A direct test of density wave theory in a grand-design spiral galaxy

TL;DR

This study provides the first direct measurement of the pattern speed in a grand-design spiral galaxy, supporting the density wave theory by showing it remains nearly constant across different radii.

Contribution

It introduces a novel method to directly measure the pattern speed using stellar population offsets, offering new evidence for the quasi-stationary density wave theory.

Findings

Pattern speed varies little with radius

Results support the density wave theory

Method proves effective for measuring pattern speed

Abstract

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.