan email: kmotogi@yamaguchi-u.ac.jp
Kazuya Hachisuka
Affiliation:
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Hoshigaoka 2-12, Mizusawa, Oshu, Iwate 023-0861, Japan
Kenta Fujisawa
Affiliation:
The Research Institute for Time Studies, Yamaguchi University, Yoshida 1677-1, Yamaguchi 753-8511, Japan
Andrew J. Walsh
Affiliation:
International Centre for Radio Astronomy Research, Curtin University, Bentley, WA 6102, Australia
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Abstract

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We report on interferometric observations of a face-on accretion system around the high mass young stellar object, G353.273+0.641. The innermost accretion system of 100-au radius was resolved in a 45-GHz continuum image taken with the Jansky Very Large Array. Our SED analysis indicated that the continuum could be explained by optically-thick dust emission. 6.7 GHz CH3OH masers associated with the same system were also observed with the Australia Telescope Compact Array. The masers showed a spiral-like, non-axisymmetric distribution with a systematic velocity gradient. The line-of-sight velocity field is explained by an infall motion along a parabolic streamline that falls onto the equatorial plane of the face-on system. The streamline is quasi-radial and reaches the equatorial plane at a radius of 16 au. The physical origin of such a streamline is still an open question and will be constrained by the higher-resolution thermal continuum and line observations with ALMA long baselines.

Keywords

ISM: individual objects (G353.273+0.641)–molecules–masers–radio continuum: ISM–stars: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S336: Astrophysical Masers: Unlocking the Mysteries of the Universe , September 2017 , pp. 267 - 270
Copyright
Copyright © International Astronomical Union 2017 

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