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Stellar Populations and Molecular Gas Composition in the Low-metallicity Environment of WLM

  • Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Leslie K. Hunt, Rosalia O'Brien, Elias Brinks, Phil Cigan, Monica Rubio, Rogier A. Windhorst, Rolf A. Jansen, Elijah P. Mathews

Haylee N. Archer et al 2025 The Astronomical Journal 169 .

  • Provider: AAS Journals

Caption: Figure 6.

Left: F336W–F438W vs. F438W–F555W color–color diagram for stars inside the PDR and outside the CO cores (blue) and stars inside the PDR and projected inside the CO cores (orange). Right: F336W–F438W vs. F438W–F555W color–color diagram for stars outside the PDR and outside the CO cores (pink), and stars outside the PDR and projected inside the CO cores (green). Stars detected in all filters are represented by circles (∘), while stars that were not detected in the F275W filter are represented by diamonds (♢). The black arrow in each plot shows the reddening vector for AV = 0.35, the mean AV of stars in WLM measured by Y. Wang et al. (2022), assuming SMC-like extinction. The error bars in the upper-left corner of each plot demonstrate the mean uncertainty associated with the data shown.

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