Azimuthal propagation of star formation in nearby spiral galaxies: NGC 628, NGC 3726 and NGC 6946
F. Sakhibov, A. S. Gusev, and C. Hemmerich
TL;DR
This paper investigates how star formation propagates azimuthally in nearby spiral galaxies by analyzing spatial separations and gas velocity fields to determine the corotation radius, revealing the influence of spiral density waves.
Contribution
It introduces a combined morphological and Fourier analysis method to accurately locate the corotation radius in spiral galaxies, enhancing understanding of star formation dynamics.
Findings
Corotation radius determined for NGC 628, NGC 3726, NGC 6946
Fourier analysis confirms morphological estimates
Star formation patterns linked to spiral density waves
Abstract
Star formation induced by a spiral shock wave, which in turn is generated by a spiral density wave, produces an azimuthal age gradient across the spiral arm, which has opposite signs on either side of the corotational resonance. An analysis of the spatial separation between young star clusters and nearby HII regions made it possible to determine the position of the corotation radius in the studied galaxies. Fourier analysis of the gas velocity field in the same galaxies independently confirmed the corotation radius estimates obtained by the morphological method presented here.
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