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The Origin of the [C II] Deficit in a Simulated Dwarf Galaxy Merger-driven Starburst

  • Authors: Thomas G. Bisbas, Stefanie Walch, Thorsten Naab, Natalia Lahén, Rodrigo Herrera-Camus, Ulrich P. Steinwandel, Constantina M. Fotopoulou, Chia-Yu Hu, Peter H. Johansson

Thomas G. Bisbas et al 2022 The Astrophysical Journal 934 .

  • Provider: AAS Journals

Caption: Figure 5.

Phase plots (T gas vs. total H nucleus, n H, number density) weighted with L CII for snapshots at t = 40, 70, 120, 170, 250, and 390 Myr. Before the second encounter (top row), L CII originates from the WNM (see Figure 4). Once the second encounter occurs (bottom row), H II regions form and their ionized gas takes over as the main contributor to the total L CII. The horizontal straight line at ﹩\mathrm{log}{T}_{\mathrm{gas}}=4﹩ is the gas temperature of the interior of H II regions.

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