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The Small Sizes and High Implied Densities of “Little Red Dots” with Balmer Breaks Could Explain Their Broad Emission Lines without an Active Galactic Nucleus

  • Authors: Josephine F. W. Baggen, Pieter van Dokkum, Gabriel Brammer, Anna de Graaff, Marijn Franx, Jenny Greene, Ivo Labbé, Joel Leja, Michael V. Maseda, Erica J. Nelson, Hans-Walter Rix, Bingjie Wang, 冰洁 王, Andrea Weibel

Josephine F. W. Baggen et al 2024 The Astrophysical Journal Letters 977 .

  • Provider: AAS Journals

Caption: Figure 1.

The spectra (gray) and best-fit model (dark blue) with maximal stellar mass of three Balmer break galaxies, obtained from B. Wang et al. (2024b). We also show 1″ × 1″ images in four different bands, F115W, F200W, F356W, and F444W. The dotted lines indicate the location of the Balmer break (black), [O III] line (red), and Hβ (blue) line, which are relevant in this work. For information on other emission lines, see B. Wang et al. (2024b).

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