arXiv 1408.69552014-08-29astro-ph.GA

双峰发射线AGN Arp 102 B：II的光谱光学监测。宽线特性的变异性

Spectral optical monitoring of the double peaked emission line AGN Arp 102B: II. Variability of the broad line properties

L. C. Popovic, A. I. Shapovalova, D. Ilic, A. N. Burenkov, V. H. Chavushyan, W. Kollatschny, A. Kovacevic, J. R. Valdes, J. Leon-Tavares, N. G. Bochkarev, V. Pa… 展开作者

L. C. Popovic, A. I. Shapovalova, D. Ilic, A. N. Burenkov, V. H. Chavushyan, W. Kollatschny, A. Kovacevic, J. R. Valdes, J. Leon-Tavares, N. G. Bochkarev, V. Patino-Alvarez, J. Torrealba

备注：: 17 pages, Accepted for publication in A&A
发表信息：: A&A 572, A66 (2014)
DOI：: 10.1051/0004-6361/201423555

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摘要：

我们调查了射电星系Arp 102 B的宽谱线特性的长期（26年，从1987年到2013年）变化，Arp 102 B是一个具有宽双峰发射线的活跃星系。我们使用论文I（Shapovalova et al. 2013）中提供的1987 - 2011年期间的观测结果，以及2012- 2013年进行的一组新观测结果。为了探索BLR的几何形状，并澄清一些矛盾的性质的BLR在Arp 102 B，我们探讨的H $α$和H $β$线参数在监测期间的变化。我们用三个宽高斯函数拟合宽线，找到H $α$和H $β$中蓝色和红色峰的位置和强度。此外，我们拟合平均线轮廓与光盘模型。我们发现，宽线轮廓是双峰，并没有改变显着的形状，旁边的一个额外的小峰，不时可以看到在H $α$线的蓝色部分。蓝色和红色峰值的位置在监测期间没有显著变化。在监测期间，H $β$线比H $α$线宽。圆盘模型能够再现H $β$和H $α$宽谱线轮廓，然而，观察到的谱线参数的变化与发射圆盘假设不一致。Arp 102 B的BLR似乎具有盘状几何形状，但流出的作用也可以在观察到的宽线性质的变化中发挥重要作用。

英文摘要：

We investigate a long-term (26 years, from 1987 to 2013) variability in the broad spectral line properties of the radio galaxy Arp 102B, an active galaxy with broad double-peaked emission lines. We use observations presented in Paper I (Shapovalova et al. 2013) in the period from 1987 to 2011, and a new set of observations performed in 2012--2013. To explore the BLR geometry, and clarify some contradictions about the nature of the BLR in Arp 102B we explore variations in the H$α$ and H$β$ line parameters during the monitored period. We fit the broad lines with three broad Gaussian functions finding the positions and intensities of the blue and red peaks in H$α$ and H$β$. Additionally we fit averaged line profiles with the disc model. We find that the broad line profiles are double-peaked and have not been changed significantly in shapes, beside an additional small peak that, from time to time can be seen in the blue part of the H$α$ line. The positions of the blue and red peaks { have not changed significantly during the monitored period. The H$β$ line is broader than H$α$ line in the monitored period. The disc model is able to reproduce the H$β$ and H$α$ broad line profiles, however, observed variability in the line parameters are not in a good agreement with the emission disc hypothesis. It seems that the BLR of Arp 102B has a disc-like geometry, but the role of an outflow can also play an important role in observed variation of the broad line properties.

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