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Probing the Initial Mass Function in the Early Universe: Direct Measurements in the Boötes I Ultrafaint Dwarf Galaxy with JWST/NIRCam

  • Authors: Keyi Ding, 可怿 丁, Mario Gennaro, Roberto J. Avila, Massimo Ricotti, Rachael L. Beaton, Martha L. Boyer, Thomas M. Brown, Annalisa Calamida, Santi Cassisi, Vedant Chandra, Roger E. Cohen, Matteo Correnti, Denija Crnojević, Kareem El-Badry, Marla Geha, Puragra Guhathakurta, Nitya Kallivayalil, Evan N. Kirby, Kristen. B. W. McQuinn, Alessandro Savino, Cheyanne Shariat, Joshua D. Simon, Daniel R. Weisz

Keyi Ding et al 2026 The Astrophysical Journal 1009 .

  • Provider: AAS Journals

Caption: Figure 3.

Luminosity function of the input magnitudes (blue) and the recovered magnitudes (orange) of the artificial stars in the F150W (top) and F322W2 (bottom) filters. The ratio of these functions (black line) represents the photometric completeness as a function of magnitude, and the error bars represent the rms variation when grouping the ASTs by mosaic tiles and SW chips. Red vertical dashed lines mark the 50% completeness limits, while the top x-axis displays the corresponding typical stellar masses based on the stellar model.

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