Spiral structure of M51: Streaming motions across the spiral arms

Details Spiral structure of M51: Streaming motions across the spiral arms Spiral structure of M51: Streaming motions across the spiral arms

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990nascp3084..298t&link_type=abstract

In NASA, Ames Research Center, The Interstellar Medium in External Galaxies: Summaries of Contributed Papers p 298-300 (SEE N91-

Computer Science

H Alpha Line, Hydrogen, Spiral Galaxies, Velocity Distribution, Angular Resolution, Atoms, Density Wave Model, Fabry-Perot Spectrometers, Radial Velocity, Radio Telescopes, Rotation, Symmetry

Scientific paper

The atomic hydrogen (HI) and the H alpha emission line in the grand-design spiral galaxy M51 have been observed with the Westerbork Synthesis Radio Telescope and the Taurus Fabry-Perot imaging spectrometer, respectively. Across the inner spiral arms significant tangential and radial velocity gradients are detected in the H alpha emission after subtraction of the axi-symmetric component of the velocity field. The shift is positive on the inside and negative on the outside of the northern arm. Across the southern arm this situation is reversed. The direction of the shifts is such that the material is moving inward and faster compared to circular rotation in both arms, consistent with the velocity perturbations predicted by spiral density wave models for gas downstream of a spiral shock. The observed shifts amount to 20 to 30 km (s-1), corresponding to streaming motions of 60 to 90 km (s-1) in the plane of the disk (inclination angle 20 degrees). Comparable velocity gradients have also been observed by Vogel et al. in the CO emission from the inner northern arm of M51. The streaming motions in M51 are about 2 to 3 times as large as the ones found in HI by Rots in M81, and successfully modelled by Visser with a self-consistent density wave model. Researchers have not been able to detect conclusively streaming motions in the HI emission from the arms, perhaps due to the relatively poor angular resolution (approx. 15 seconds) of the HI observations.

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