Constraints on the presence of a 3.5 keV dark matter emission line from Chandra observations of the Galactic centre
Constraints on the presence of a 3.5 keV dark matter emission line from Chandra observations of the Galactic centre
复制标题
钱德拉对银河中心的观测对 3.5 keV 暗物质发射线存在的限制
DOI：
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发表时间：
2016
期刊：
影响因子：
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通讯作者：
S. Riemer
中科院分区：
文献类型：
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作者：
S. Riemer
上下文最近发现的线发射在3.5千电子伏的星系团的个人和堆叠的X射线光谱已被推测有暗物质的起源。目标。如果起源确实是暗物质，那么发射线预计可以从银河系暗物质晕中检测到。方法.我们在公共钱德拉X射线观测的Sgr A* 附近的区域进行线搜索。我们推导了2.0 - 9.0 keV能量区间的线发射通量上限，并讨论了它们潜在的物理解释，包括暗物质衰变和湮灭的各种场景。结果虽然我们没有发现它存在的明确证据，但流量上限与最近对银河系保守质量分布的探测并不矛盾。结论.结果轻微地依赖于光谱模型，强烈地依赖于暗物质轮廓的选择。
Context. Recent findings of line emission at 3.5 keV in both individual and stacked X-ray spectra of galaxy clusters have been speculated to have dark matter origin. Aims. If the origin is indeed dark matter, the emission line is expected to be detectable from the Milky Way dark matter halo. Methods. We perform a line search in public Chandra X-ray observations of the region near Sgr A*. We derive upper limits on the line emission flux for the 2.0−9.0 keV energy interval and discuss their potential physical interpretations including various scenarios of decaying and annihilating dark matter. Results. While we find no clear evidence for its presence, the upper flux limits are not inconsistent with the recent detections for conservative mass profiles of the Milky Way. Conclusions. The results depend mildly on the spectral modelling, and strongly on the choice of dark matter profile.