论文标题
具有极高积聚率的超质量黑洞的无线电活动
Radio activity of supermassive black holes with extremely high accretion rates
论文作者
论文摘要
高和超级埃德丁顿积聚活性银河核（AGN）的无线电发射具有各种起源：持续的射流，磁化的电晕和风向流出。现在尚不清楚哪种领先的机制是负责观察到的无线电发射的领先机制，以及无线电发射与其他特征参数（例如爱丁顿的比率和黑洞质量）如何相关。在本文中，我们介绍了25个极高的Eddington样本的5 GHz非常大的阵列（VLA）观察结果，从窄线Seyfert 1 Galaxies中获得了超级质量黑洞（EESBH，EESBH，EESBHS，接近或以上的Eddington比率），其中22个来源被检测到22个来源。大多数EESBH都显示出从几百个parsec到一公斤级量表的紧凑型无线电结构。我们估计了产生观察到的无线电发射所需的恒星形成速率表面密度最低，并发现它高于周期核星脉星系中先前检测到的最大值，这意味着无线电发射来自AGN活性。除了一个比较样本外，我们还发现了从子埃德丁顿比率范围从埃德丁顿比率到超级无线电比率相关性的总体反向无线电比率相关性。 The high-Eddington and mildly super-Eddington AGNs (-0.5<log lambda_Edd<0.6) have a radio to X-ray luminosity ratio L_R/L_X~10^-5 to 10^-4 and a steep radio spectrum, supporting that the radio emission is from transient ejecta (outflows) of corona, however, the jet contribution cannot be fully ruled out.我们高度超级 - 埃德丁顿的来源（log lambda_edd> 〜0.6）具有平坦的无线电光谱，其无线电发光度：l_r/l_x〜10^-5，它们的无线电发射可能由磁化的电晕主导，并且在本文中也提出了辐射压力。
Radio emission from the high- and super-Eddington accreting active galactic nuclei (AGNs) has various origins: a persistent jet, the magnetized corona and the wind-like outflows. It is now still unclear which is the leading mechanism responsible for the observed radio emission and how the radio emission is related to other characteristic parameters such as the Eddington ratio and black hole mass. In this paper, we present the 5 GHz Very Large Array (VLA) observational results of a sample of 25 extremely high Eddington accreting supermassive black holes (EESBHs, the Eddington ratio close to or above one) from narrow-line Seyfert 1 galaxies, among which 22 sources are detected. Most of EESBHs show a compact radio structure from a few hundred parsecs to one-kiloparsec scale. We estimated the lowest star formation rate surface density required for producing the observed radio emission, and found it is higher than the largest value previously detected in circumnuclear starburst galaxies, implying that the radio emission is from the AGN activity. Along with a comparison sample, we find an overall inverse radio loudness and Eddington ratio correlation ranging from sub- to super-Eddington ratios. The high-Eddington and mildly super-Eddington AGNs (-0.5<log lambda_Edd<0.6) have a radio to X-ray luminosity ratio L_R/L_X~10^-5 to 10^-4 and a steep radio spectrum, supporting that the radio emission is from transient ejecta (outflows) of corona, however, the jet contribution cannot be fully ruled out. Our highly super-Eddington sources (log lambda_Edd>~0.6) have a flatter radio spectrum, along with its low radio luminosity: L_R/L_X~10^-5, their radio emission is likely dominated by a magnetized corona, and a radiation pressure caused jet is also proposed in this paper.
