Locations of optical and gamma-ray emitting regions and variation phenomena of PMN J2345-1555
Locations of optical and gamma-ray emitting regions and variation phenomena of PMN J2345-1555
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PMN J2345-1555光学和伽马射线发射区域的位置及变化现象
DOI：
10.1093/mnras/staa475
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发表时间：
2020
影响因子：
4.8
通讯作者：
Huo Qiu-Hong
中科院分区：
文献类型：
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作者：
Jiang Yunguo;Hu Shao-Ming;Chen Xu;Shao Xi;Huo Qiu-Hong
我们收集了类星体PMN J2345 - 1555的15 GHz长时γ光、光和射电光变曲线，并对它们进行了相关分析。我们发现，不同的采样可以导致不同的时间延迟，光变曲线的周期性可以产生超过3σ显著性水平的信号。光VandR波段和红外J波段的光变曲线超前射电15 GHz光变曲线。在光学和γ射线光变曲线之间没有滞后。我们使用的时间滞后，以获得核心的大小和它的不确定性。我们发现15 GHz的核心区距离喷流底部约为秒差距。光学区和γ射线发射区重合，位于15 GHz核心区上游的秒差距处。因此，光学和γ射线发射区域最有可能在宽线区域内。对于这个目标，在1秒差距的喷流中的磁场和粒子密度分别为0.16 G和247/γmincm−3。黑洞的质量估计为108.44M <$。δV− δ R的行为很复杂，而R-J则表现出越亮越蓝的趋势。我们提出了与原子核共振相关的光谱指数模型来解释色指数行为，这是对喷流中激波模型的补充。不排除光谱折射率行为是由于圆盘的贡献和变化的多普勒因子的可能性。
We collect the long-term γ-ray, optical, and radio 15 GHz light curves of quasar object PMN J2345−1555, and make correlation analyses between them. We find that different samplings can lead to different time delays, and the periodicity of light curves can produce signals that are beyond 3σ significance level. The opticalVandRband and the infraredJband light curves lead the radio 15 GHz light curve byd. There is no lag between the optical and γ-ray light curves. We use the time lags to derive the core size and its uncertainty. We find that the core region of 15 GHz isparsec away from the jet base. The optical and γ-ray emitting regions coincide, which are located atparsec upstream of the core region of 15 GHz. Thus, the optical and γ-ray emitting regions are most probably inside the broad-line region. For this target, the magnetic field and particle density at 1 parsec in the jet are derived to be 0.16 G and 247/γmincm−3, respectively. The black hole mass is estimated to be 108.44M⊙. The behaviour of δV− δRis complex, while theR−Jshows a bluer-when-brighter trend. We proposed anr-dependent spectral index model to explain the colour index behaviours, which is complementary for the shock in jet model. The possibility that the spectral index behaviours are due to the contribution from the disc and the varying Doppler factor is not excluded.