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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 4.

Sharpness (left) and χ (right) values as a function of Vega magnitude for all sources detected in the F625W filter. Gray vertical and horizontal lines are shown to demarcate which sources were stars or galaxies. Sources with a Vega magnitude brighter than 24 were determined to be stars if their sharpness was less than zero (bottom-left quadrant in the sharpness plot), while sources with a Vega magnitude fainter than 24 were determined to be stars if both their sharpness was less than zero and their χ was less than 1 (bottom-right quadrant in both plots). Sources determined to be galaxies are shown as gold points, while sources determined to be stars are shown as purple stars.

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