A direct test of density wave theory in a grand-design spiral galaxy
  The exact nature of the arms of spiral galaxies is still an open question. It
has been widely assumed that spiral arms in galaxies with two distinct
symmetrical arms are the products of density waves that propagate around the
disk, with the spiral arms being visibly enhanced by the star formation that is
triggered as the passing wave compresses gas in the galaxy disk. Such a
persistent wave would propagate with an approximately constant angular speed,
its pattern speed Op. The quasi-stationary density wave theory can be tested by
measuring this quantity and showing that it does not vary with radius in the
galaxy. Unfortunately, this measurement is difficult because Op is only
indirectly connected to observables such as the stellar rotation speed. Here,
we use the detailed information on stellar populations of the grand-design
spiral galaxy UGC 3825, extracted from spectral mapping, to measure the offset
between young stars of a known age and the spiral arm in which they formed,
allowing the first direct measure of Op at a range of radii. The offset in this
galaxy is found to be as expected for a pattern speed that varies little with
radius, indicating consistency with a quasi-stationary density wave, and
lending credence to this new method.
