The Effect of Radiation and Supernovae Feedback on LyC Escape in Local Star-forming Galaxies

Cody A. Carr, Renyue Cen, Claudia Scarlata, Xinfeng Xu, Alaina Henry, Rui Marques-Chaves, Daniel Schaerer, Ricardo O. Amorín, M. S. Oey, Lena Komarova, Sophia Flury, Anne Jaskot, Alberto Saldana-Lopez, Zhiyuan Ji, Mason Huberty, Timothy Heckman, Göran Ostlin, Omkar Bait, Matthew James Hayes, Trinh Thuan, Danielle A. Berg, Mauro Giavalisco, Sanchayeeta Borthakur, John Chisholm, Harry C. Ferguson, Leo Michel-Dansac, Anne Verhamme, Gábor Worseck
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Abstract

Feedback is widely recognized as an essential condition for Lyman continuum (LyC) escape in star-forming galaxies. However, the mechanisms by which galactic outflows clear neutral gas and dust remain unclear. In this paper, we model the Mg II 2796\r{A}, 2804\r{A} absorption + emission lines in 29 galaxies taken from the Low-z LyC Survey (LzLCS) to investigate the impact of (radiation + mechanical) feedback on LyC escape. Using constraints on Mg$^+$ and photoionization models, we map the outflows' neutral hydrogen content and predict $f_{esc}^{LyC}$ with a multiphase wind model. We measure mass, momentum, and energy loading factors for the neutral winds, which carry up to 10% of the momentum and 1% of the energy in SFR-based deposition rates. We use SED template fitting to determine the relative ages of stellar populations, allowing us to identify radiation feedback dominant systems. We then examine feedback related properties (stellar age, loading factors, etc.) under conditions that optimize feedback efficiency, specifically high star formation rate surface density and compact UV half-light radii. Our findings indicate that the strongest leakers are radiation feedback dominant, lack Mg II outflows, but have extended broad components in higher ionization lines like [O III] 5007\r{A}, as observed by Amor\'in et al. (2024). In contrast, galaxies experiencing supernovae feedback typically exhibit weaker $f_{esc}^{LyC}$ and show evidence of outflows in both Mg II and higher ionization lines. We attribute these findings to rapid or "catastrophic" cooling in the radiation-dominant systems, which, given the low metallicities in our sample, are likely experiencing delayed supernovae.
辐射和超新星反馈对本地恒星形成星系中 LyC 逃逸的影响
反馈被广泛认为是恒星形成星系中莱曼连续光(LyC)逸出的必要条件。然而,星系外流清除中性气体和尘埃的机制仍不清楚。在本文中,我们模拟了低兹LyC巡天(LzLCS)中29个星系的Mg II 2796\r{A}, 2804\r{A} 吸收+发射线,以研究(辐射+机械)反馈对LyC逸出的影响。利用对 Mg$^+$ 和光离子化模型的约束,我们绘制了外流的中性氢含量图,并利用多相风模型预测了 $f_{esc}^{LyC}$。我们测量了中性风的质量、动量和能量负荷因子,它们携带了基于 SFR 的沉积率中高达 10% 的动量和 1% 的能量。我们使用 SED 模板拟合来确定恒星群的相对年龄,从而识别出辐射反馈主导系统。然后,我们考察了反馈相关特性(恒星年龄、负载因子等)在优化反馈效率条件下的表现,特别是高恒星形成率表面密度和紧凑的紫外半光速半径。我们的研究结果表明,最强的泄漏星系是辐射反馈占主导地位的,缺乏Mg II外流,但在较高电离线(如[OIII] 5007\r{A})中有扩展的宽成分,正如Amor\'in等人(2024年)所观测到的那样。相比之下,经历过超新星反馈的星系通常会表现出较弱的 $f_{esc}^{LyC}$,并在 Mg II 和较高电离线中显示出外流的证据。我们将这些发现归因于辐射主导系统的快速或 "灾难性 "冷却,鉴于我们样本中的低金属性,这些系统很可能正在经历延迟超新星。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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