Delayed triggering of radio Active Galactic Nuclei in gas-rich minor mergers in the local Universe
Delayed triggering of radio Active Galactic Nuclei in gas-rich minor mergers in the local Universe
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本地宇宙中富含气体的小型合并中延迟触发射电活动星系核
DOI：
10.1093/mnras/stw2536
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发表时间：
2016
影响因子：
4.8
通讯作者：
T. Davis
中科院分区：
文献类型：
--
作者：
S. Shabala;A. Deller;S. Kaviraj;E. Middelberg;R. Turner;Y. Ting;J. Allison;T. Davis
我们在mJIVE-20探测所需的25个低红移（z 107 K）亮度温度的样品中检查触发恒星形成和活动星系核（AGN）活动的过程，使我们能够明确地识别样品中的射电AGN。我们找到了三个这样的对象。我们的VLBI AGN识别在窄线光学诊断图中被划分为塞弗特区或低电离核发射线区（liner）；我们的目标的中红外颜色和Hα星形成速率与综合射电光度的比较也与VLBI的识别一致。我们利用光学和紫外光度法重建了银河系的恒星形成历史，发现这些射电AGN在合并过程中没有被及时触发，这与之前对非vlbi射电AGN样本的发现一致。这种延迟会极大地限制星系合并触发的射电AGN反馈的效率。我们发现，在相同的星暴年龄下，射电AGN宿主的恒星形成率低于非AGN射电选择星系。常规和VLBI射电成像显示这些AGN在弧秒尺度上是紧凑的。我们的模型表明，agn膨胀的射电叶的实际大小可能比这个大得多，但它们太微弱了，无法在现有的观测中检测到。深射电成像需要绘制出AGN的真实范围，并确定射电AGN主机中的低恒星形成率是射电喷流触发所需的特殊条件的结果，还是AGN反馈的影响。
We examine the processes triggering star formation and active galactic nucleus (AGN) activity in a sample of 25 low-redshift (z 107 K) brightness temperature required for an mJIVE-20 detection allows us to unambiguously identify the radio AGN in our sample. We find three such objects. Our VLBI AGN identifications are classified as Seyferts or low-ionization nuclear emission-line regions (LINERs) in narrow line optical diagnostic plots; mid-infrared colours of our targets and the comparison of Hα star formation rates with integrated radio luminosity are also consistent with the VLBI identifications. We reconstruct star formation histories in our galaxies using optical and UV photometry, and find that these radio AGN are not triggered promptly in the merger process, consistent with previous findings for non-VLBI samples of radio AGN. This delay can significantly limit the efficiency of feedback by radio AGN triggered in galaxy mergers. We find that radio AGN hosts have lower star formation rates than non-AGN radio-selected galaxies at the same starburst age. Conventional and VLBI radio imaging shows these AGN to be compact on arcsecond scales. Our modelling suggests that the actual sizes of AGN-inflated radio lobes may be much larger than this, but these are too faint to be detected in existing observations. Deep radio imaging is required to map out the true extent of the AGN, and to determine whether the low star formation rates in radio AGN hosts are a result of the special conditions required for radio jet triggering, or the effect of AGN feedback.
影响因子：
4.8
作者：
T. Davis;K. Rowlands;J. Allison;S. Shabala;Y. Ting;C. Lagos;S. Kaviraj;N. Bourne;L. Dunne
通讯作者：
T. Davis;K. Rowlands;J. Allison;S. Shabala;Y. Ting;C. Lagos;S. Kaviraj;N. Bourne;L. Dunne
DOI：
10.1088/0004-637x/782/2/90
发表时间：
2014-01
期刊：
The Astrophysical Journal
影响因子：
--
作者：
M. Cluver;M. Cluver;T. Jarrett;A. Hopkins;S. Driver;S. Driver;J. Liske;M. Gunawardhana;M. Gunawardhana;M. Gunawardhana;E. Taylor;A. Robotham;M. Alpaslan;I. Baldry;Michael J. I. Brown;J. Peacock;C. Popescu;R. Tuffs;A. Bauer;J. Bland-Hawthorn;M. Colless;B. Holwerda;M. Lara-López;K. Leschinski;Á. López-Sánchez;Á. López-Sánchez;P. Norberg;M. Owers;Lingyu Wang;S. Wilkins
通讯作者：
M. Cluver;M. Cluver;T. Jarrett;A. Hopkins;S. Driver;S. Driver;J. Liske;M. Gunawardhana;M. Gunawardhana;M. Gunawardhana;E. Taylor;A. Robotham;M. Alpaslan;I. Baldry;Michael J. I. Brown;J. Peacock;C. Popescu;R. Tuffs;A. Bauer;J. Bland-Hawthorn;M. Colless;B. Holwerda;M. Lara-López;K. Leschinski;Á. López-Sánchez;Á. López-Sánchez;P. Norberg;M. Owers;Lingyu Wang;S. Wilkins
影响因子：
6.5
作者：
van Haarlem, M. P.;Wise, M. W.;van Zwieten, J.
通讯作者：
van Zwieten, J.