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Disk Structure of the H2O Maser IC 1396N

Published online by Cambridge University Press:  12 April 2016

I. E. Val’tts ,
V. I. Slysh ,
V. Migenes ,
T. Umemoto ,
R. Furuya ,
R. Kawabe ,
E. B. Fomalont ,
H. Hirabayashi  and
M. Inoue
I. E. Val’tts
Affiliation:
Astro Space Center, Lebedev Physical Institute, Moscow, Russia
V. I. Slysh
Affiliation:
Astro Space Center, Lebedev Physical Institute, Moscow, Russia
V. Migenes
Affiliation:
National Astronomical Observatory, Japan
T. Umemoto
Affiliation:
National Astronomical Observatory, Japan
R. Furuya
Affiliation:
National Astronomical Observatory, Japan
R. Kawabe
Affiliation:
National Astronomical Observatory, Japan
E. B. Fomalont
Affiliation:
Institute of Space and Astronautical Science, Japan
H. Hirabayashi
Affiliation:
Institute of Space and Astronautical Science, Japan
M. Inoue
Affiliation:
Nobeyama Radio Observatory, Japan

Abstract

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The VLBA map of the H2O maser IC 1396N, which was obtained during the VSOP pre-launch survey, shows an ordered position of maser spots. The maser spots are located along an almost straight line with the separation between extreme maser spots of 20 mas. The radial velocity varies along the line from by 3 km s−1. In total 9 maser features have been located on the line, all of them unresolved by the VLBA beam. This geometry is consistent with the disk model of masers. The mass of the disk is estimated between 10−7 and 10−4 M⊙, depending on the thickness and density. The disk must be supported by a central star with the mass of about 0.07 M⊙. The H2O maser in IC 1396N may be a proto-planetary disk around a low mass protostar in the process of accretion.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 164: Radio Emission from Galactic and Extragalactic Compact Sources , 1998 , pp. 365 - 366
Copyright
Copyright © Astronomical Society of the Pacific 1998

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