论文标题
伽玛射线发射Blazars的中红外变异性
Mid-infrared Variability of gamma-ray emitting blazars
论文作者
论文摘要
使用来自宽场红外调查探险家的数据，我们研究了中红外3.4 $ $ $ m（W1频段）和4.6 $ $ m $ m（W2频段）的通量变异性$γ$ -RARE-ray-ray-ray-ray-rayting blazars。我们的样本由460个平光无线电类星体（FSRQ）和575个Bl lacertae（Bl Lac）对象组成。在日内时间表上，FSRQS的可变性中值（$σ_{M} $）为0.04 $^{+0.03} _ { - 0.02} $ mag和0.05 $^{+0.05 $^{+0.03} _ { - 0.02} _ { - 0.02} $ mag in W1 and W1和W2乐队。对于BL LACS，我们在W1（W2）频段中找到了中值$σ_{M} $ 0.04 $^{+0.01} _ { - 0.02} $（0.04 $^{+0.02} _ { - 0.02} _ { - 0.02} $）$。在长时间大小上，对于FSRQS，我们发现了一个中值$σ_{m} $ 0.44 $^{+0.28} _ { - 0.27} $ mag和0.45 $^{+0.27} _ { - 0.27} _ { - 0.27} 0.21 $^{+0.18} _ { - 0.12} $ mag和0.22 $^{+0.18} _ { - 0.11} $ mag在W1和W2频段中。从统计测试中，我们发现FSRQ在日内和长时间尺度上显示出比BL LACS更大的$σ_m$。在Blazars中，与中间同步器（ISP）（ISP）和高同步子（HSP）峰值（HSP）源相比，低同步器达到峰值（LSP）源显示出更大的$σ_m$。带与电子能量分布的峰值一致。 BL LACS具有低功率喷射，观察窗也可以追溯到低能电子的发射，从而导致低$σ_{M} $。在观察到更明亮的行为时，在FSRQ和BL LAC中，主要是蓝色。在$σ_m$和黑洞质量之间未发现相关性。
Using data from the Wide-field Infrared Survey Explorer we studied the mid infrared 3.4 $μ$m (W1-band) and 4.6 $μ$m (W2-band) flux variability of $γ$-ray emitting blazars. Our sample consists of 460 flat spectrum radio quasars (FSRQs) and 575 BL Lacertae (BL Lac) objects. On intra-day timescales, the median amplitude of variability ($σ_{m}$) for FSRQs is 0.04$^{+0.03}_{-0.02}$ mag and 0.05$^{+0.03}_{-0.02}$ mag in W1 and W2 bands. For BL Lacs we found median $σ_{m}$ in W1(W2) bands of 0.04$^{+0.01}_{-0.02}$ (0.04$^{+0.02}_{-0.02}$) mag. On long timescales, for FSRQs we found a median $σ_{m}$ of 0.44$^{+0.28}_{-0.27}$ mag and 0.45$^{+0.27}_{-0.27}$ mag in W1 and W2 bands, while for BL Lacs the median values are 0.21$^{+0.18}_{-0.12}$ mag and 0.22$^{+0.18}_{-0.11}$ mag in W1 and W2 bands. From statistical tests, we found FSRQs to show larger $σ_m$ than BL Lacs on both intra-day and long timescales. Among blazars, low synchrotron peaked (LSP) sources showed larger $σ_m$ compared to intermediate synchrotron peaked (ISP) and high synchrotron peaked (HSP) sources.The larger $σ_{m}$ seen in FSRQs relative to BL Lacs on both intra-day and long timescales could be due to them having the most powerful relativistic jets and/or their mid infrared band coinciding with the peak of the electron energy distribution. BL Lacs have low power jets and the observational window too traces the emission from low energy electrons, thereby leading to low $σ_{m}$. In both FSRQs and BL Lacs predominantly a bluer when brighter behaviour was observed. No correlation is found between $σ_m$ and black hole mass.
