Structure and kinematics of the molecular spiral arms in M51

Details Structure and kinematics of the molecular spiral arms in M51 Structure and kinematics of the molecular spiral arms in M51

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987nascp2466..315r&link_type=abstract

Star formation in galaxies, Proceedings of a conference at the California Institute of Technology, Pasadena, California, June 16

Computer Science

Density Wave Model, Flow Velocity, Galactic Structure, Kinematics, Molecular Clouds, Molecular Gases, Background Radiation, Carbon Monoxide, Emission Spectra, Space Observations (From Earth)

Scientific paper

Mapping of the CO(1-0) emission from the spiral galaxy was made with the Onsala 20 m antenna. The observations show that the emission is considerably enhanced in spiral arms which appear to originate as intense ridges of emission about 1 kpc from the nucleus. One of the main objectives for the 1986 observations was to study the variations of the tangential velocity component of molecular gas across a spiral arm. The radial velocity was found to have a velocity shift similar to that predicted by the density wave theory. The present (1986) observations of the inner southern spiral arm of M51 show that the tangential velocity component also behaves in a way which conforms with the density wave model. The molecular arms were compared with the H alpha ionized gas arms of Tully (1974) and it was found that the ionized gas appears to have its maximum intensity slightly outside the molecular arm.

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