论文标题
NGC 4395中中间质量AGN的可变性和尺寸亮度关系
Variability and the size-luminosity relation of the intermediate mass AGN in NGC 4395
论文作者
论文摘要
我们根据2017年和2018年的光度监测活动介绍了最低的亮度Seyfert 1 Galaxy NGC 4395的可变性研究。使用22个地面和太空望远镜，我们在10天内使用了$ \ sim $ 5分钟的ngc 4395，并在10天内获得了$ 5分钟的频率，并在10天内获得了uv，js和ks/js/ks的ks，ks，ks，j，ks，ks，j，ks，j，ks，ks，ks，ks，ks，ks，ks，ks，j，j，k，k，k， h $α$窄带。 RMS的可变性为$ \ sim $ 0.13 mag \ emph {swift} -uvm2和v滤光灯曲线，在k滤波器上降低至$ \ sim $ 0.01 mag。在纠正了对H $α$窄带的连续贡献后，我们测量了H $α$发射线的时间滞后，相对于V频段连续量为$ {55}^{+27} _ { - 31} $ {-31} $ to $ {+$ {122}^{+33}^{+33}^{+33} _ { - 67} $ { - 67} $。在2017年和$ {49}^{+15} _ { - 14} $ to $ {83}^{+13} _ { - 14} $ min。在2018年，取决于H $α$窄带中连续变异幅度的假设。由于紫外线观测的不确定性和有限的时间基线，我们无法获得对紫外线和V频段之间以及近IR带之间连续的延迟滞后滞后的可靠测量。我们确定了5100Å$λl_λ= \左（5.75 \ pm0.40 \ right）\ times 10^{39} \，\ Mathrm {erg {erg \，s^{ - 1}} $的AGN单色光度。尽管NGC 4395的光亮度比其他型映射AGN低两个数量级，但NGC 4395遵循尺寸左右的关系，尽管从以前的最佳fit fit fit-Fit Relation vell bentz et a bentz et a a bentz et a a ngc luminity关系（尽管占0.48 dex（$ \ geq $ 2.5 $σ$））。 （2013）。
We present the variability study of the lowest-luminosity Seyfert 1 galaxy NGC 4395 based on the photometric monitoring campaigns in 2017 and 2018. Using 22 ground-based and space telescopes, we monitored NGC 4395 with a $\sim$5 minute cadence during a period of 10 days and obtained light curves in the UV, V, J, H, and K/Ks bands as well as the H$α$ narrow-band. The RMS variability is $\sim$0.13 mag on \emph{Swift}-UVM2 and V filter light curves, decreasing down to $\sim$0.01 mag on K filter. After correcting for continuum contribution to the H$α$ narrow-band, we measured the time lag of the H$α$ emission line with respect to the V-band continuum as ${55}^{+27}_{-31}$ to ${122}^{+33}_{-67}$ min. in 2017 and ${49}^{+15}_{-14}$ to ${83}^{+13}_{-14}$ min. in 2018, depending on the assumption on the continuum variability amplitude in the H$α$ narrow-band. We obtained no reliable measurements for the continuum-to-continuum lag between UV and V bands and among near-IR bands, due to the large flux uncertainty of UV observations and the limited time baseline. We determined the AGN monochromatic luminosity at 5100Å $λL_λ= \left(5.75\pm0.40\right)\times 10^{39}\,\mathrm{erg\,s^{-1}}$, after subtracting the contribution of the nuclear star cluster. While the optical luminosity of NGC 4395 is two orders of magnitude lower than that of other reverberation-mapped AGNs, NGC 4395 follows the size-luminosity relation, albeit with an offset of 0.48 dex ($\geq$2.5$σ$) from the previous best-fit relation of Bentz et al. (2013).
