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

Abstract

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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.

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

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