Tidal interactions and the formation of Magellanic spiral galaxies

Details Tidal interactions and the formation of Magellanic spiral galaxies Tidal interactions and the formation of Magellanic spiral galaxies

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993egte.conf..235o&link_type=abstract

In NASA. Ames Research Center, The Evolution of Galaxies and Their Environment p 235-237 (SEE N93-26706 10-90)

Astronomy and Astrophysics

Astronomy

1

Disk Galaxies, Galactic Evolution, Magellanic Clouds, Spiral Galaxies, Tides, Asymmetry, Barred Galaxies, Brightness, H I Regions, Infrared Astronomy, Irregular Galaxies, Luminosity, Morphology

Scientific paper

The closest, brightest and best resolved galaxy in the sky, the Large Magellanic Cloud, is a prototype of the late-type disk systems referred to collectively as barred Magellanic spiral galaxies (SBm). These systems occupy a pivotal stage in the Hubble sequence since they represent the transition from spiral disk galaxies to chaotic, irregular galaxies and are characterized by an asymmetric spiral arm which emanates from one end of a high surface brightness bar. We present evidence that the formation of the one-armed spiral morphology involves the tidal interaction with a companion galaxy. In summary the major points of our observational investigation include the following: (1) The vast majority of one-armed spiral galaxies possess bright nearby neighbors which appear to be physically associated. (2) The HI gas distribution and kinematics of one pair of SBm galaxies clearly reveal this system to be tidally interacting. (3) The infrared properties of the bars in two SBm galaxies support optical studies of bar luminosity profiles in late-type systems, and also suggest that the formation of compact star forming regions in these bars may not be uncommon.

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