Gamma-ray luminosity function of BL Lac objects and contribution to the extragalactic gamma-ray background

Gamma-ray luminosity function of BL Lac objects and contribution to the extragalactic gamma-ray background
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BL Lac天体的伽马射线光度函数及其对河外伽马射线背景的贡献

DOI：
10.1093/mnras/stz2651
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发表时间：
2019-09
期刊：
Monthly Notices of the Royal Astronomical Society
影响因子：
4.8
通讯作者：
Yan Dahai
Yan Dahai
中科院分区：
物理与天体物理2区
文献类型：
--
作者：
Qu Yankun;Zeng Houdun;Yan Dahai

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利用一个显著放大的费米-LAT BL Lac天体（BL拉克）样本，结合空间密度分布和源计数分布，构造了BL拉克的γ射线光度函数（GLF）。我们使用了三种研究得很好的GLF形式，即纯密度演化（PDE），纯光度演化（PLE）和光度依赖的密度演化（LDDE）的形式。马尔可夫链蒙特卡罗（MCMC）技术被用来约束模型参数。我们的结果表明LDDE模型可以给出BL Lac GLF的最佳描述。该模型还表明，具有较硬GeV谱和较低光度的BL拉克类星体的演化与平谱射电类星体一样强烈，且演化随光度的增加而减弱。我们还用双幂律模型模拟了BL拉克的平均光子谱。使用此模型化的光谱，BL拉克贡献$\sim \！在E > 100 MeV时，总河外伽马射线背景（EGB）的20{{\rm %}}$，$\sim \！100{{\rm %}}$的EGB在E > 50 GeV，和未解决的BL拉克贡献$\sim\！在E > 100 MeV时，各向同性漫射伽马射线背景的20%。给出了TeV EGB谱的预测，可供将来的探测器检验。
Using a significantly enlarged Fermi-LAT BL Lac objects (BL Lacs) sample, we construct the gamma-ray luminosity function (GLF) of BL Lacs, by the joint use of the space density distribution and source counts distribution. We use three well-studied forms of the GLF, i.e. the forms of pure density evolution (PDE), pure luminosity evolution (PLE), and luminosity-dependent density evolution (LDDE). The Markov Chain Monte Carlo (MCMC) technique is used to constrain model parameters. Our results suggest that LDDE model can give the best description for the BL Lac GLF. And the model shows that the BL Lacs with a harder GeV spectrum and a less luminosity evolve as strongly as flat spectrum radio quasars, and the evolution decreases as increasing luminosity. We also model the average photon spectra of BL Lacs with a double power-laws model. Using this modelled spectra, BL Lacs contribute $\sim \!20{{\ \rm per\ cent}}$ of the total extragalactic gamma-ray background (EGB) at E > 100 MeV, $\sim \!100{{\ \rm per\ cent}}$ of the EGB at E > 50 GeV, and the unresolved BL Lacs contribute $\sim\! 20 {{\ \rm per\ cent}}$ of the isotropic diffuse gamma-ray background at E > 100 MeV. A prediction of the TeV EGB spectra are given, which may be tested by the future detectors.
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影响因子： 6.4
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