我们目前的一个非常广泛的线塞弗特1星系Mrk 926密集的光谱变化运动的结果。我们的目标是调查宽线区（BLR）通过研究该星系的强度和线轮廓的变化在短时间尺度上。高信噪比（S/N）光谱是在2004年和2005年的两次观测活动中，在相同的条件下用9.2米的霍比-埃伯利望远镜（HET）拍摄的。在光谱缩减和内部校准之后，我们实现了优于1%的相对通量精度。非常宽的巴耳末线的均方根剖面的形状与其平均线剖面不同，除了中心分量（v $\lesssim \pm{}$ 600 km s $^{-1}$）外，还包括两个内部（v $\lesssim \pm{}$ 6000 km s $^{-1}$）和两个外部（v $\gtrsim \pm{}$ 6000 km s $^{-1}$）线分量。这些内外线段在我们的战役中以不同的幅度变化。BLR的半径非常小，H $β$ BLR的半径上限为2光日。我们导出了$ M= 11.2 \times 10^{7} M_{\odot} $中心黑洞质量的上限。H $β$和H $α$的二维互相关联函数CCF（$τ$，$v$）在误差范围内是平坦的.在H $α$和H $β$的外翼和内翼中，巴耳末线段对连续变化的响应是不同的。响应曲线中的这种双重结构-两个独立的内部和外部分量-也可以在均方根线轮廓中看到。我们的结论是，外部和内部线段起源于不同的区域和/或在不同的物理条件下。
英文摘要：
We present results of an intensive spectroscopic variability campaign of the very broad-line Seyfert 1 galaxy Mrk 926. Our aim is to investigate the broad-line region (BLR) by studying the intensity and line profile variations of this galaxy on short timescales. High signal-to-noise ratio(S/N) spectra were taken with the 9.2m Hobby-Eberly Telescope (HET) in identical conditions during two observing campaigns in 2004 and 2005. After the spectral reduction and internal calibration we achieved a relative flux accuracy of better than 1%. The rms profiles of the very broad Balmer lines have shapes that differ from their mean line profiles, consisting of two inner (v $\lesssim \pm{}$ 6000 km s$^{-1}$) and two outer (v $\gtrsim \pm{}$ 6000 km s$^{-1}$) line components in addition to a central component (v $\lesssim \pm{}$ 600 km s$^{-1}$). These outer and inner line segments varied with different amplitudes during our campaign. The radius of the BLR is very small with an upper limit of 2 light-days for the H$β$ BLR size. We derived an upper limit to the central black hole mass of $ M= 11.2 \times 10^{7} M_{\odot} $. The 2-D cross-correlation functions CCF($τ$,$v$) of H$β$ and H$α$ are flat within the error limits. The response of the Balmer line segments with respect to continuum variations is different in the outer and inner wings of H$α$ and H$β$. This double structure in the response curves - of two separate inner and outer components - has also been seen in the rms line profiles. We conclude that the outer and inner line segments originate in different regions and/or under different physical conditions.
Optical multiband surface photometry of a sample of Seyfert galaxies. I. Large-scale morphology and local environment analysis of matched Seyfert and inactive galaxy samples
