将射电活动星系核（radio AGN）生命周期与反馈关联：年轻射电AGN的电离气体扰动更显著
Connecting the radio AGN life cycle to feedback: Ionised gas is more disturbed in young radio AGN
AI总结：
本研究通过划分射电AGN生命周期阶段，发现年轻射电AGN的电离气体扰动概率远高于演化源，喷流强影响集中在活动初始阶段，且差异随射电光度升高而增大。
摘要：
在射电活动星系核（radio AGN）的宿主星系中，由喷流驱动的反馈导致的气体运动学扰动是一种被广泛观测到的现象。模拟预测，喷流对周围气体的影响会随着喷流的演化而改变。将射电AGN划分为不同演化阶段并研究其对气体运动学的影响，可为此现象提供有价值的洞见。我们对红移z~0.8以内的5720个射电AGN样本开展了[OIII]气体运动学的系统性研究，样本的1.4 GHz光度范围宽达约10^22.5–10^28 W/Hz，其中包含1693个[OIII]探测源。利用LOFAR和VLA巡天在144–3000 MHz的宽频率覆盖优势，我们测定了射电谱形，并据此将源划分为射电AGN生命周期的不同阶段。我们从SDSS光谱中提取[OIII]运动学信息，并将其与生命周期相关联。我们的主要结论是：在z<0.4的红移范围内，峰谱（PS，代表活动年轻阶段）源的[OIII]气体发生扰动的概率约为非峰谱（NPS，代表演化程度更高的源）源的3倍；在z>0.4时，该倍数变为约2倍。这表明平均而言，喷流的强影响仅限于射电AGN生命周期的初始阶段，在后期阶段，喷流对气体的影响更为温和。我们还测定了这一趋势对1.4GHz光度和[OIII]光度的依赖关系，发现两类源之间的差异随1.4GHz光度的升高而增大。1.4GHz光度L_1.4GHz>10^25 W/Hz的年轻射电AGN对[OIII]的影响最为极端。通过叠加分析，我们进一步得以追踪高频峰谱（即最年轻）、低频峰谱（“相对没那么年轻”）和非峰谱（已演化）射电AGN对[OIII]影响的变化过程。
英文摘要：
In the host galaxies of radio AGN, kinematically disturbed gas due to jet-driven feedback is a widely observed phenomenon. Simulations predict that the impact of jets on the surrounding gas changes as they grow. Useful insights into this phenomenon can be obtained by characterising radio AGN into different evolutionary stages and studying their impact on gas kinematics. We present a systematic study of the [OIII] gas kinematics for a sample of 5720 radio AGN up to $z\sim0.8$ with a large 1.4 GHz luminosity range of $\approx10^{22.5}-10^{28}$W/Hz, and 1693 [OIII] detections. Taking advantage of the wide frequency coverage of LOFAR and VLA surveys from $144-3000$MHz, we determine the radio spectral shapes, using them to characterise sources into different stages of the radio AGN life cycle. We determine the [OIII] kinematics from SDSS spectra and link it to the life cycle. Our main conclusion is that the [OIII] gas is $\sim$3 times more likely to be disturbed in the peaked spectrum (PS) sources (that represent a young phase of activity) than non-peaked spectrum (NPS) sources (that represent more evolved sources) at $z<0.4$. This changes to a factor of $\sim$2 at $z>0.4$. This shows that on average, the strong impact of jets is limited to the initial stages of the radio AGN life cycle. At later stages, the impact on gas is more gentle. We also determine the dependence of this trend on 1.4GHz and [OIII] luminosities and find that the difference between the two groups increases with 1.4GHz luminosity. Young radio AGN with $L_\mathrm{1.4GHz}>10^{25}$W/Hz have the most extreme impact on [OIII]. Using a stacking analysis, we are further able to trace the changing impact on [OIII] in the high-frequency peaked spectrum (i.e. youngest), low-frequency peaked spectrum ("less young"), and non-peaked spectrum (evolved) radio AGN.
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