Fig. 3.
Same as Fig. 1b, but compared to the distribution of the young and instrinsically bright open clusters sample (see Sect. 2.2) shown by the black dots. The size of the dots is proportional to the number of cluster members brighter than absolute magnitude MG > 0 (see text). Solid lines show the spiral arm model of Taylor & Cordes (1993), which is based on HII regions.
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