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Keywords:

  • galaxies: dwarf;
  • galaxies: kinematics and dynamics;
  • galaxies: spiral

ABSTRACT

The observed rotation curves of disc galaxies, ranging from late-type dwarf galaxies to early-type spirals, can be fitted remarkably well simply by scaling up the contributions of the stellar and H i discs. This ‘baryonic scaling model’ can explain the full breadth of observed rotation curves with only two free parameters. For a small fraction of galaxies, in particular early-type spiral galaxies, H i scaling appears to fail in the outer parts, possibly due to observational effects or ionization of H i. The overall success of the baryonic scaling model suggests that the well-known global coupling between the baryonic mass of a galaxy and its rotation velocity (known as the baryonic Tully–Fisher relation) applies at a more local level as well, and it seems to imply a link between the baryonic mass distribution and the distribution of total mass (including dark matter).