论文标题
伽马射线和光谱电台的光学特性3C 279 Flare 2015年6月
Gamma-ray and Optical properties of the flat spectrum radio quasar 3C 279 flare in June 2015
论文作者
论文摘要
2015年6月16日，在极高的活动状态下观察到扁平频谱无线电排3c 279（MJD 57189）。在本文中，我们使用\ emph {fermi} -lat，smarts和spol观测的数据在2015年6月1日至30日（MJD 57174-57203）期间，使用来自\ emph {fermi} -lat，Smarts和Spol观测的数据研究了此耀斑插曲的特性。 \ emph {fermi} -lat检测到的$γ$ - 雷频带中的最高排放状态表现出$ \ sim $ 2 $ 2 $ \ times $ 10 $ 10 $^{ - 7} $ erg〜cm $^cm $^{ - 2} $ 〜s $ 〜s $^s $^s $^{ - 1} $超过25倍的通量级别的级别，该级别的级别是低于低的活动。对每日\ emph {fermi} -lat光曲线的时间分析表明，巨大的耀斑发作具有特征性的上升和衰减时间少于一天。 B，V，R和J频段中的光学每日光曲线也表明了2015年6月16日至17日的3C 279的耀斑活性，升高两天（MJD 57189-57190）。离散的相关函数分析表明在耀斑发作期间$γ$ ray和光峰之间的时间滞后为1天或更长。还观察到$γ$ - 射线的发射表现出更艰难的行为，而光学发射则表现出相反的行为。耀斑期间的$γ$ - 射线发射区非常紧凑，位于射流底部附近。在此期间，使用SPOL测量的波长范围500-700 nm的线性极化程度也很大可变，$ \ sim $ 30 $ \％\％$ \％$ \％$ \％$ \％$ \％$ $ \％$ $ \％$ $ \％$。几乎同时发生$γ$ ray通量点显示了在$γ$ -Ray耀斑期间的极化程度的线性反相关。线性极化程度的显着下降表明发射区域纠结的磁场强度突然增加。
The flat spectrum radio quasar 3C 279 was observed in an extremely high activity state on June 16, 2015 (MJD 57189). In this paper, we investigate the properties of this flaring episode in the high energy $γ$-ray and optical bands using data from the \emph{Fermi}-LAT, SMARTS, and SPOL observations during the period June 1-30, 2015 (MJD 57174-57203). The highest emission state in the $γ$-ray band detected by the \emph{Fermi}-LAT exhibits a peak flux of $\sim$ 2$\times$10$^{-7}$ erg~cm$^{-2}$~s$^{-1}$ which is more than 25 times the flux level measured in the low activity state of the source. The temporal analysis of the daily \emph{Fermi}-LAT light curve suggests that the giant flaring episode has characteristic rise and decay times less than one day. The optical daily light curves in B, V, R, and J bands also indicate the flaring activity from 3C 279 with flux levels peaking for two days on June 16-17, 2015 (MJD 57189-57190). The discrete correlation function analysis indicates a time lag of 1 day or longer between the $γ$-ray and optical peaks during the flaring episode. The $γ$-ray emission is also observed to show a harder-when-brighter behaviour whereas optical emission exhibits an opposite behaviour. The $γ$-ray emission region during the flare is observed to be very compact and is located close to the base of the jet. The degree of linear polarization in the wavelength range 500-700 nm measured using SPOL during this period is also highly variable with a peak of $\sim$ 30$\%$ one day after the $γ$-ray flare. Near simultaneous $γ$-ray flux points show a linear anti-correlation with the degree of polarization during the period of $γ$-ray flare. The significant drop in the degree of linear polarization suggests a sudden increase in the tangled magnetic field strength in the emission region.
