TESTING THE MILLISECOND PULSAR SCENARIO OF THE GALACTIC CENTER GAMMA-RAY EXCESS WITH VERY HIGH ENERGY GAMMA-RAYS
TESTING THE MILLISECOND PULSAR SCENARIO OF THE GALACTIC CENTER GAMMA-RAY EXCESS WITH VERY HIGH ENERGY GAMMA-RAYS
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DOI：
10.1088/0004-637x/802/2/124
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发表时间：
2014-11
期刊：
影响因子：
--
通讯作者：
Q. Yuan;K. Ioka
中科院分区：
文献类型：
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作者：
Q. Yuan;K. Ioka
最近对费米大天区望远镜数据的分析显示，在银河系中心区域预期的扩散背景之上，有一个扩展的GeV γ射线过剩，这可以通过湮灭暗物质（DM）或毫秒星（MSP）来解释。我们建议观测甚高能量（VHE）γ射线，以区分MSP方案从DM方案。GeV的γ射线MSPs应该将其大部分能量释放到相对论e±风中，这些相对论e ±风将扩散到银河系中，并通过逆康普顿散射和韧致辐射过程辐射TeV的γ射线。通过计算谱和空间分布，我们证明了在合理的模型参数下，这种辐射是可以被下一代VHE γ射线天文台--切伦科夫望远镜阵列（CTA）探测到的。为了解决高能宇宙中的这个谜团，寻找GeV γ射线过剩的多波长对应物是必不可少的。
Recent analyses of Fermi Large Area Telescope data show an extended GeV γ-ray excess on top of the expected diffuse background in the Galactic center region, which can be explained by annihilating dark matter (DM) or a population of millisecond pulsars (MSPs). We propose observations of very high energy (VHE) γ-rays to distinguish the MSP scenario from the DM scenario. GeV γ-ray MSPs should release most of their energy to the relativistic e± wind, which will diffuse into the Galaxy and radiate TeV γ-rays through inverse Compton scattering and bremsstrahlung processes. By calculating the spectrum and spatial distribution, we show that such emission is detectable with the next generation VHE γ-ray observatory, the Cherenkov Telescope Array (CTA), under reasonable model parameters. It is essential to search for multi-wavelength counterparts to the GeV γ-ray excess in order to solve this mystery in the high-energy universe.