Nuclear activity of NGC 4151 as inferred from UBVRI observations in 1989–2000
Nuclear activity of NGC 4151 as inferred from UBVRI observations in 1989–2000
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DOI：
10.1134/1.1344256
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发表时间：
2001-02
期刊：
影响因子：
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通讯作者：
V. Doroshenko;V. M. Lyuty;N. Bochkarev;V. Vlasyuk;V. Mikhailov;O. Spiridonova;K. Grankin;O. Ezhkova;S. Mel’nikov
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作者：
V. Doroshenko;V. M. Lyuty;N. Bochkarev;V. Vlasyuk;V. Mikhailov;O. Spiridonova;K. Grankin;O. Ezhkova;S. Mel’nikov
我们介绍了我们从到2000年在三个天文台对Seyfert星系NGC4151核的宽带UBVRI观测：Sternberg天文研究所的克里米亚天文台、高加索的特殊天体物理观测站和乌兹别克斯坦Ulugbek天文研究所的Maidanak天文台。所有的数据都被简化成一个单一的系统，并给出了ANA=27.“5光圈。规则RandI的观测表明，所有波段的光学变率模式都是相同的；相对变率幅度从UtoV开始下降，但Rv比Inv略大。分量的变化幅度在几个月的时间尺度上波动，与分量的UBV通量在几年的时间尺度上变化成正比。在红色区域，慢分量和快分量之间的相关性显著减弱，而来自慢分量的通量与快分量INR的幅度之间没有相关性。颜色特征对应于超过巴尔默极限的光学厚等离子体的复合辐射。
We present our broadbandUBVRIobservations of the nucleus of the Seyfert galaxy NGC 4151 from 1989 until 2000 at three astronomical observatories: the Crimean Station of the Sternberg Astronomical Institute, the Special Astrophysical Observatory in the Caucasus, and the Maidanak Observatory of the Ulugbek Astronomical Institute in Uzbekistan. All data have been reduced to a single system and are given for anA=27.″5 aperture. RegularRandIobservations show that the pattern of optical variability is the same in all bands; the relative variability amplitude decreases fromUtoV, but it is even slightly larger inRthan inV. The variability amplitude of the component fluctuating on time scales of several months is proportional to theUBVflux from the component varying on times scales of several years. The correlation between the slow and rapid components significantly weakens in the red, and no correlation has been found between the flux from the slow component and the amplitude of the rapid component inR. The color characteristics correspond to the recombination radiation from an optically thick plasma beyond the Balmer limit.