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We analyze recent observations of the spiral arm width in the Milky Way, as afunction of the galactic radius, and we compare this relation with theprediction from the density wave theory. We use the following method: in eachspiral arm, we concentrate on the separation (or offset) between thestarforming region (radio masers) near the shock front of a density wave, andthe aged star region (diffuse CO gas) near the potential minimum of a densitywave; we take this separation between these two tracers as the arm width.  New results: we find a typical separation (maser to diffuse CO gas) near 250+/- 50 pc, and an increase of this separation with galactic radius of about 25+/- 5 pc per kpc. We note that, as expected, this separation is somewhatsmaller than that found earlier between the dust lane and the aged star region.Overall, these results supports the basics of a density wave.

A New Multi-Tracer Approach to Defining the Spiral arm width in the Milky Way