从光学到远紫外活动星系核连续统的变红和可变分量的形状。I
Reddening and the Shape of the Variable Component of the Continua of Active Galactic Nuclei From the Optical to the Far Ultraviolet. I
摘要：
我们分析了斯隆数字巡天条纹82的4，611个活动星系核（AGN）的光度变化。我们恢复的光谱能量分布（SED）的可变流量作为波长的函数。对于比$\sim \lambda2200$长的静止波长，我们发现最蓝活动星系核的可变分量的SED与预测的外部照明吸积盘的$F_ν \propto ν^{+1/3}$光谱是一致的。我们确认有一些残余的可变发射对应的“蓝色小凸起”和其他宽线区域的变化。我们解释陡峭的光谱的可变组件是由于内在的红化。这是支持的相关性的巴耳末减量与颜色过剩的可变组件。用$z < 0.4$方法计算了第82带SDSS活动星系核的内部红化中值为$E(B-V) \thickapprox 0.10$，这与Balmer减量法计算的红化值一致。样本中的单个活动星系核可以具有$E(B-V) > 0.4$
英文摘要：
We analyze the photometric variability of 4,611 active galactic nuclei (AGNs) from the Sloan Digital Sky Survey Stripe 82. We recover the spectral energy distribution (SED) of the variable flux as a function of wavelength. For rest wavelengths longer than $\sim \lambda2200$ we find that the SED of the variable component of the bluest AGNs is consistent with the $F_ν \propto ν^{+1/3}$ spectrum predicted for an externally-illuminated accretion disc. We confirm there is some residual variable emission corresponding to the "small blue bump" and other broad-line region variability. We interpret steeper optical spectra of the variable component as being due to intrinsic reddening. This is supported by the correlation of the Balmer decrement with the colour excess of the variable component. We find the median internal reddening of SDSS AGNs in Stripe 82 with $z < 0.4$ to be $E(B-V) \thickapprox 0.10$ in agreement with the reddening derived from the Balmer decrement. Individual AGNs in the sample can have $E(B-V) > 0.4$
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