The impact of AGN-driven winds on physical and observable galaxy sizes
The impact of AGN-driven winds on physical and observable galaxy sizes
复制标题
AGN 驱动的风对物理和可观测星系大小的影响
DOI：
10.1093/mnras/stad1528
复制
发表时间：
2023
影响因子：
4.8
通讯作者：
Moreno, J.
中科院分区：
文献类型：
--
作者：
Cochrane, R. K.;Anglés-Alcázar, D.;Mercedes-Feliz, J.;Hayward, C. C.;Faucher-Giguère, C-A;Wellons, S.;Terrazas, B. A.;Wetzel, A.;Hopkins, P. F.;Moreno, J.
没有活动星系核（AGN）的反馈，模拟的大质量恒星形成星系相对于观测到的星系而言变得过于紧凑。在本文中，我们执行高分辨率的再模拟的大规模（）星系atz 2.3，来自现实环境中的反馈（FIRE）项目。在没有AGN反馈的模拟中，星系经历了快速的星暴和半质量半径的收缩。我们实验驱动机械AGN风，使用最先进的超拉格朗日细化技术，以提高粒子分辨率。这些风降低了星系内部区域的气体表面密度，抑制了致密的星暴，并保持了近似恒定的半质量半径。利用辐射传递，我们研究了活动星系核反馈对多波长连续辐射的大小和范围的影响。当包含活动星系核风时，相对于没有活动星系核风的情况，压缩的尘埃星爆导致远红外波段的通量降低（由于星星形成减少），但光学到近红外波段的通量增加（由于尘埃衰减减少，尽管星星形成率降低）。当不包括活动星系核风时，远红外半光半径从0.01减小到0.01，而当包括活动星系核风时，远红外半光半径增加到0.01。有趣的是，在光学近红外波长的半光半径保持近似恒定，模拟与活动星系核风。在没有风的情况下，尽管快速压缩，但这种情况仍然发生，这是由于星系内部区域的重尘埃遮蔽。这项工作突出了在比较模拟和观测到的星系种群时，前向建模的重要性。
Without active galactic nucleus (AGN) feedback, simulated massive, star-forming galaxies become too compact relative to observed galaxies atz≲ 2. In this paper, we perform high-resolution re-simulations of a massive () galaxy atz∼ 2.3, drawn from the Feedback in Realistic Environments (FIRE) project. In the simulation without AGN feedback, the galaxy experiences a rapid starburst and shrinking of its half-mass radius. We experiment with driving mechanical AGN winds, using a state-of-the-art hyper-Lagrangian refinement technique to increase particle resolution. These winds reduce the gas surface density in the inner regions of the galaxy, suppressing the compact starburst and maintaining an approximately constant half-mass radius. Using radiative transfer, we study the impact of AGN feedback on the magnitude and extent of the multiwavelength continuum emission. When AGN winds are included, the suppression of the compact, dusty starburst results in lowered flux at FIR wavelengths (due to decreased star formation) but increased flux at optical-to-near-IR wavelengths (due to decreased dust attenuation, in spite of the lowered star formation rate), relative to the case without AGN winds. The FIR half-light radius decreases from ∼1 toinwhen AGN winds are not included, but increases towhen they are. Interestingly, the half-light radius at optical-NIR wavelengths remains approximately constant over, for simulations with and without AGN winds. In the case without winds, this occurs despite the rapid compaction, and is due to heavy dust obscuration in the inner regions of the galaxy. This work highlights the importance of forward-modelling when comparing simulated and observed galaxy populations.