Cosmic gamma-ray background from type ia supernovae reexamined : Evidence for missing gamma rays at MeV energy
Cosmic gamma-ray background from type ia supernovae reexamined : Evidence for missing gamma rays at MeV energy
复制标题
重新审视 ia 型超新星的宇宙伽马射线背景：MeV 能量伽马射线缺失的证据
DOI：
10.1103/physrevd.71.121301
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发表时间：
2005
影响因子：
5
通讯作者：
P. Hoflich
中科院分区：
文献类型：
--
作者：
K. Ahn;E. Komatsu;P. Hoflich
观测到的 {约}MeV 宇宙 {γ} 射线背景通常归因于 Ia 型超新星 (SNIa)。由于 SNIa 接近标准蜡烛，一旦知道 SNIa 速率的演变，就可以相当准确地计算出 SNIa 在红移上积分的 {gamma} 射线强度。在 z < 或大约处测量的最新 SNIa 速率。 1.6 [达伦等人，天体物理学。 J. 613, 189 (2004)]表明先前对{gamma}射线背景的计算始终高估了SNIa速率。根据新的比率，我们发现 SNIa 的贡献比观察到的要小一个数量级，因此应该调用新的源群体。
The observed cosmic {gamma}-ray background at {approx}MeV has often been attributed to Type Ia supernovae (SNIa). Since SNIa is close to a standard candle, one can calculate the {gamma}-ray intensity of SNIa integrated over redshifts fairly accurately, once the evolution of the SNIa rate is known. The latest SNIa rate measured at z < or approx. 1.6 [Dahlen et al., Astrophys. J. 613, 189 (2004)] indicates that the previous calculations of the {gamma}-ray background consistently overestimated the SNIa rate. With the new rate, we find that the SNIa contribution is an order of magnitude smaller than observed, and thus new population(s) of sources should be invoked.