类星体主序上从太阳系以下到太阳系以上的化学丰度

Physics Pub Date : 2024-01-04 DOI:10.3390/physics6010016
Paola Marziani, Alberto Floris, A. Deconto‐Machado, S. Panda, M. Śniegowska, Karla Garnica, D. Dultzin, Mauro D’Onofrio, A. del Olmo, E. Bon, N. Bon
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引用次数: 0

摘要

事实证明,4D(四维)特征向量 1(E1)序列是组织 1 型活动星系核(AGN)观测和物理特性的一个非常有效的工具。在本文中,我们介绍了根据新数据和以前发表的数据对宽线区气体的金属性进行的多次测量。我们展示了沿 E1(也称类星体主序)光学平面的一致趋势,该趋势由巴尔默氢 Hβ 曲线的线宽和一个测量单电离铁发射突出的参数所定义。其趋势是从亚太阳金属性(与极端B种群相对应)(弱Feii发射、大Hβ FWHM(半最大全宽))到金属性(与极端A种群相对应)的几十倍太阳值(最强Feii光学发射、较窄Hβ剖面)。这些数据确定了金属性与 4DE1/main sequence 的相关性。如果相当高金属度(Z≳10Z⊙,太阳金属度)的气体是从中心黑洞的影响范围内排出的,就像在高爱丁顿比辐射源的情况下核外流和盘风的广泛证据所表明的那样,那么类星体的外流就有可能在宿主星系的化学富集过程中发挥了作用。
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From Sub-Solar to Super-Solar Chemical Abundances along the Quasar Main Sequence
The 4D (four-dimensional) eigenvector 1 (E1) sequence has proven to be a highly effective tool for organizing observational and physical properties of type-1 active galactic nuclei (AGNs). In this paper, we present multiple measurements of metallicity for the broad line region gas, from new and previously-published data. We demonstrate a consistent trend along the optical plane of the E1 (also known as the quasar main sequence), defined by the line width of Balmer hydrogen Hβ profile and by a parameter measuring the prominence of singly-ionized iron emission. The trend involves an increase from sub-solar metallicity in correspondence with extreme Population B (weak Feii emission, large Hβ FWHM (full width at half maximum)) to metallicity several tens the solar value in correspondence with extreme Population A (strongest Feii optical emission, narrower Hβ profiles). The data establish the metallicity as a correlate of the 4DE1/main sequence. If the considerably high metallicity (Z≳10Z⊙, solar metallicity) gas is expelled from the sphere of influence of the central black hole, as indicated by the widespread evidence of nuclear outflows and disk wind in the case of sources radiating at a high Eddington ratio, then it is possible that the outflows from quasars played a role in chemically enriching the host galaxy.
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