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Imaging of 2-mm dust continuum emission towards S106 FIR and its spectral energy distribution

Published online by Cambridge University Press:  03 August 2017

Ray S. Furuya
Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125, Firenze, Italy
Yoshimi Kitamura
Institute of Space and Astronautical Science, Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan
Alwyn Wootten
National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
Mark J. Claussen
National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA
Ryohei Kawabe
Nobeyama Radio Observatory, Nobeyama 411, Minamimaki, Minamisaku, Nagano 384-1305, Japan


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The class 0 source S106 FIR is a good candidate to investigate a very early phase of star formation because of the presence of an AU-scale Microjet, discovered by our VLBA H2O maser observations and the absence of an extensive CO outflow. In order to reveal the properties of S106 FIR, we conducted observations of 2-mm continuum emission with the Nobeyama Millmeter Array. We detected a weak compact continuum emission around S106 FIR. We analysed the spectral energy distribution of S106 FIR. It is found that the dust temperature and the β index of the dust opacity range from 31 to 55 K and from 1.4 to 1.6, respectively. Using these results, we computed the mass of the core aound S106 FIR and the bolometric luminosity of 3.1 to 5.8 M and 230 to 1070 L, respectively.

Part 1. Star Formation
Copyright © Astronomical Society of the Pacific 2002 


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