The pc-scale radio structure of MIR-observed radio galaxies
The pc-scale radio structure of MIR-observed radio galaxies
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MIR 观测到的射电星系的 PC 级射电结构
DOI：
10.1088/1674-4527/18/9/108
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发表时间：
2018-04
期刊：
影响因子：
--
通讯作者：
Yongjun Chen
中科院分区：
文献类型：
--
作者：
Ye Yuan;Minfeng Gu;Yongjun Chen
利用甚长基线阵（VLBA）和中红外（MIR）观测资料，选取了45个3CRR射电星系样本，其中178 MHz流量密度> 16.4Jy，5GHz甚大阵（VLA）核心流量密度≥ 7 mJy，研究了吸积过程与喷流性质之间的关系。利用我们在2016年2月获得的21个源的VLBA观测数据、16个天体的档案数据分析和8个射电星系的直接测量数据，给出了5 GHz的pc尺度射电结构。吸积模式的约束下，爱丁顿比的分割值为0.01，这是估计基于红外辐射光度和黑洞质量。虽然大多数Fanaroff-Riley II型射电星系（FRIIs）的爱丁顿比比Fanaroff-Riley I型射电星系（FRIs）高，但我们发现，在低吸积率时有8个FRIIs，而在高吸积率时有2个FRIs，它们的FR形态与吸积模式之间并不存在单一的对应关系。VLBA核心在5GHz的光度和爱丁顿比之间存在显著的相关性。在我们的样品中鉴定了各种形态，包括仅核心、单侧核心喷射和双侧核心喷射结构。我们发现，较高的吸积率可能更可能与核心喷流结构有关，从而产生更长的喷流。这些结果意味着更高的吸积率可能能够产生更强大的喷流。MIR的15 μ m光度与VLBA的5GHz核心光度之间有很强的相关性，这有利于吸积盘与喷流之间的紧密联系。在我们的样品中，核心亮度温度范围从109至10 13.38 K的中值为10 11.09 K，表明系统的聚束效应可能并不显着。例外的情况下，FRI在高吸积率和FRI在低吸积率，是专门在高端和低端，分别为VLBA核心的通量比178 MHz通量密度的分布。并非不可能的是，这些来源的位置是由于最近的光辉或削弱其中央引擎（即，吸积和喷流）。
We investigated the relationship between the accretion process and jet properties by utilizing very long baseline array (VLBA) and mid-infrared (MIR) data for a sample of 45 3CRR radio galaxies selected with a flux density at 178 MHz > 16.4 Jy , 5 GHz very large array (VLA) core flux density ≥ 7 mJy and MIR observations. The pc-scale radio structure at 5 GHz is presented by using our VLBA observations for 21 sources acquired in February, 2016, the analysis of archival data for 16 objects and directly obtaining measurements for eight radio galaxies available from literatures. The accretion mode is constrained from the Eddington ratio with a dividing value of 0.01, which is estimated from the MIR-based bolometric luminosity and the black hole masses. While most Fanaroff-Riley type II radio galaxies (FRIIs) have higher Eddington ratio than Fanaroff-Riley type I radio galaxies (FRIs), we found that there is indeed no single correspondence between the FR morphology and accretion mode with eight FRIIs at low accretion rate and two FRIs at high accretion rate. There is a significant correlation between the VLBA core luminosity at 5 GHz and the Eddington ratio. Various morphologies are identified in our sample, including core only, single-sided core-jet and two-sided core-jet structures. We found that the higher accretion rate may be more likely related with the core-jet structure, thus generating a more extended jet. These results imply that the higher accretion rates are likely able to produce more powerful jets. There is a strong correlation between the MIR luminosity at 15 μ m and VLBA 5 GHz core luminosity, in favor of the tight relation between the accretion disk and jets. In our sample, the core brightness temperature ranges from 109 to 10 13.38 K with a median value of 10 11.09 K , indicating that systematically the beaming effect may not be significant. The exceptional cases, FRIs at high accretion rates and FRIIs at low accretion rates, are exclusively at the high and low ends, respectively, of the distribution of the flux ratio for VLBA core to 178 MHz flux density. It is not impossible that the locations of these sources are due to the recent shining or weakening of their central engines (i.e., both accretion and jet).
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DOI：
10.1086/161816
发表时间：
1984-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
R. Antonucci
通讯作者：
R. Antonucci
DOI：
10.1086/427867
发表时间：
2004-12
期刊：
The Astrophysical Journal
影响因子：
--
作者：
P. Temi;W. Mathews;F. Brighenti
通讯作者：
P. Temi;W. Mathews;F. Brighenti
DOI：
10.1111/j.1365-2966.2004.07793.x
发表时间：
2004-03
影响因子：
4.8
作者：
R. McLure;C. Willott;M. Jarvis;S. Rawlings;G. Hill;E. Mitchell;J. Dunlop;M. Wold
通讯作者：
R. McLure;C. Willott;M. Jarvis;S. Rawlings;G. Hill;E. Mitchell;J. Dunlop;M. Wold
DOI：
10.1111/j.1365-2966.2009.15127.x
发表时间：
2009-05
影响因子：
4.8
作者：
Qingwen Wu
通讯作者：
Qingwen Wu
影响因子：
4.8
作者：
B. Mingo;B. Mingo;M. Hardcastle;J. Croston;D. Dicken;D. Evans;R. Morganti;C. Tadhunter
通讯作者：
B. Mingo;B. Mingo;M. Hardcastle;J. Croston;D. Dicken;D. Evans;R. Morganti;C. Tadhunter