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Infrared emission from dust and the spectral features of extragalactic gamma-ray sources

机译:来自灰尘的红外排放和胶质伽马射线源的光谱特征

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In this work, we investigate the role of emission by dust at infrared wavelengths in the absorption of gamma radiation from distant extragalactic sources, especially blazars. We use an existing EBL model based on direct starlight emission at UV/visible and secondary radiation due to dust (PAHs (polycyclic aromatic hydrocarbons), small and large grains) at IR due to partial absorption of the stellar component. The relative contribution of each grain type to the total EBL energy density was determined from a combined fit to the Markarian 501 (z ~ 0.034) SED in flare state, where both the parameters of the intrinsic source spectrum (with or without curvature) and the dust fractions were allowed to vary. By separating the attenuation due to each EBL component, the importance of individual grain types to the opacity of the extragalactic medium for the TeV emission of a blazar like Markarian 501 could be better understood. Using a nested log-likelihood ratio test, we compared null hypotheses represented by effective 1- and 2-grain models against a 3-grain alternative scenario. When the temperatures of the grains are fixed a priori, the 1-grain scenario with only PAHs can be excluded at more than 5σ (p = 2.9 × 10 ~(-8) ), irrespective of the curvature in the intrinsic spectrum. The effective 3-grain EBL model with the tuned fractions was finally used to fit the SEDs of a sample of extragalactic gamma-ray sources (dominated by blazars). Such a sample is still dominated by starlight attenuation, therefore, no statistically significant improvement in the quality of fits was observed when the tuned fractions are used to account for the EBL attenuation and the intrinsic spectrum parameters are allowed to vary during the fit. The potential of this kind of analysis when the next generation of IACTs, represented by the Cherenkov Telescope Array (CTA), starts observations is enormous. The newly discovered AGNs at a broad range of redshifts should break many of the degeneracies cu
机译:在这项工作中,我们研究了灰尘在红外波长下吸收的发射在远处近似术来源的吸收中的作用,尤其是布拉齐。我们根据恒星组分的部分吸收,基于UV /可见和次级辐射的直接星光发射,基于UV /可见和次级辐射的直星发射,其使用现有的EBL模型。从闪光状态的组合拟合与标记物501(Z〜0.034)SED中的组合符合燃烧状态,确定每个晶粒类型对总EBL能量密度的相对贡献,其中内在源谱(有或没有曲率)和允许粉尘级分不同。通过将衰减分开由于每个EBL分量,可以更好地理解各个谷物类型对紫外线介质的紫外线介质的不透明度的重要性。使用嵌套的日志似然比测试,我们比较了通过有效的1和2粒模型表示的空假设,而不是3粒替代方案。当晶粒的温度固定为先验时,只有PAHS的1粒场景可以在超过5σ(P = 2.9×10〜(-8))中,无论内在光谱中的曲率如何。最终使用具有调谐级分的有效的3粒EBL模型来适合胶质型γ射线源的样品(由布拉恩支配)的样品。这种样品仍然是星光衰减的主导,因此,当使用调谐的级分来解释EBL衰减时,观察到拟合质量的统计学上显着改善,并且允许内在光谱参数在配合期间变化。这种分析的潜力当由Cherenkov望远镜阵列(CTA)表示的下一代IACT开始观察是巨大的。新发现的AGNS在广泛的红移时应破坏许多退化级

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