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Kinematics of Molecules at the Galactic Centre

Published online by Cambridge University Press:  14 August 2015

B. J. Robinson
B. J. Robinson*
Affiliation:
Division of Radiophysics, CSIRO, Sydney, Australia

Abstract

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Dense gas clouds containing OH, CO, NH3 and H2CO are found in the inner part of the H1 nuclear disk. The molecular spectral lines allow direct observations of the kinematics of the gas near the galactic centre. Strong absorption of the thermal continuum sources by OH and H2CO shows that much of the gas on the near side of the centre can be located in a massive ‘ring’ expanding at 130 km s-1 which may have originated close to the nucleus about 106yr ago. Observations of CO emission from beyond the centre show that the far side of the ‘ring’ is expanding at a lower velocity, less than 90 km s-1. Observations of CO and NH3 emission with positive velocities for l < 360° are needed to establish whether the ‘ring’ is a continuous structure.

OH and H2CO are also observed to be falling towards the centre. There is no agreement as to the location of this infalling matter.

The nuclear regions of the Galaxy are compared with those of NGC 253, particularly in regard to expansional velocities, IR and radio emission, and OH absorption.

Type
Part 5: The Galactic Center
Information
Symposium - International Astronomical Union , Volume 60: Galactic Radio Astronomy , 1974 , pp. 521 - 535
Copyright
Copyright © Reidel 1974 

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