The dependence of stellar age distributions on GMC environment

Abstract

In this Letter, we analyse the distributions of stellar ages in Giant Molecular Clouds (GMCs) in spiral arms, inter-arm spurs, and at large galactic radii, where the spiral arms are relatively weak. We use the results of numerical simulations of galaxies, which follow the evolution of GMCs and include star particles where star formation events occur. We find that GMCs in spiral arms tend to have predominantly young (< 10 Myr) stars. By contrast, clouds which are the remainders of spiral arm GMAs that have been sheared into inter-arm GMCs, contain fewer young (< 10 Myr) stars, and more ~20 Myr stars. We also show that clouds which form in the absence of spiral arms, due to local gravitational and thermal instabilities, contain preferentially young stars. We propose the age distributions of stars in GMCs will be a useful diagnostic to test different cloud evolution scenarios, the origin of spiral arms, and the success of numerical models of galactic star formation. We discuss the implications of our results in the context of Galactic and extragalactic molecular clouds.

5 pages, 2 figures, accepted for publication in MNRAS Letters

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• The Galactic Census of High- and Medium-mass Protostars. IV. Molecular Clump Radiative Transfer, Mass Distributions, Kinematics, and Dynamical Evolution
• The properties, origin and evolution of stellar clusters in galaxy simulations and observations
• Star Formation Histories of the LEGUS Spiral Galaxies. I. The flocculent spiral NGC 7793
• Molecular cloud formation as seen in synthetic Hi and molecular gas observations
• Cloud angular momentum and effective viscosity in global SPH simulations with feedback
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