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SIO maser survey of the Bulge IRAS sources

Published online by Cambridge University Press:  07 August 2017

H. Izumiura ,
T. Ono ,
I. Yamamura ,
K. Okumura ,
T. Onaka ,
S. Deguchi ,
N. Ukita ,
O. Hashimoto  and
Y. Nakada
H. Izumiura
Affiliation:
Department of Astronomy and Earth Sciences, Tokyo Gakugei University 4-1-1 Nukui-kita, Koganei, Tokyo 184, Japan
T. Ono
Affiliation:
Department of Astronomy and Earth Sciences, Tokyo Gakugei University 4-1-1 Nukui-kita, Koganei, Tokyo 184, Japan
I. Yamamura
Affiliation:
Department of Astronomy, Faculty of Science, University of Tokyo Bunkyo-ku, Tokyo 113, Japan
K. Okumura
Affiliation:
Department of Astronomy, Faculty of Science, University of Tokyo Bunkyo-ku, Tokyo 113, Japan
T. Onaka
Affiliation:
Department of Astronomy, Faculty of Science, University of Tokyo Bunkyo-ku, Tokyo 113, Japan
S. Deguchi
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory Mimamimaki, Minamisaku, Nagano 384-13, Japan
N. Ukita
Affiliation:
Nobeyama Radio Observatory, National Astronomical Observatory Mimamimaki, Minamisaku, Nagano 384-13, Japan
O. Hashimoto
Affiliation:
Department of Applied Physics, Seikei University 3-3-1 Kichijouji-kita, Musashino, Tokyo 180, Japan
Y. Nakada
Affiliation:
Kiso Observatory, Faculty of Science, University of Tokyo Mitake-mura, Kiso-gun, Nagano, 397-01, Japan

Abstract

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SiO maser emission from the Bulge IRAS sources has been searched by the v=1, J=1−0 and v=2, J=1—0 transitions to investigate the kinematics of the Galactic Bulge, resulting in a sample of 124 line-of-sight velocities. The rotation velocity, velocity dispersion, and velocity offset at l = 0° for the sample are found to be , and —18.2±9.7 km s−1, respectively (80% confidence interval). Furthermore we find trends for the rotation velocity and velocity dispersion to decrease with distance from the galactic plane. These trends are supported by a larger sample constructed by incorporating other available velocity data on the Bulge IRAS sources. The rotation velocity and velocity dispersion are expressed as 15.6—1.23x|b(deg)| km s−1 deg−1 and 101−3.6x |b(deg)| km s−1, respectively. The implications of the observed quantities are discussed.

Type
Contributed Papers
Information
Symposium - International Astronomical Union , Volume 153: Galactic Bulges , 1993 , pp. 303 - 308
Copyright
Copyright © Kluwer 1993 

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