从WMAP霾看用GLAST探测暗物质的前景
Prospects For Detecting Dark Matter With GLAST In Light Of The WMAP Haze
摘要：
WMAP实验的观测已经确定了来自银河系中心的过量微波辐射。先前已经表明，这种“WMAP薄雾”可能是暗物质粒子湮灭时产生的相对论电子和正电子的同步辐射。特别是，WMAP霾的强度、光谱和角分布与电弱标度的暗物质粒子（如具有普适额外维度的模型中的超对称中性伴子或卡鲁扎-克莱因暗物质）相一致，其湮灭的截面约为σ v~ 3 × 10 ^-26 cm ^3/s，并以尖晕轮廓分布。不需要进一步的奇异天体物理或湮灭助推因子。如果暗物质湮灭实际上是观测到的霾的原因，那么其他湮灭产物也将产生，包括伽马射线。在这篇文章中，我们研究的前景GLAST卫星探测伽马射线的暗物质湮灭在银河系中心地区在这种情况下。我们发现，通过研究银河系中心周围的内部0.1度，GLAST将能够检测到暗物质湮灭为重夸克或规范玻色子超过天体物理背景与5西格玛（3西格玛）的意义，如果他们是轻于约320-500 GeV（500-750 GeV）。如果将角窗扩大以研究暗物质晕轮廓的角扩展（同时减少天体物理背景），那么GLAST可以识别出重达几TeV的WIMP，具有很高的意义。只有当暗物质粒子湮灭为电子或μ子时，GLAST才无法识别与WMAP霾相关的伽马射线谱。
英文摘要：
Observations by the WMAP experiment have identified an excess of microwave emission from the center of the Milky Way. It has previously been shown that this "WMAP Haze" could be synchrotron emission from relativistic electrons and positrons produced in the annihilations of dark matter particles. In particular, the intensity, spectrum and angular distribution of the WMAP Haze is consistent with an electroweak scale dark matter particle (such as a supersymmetric neutralino or Kaluza-Klein dark matter in models with universal extra dimensions) annihilating with a cross section on the order of sigma v~3x10^-26 cm^3/s and distributed with a cusped halo profile. No further exotic astrophysical or annihilation boost factors are required. If dark matter annihilations are in fact responsible for the observed Haze, then other annihilation products will also be produced, including gamma rays. In this article, we study the prospects for the GLAST satellite to detect gamma rays from dark matter annihilations in the Galactic Center region in this scenario. We find that by studying only the inner 0.1 degrees around the Galactic Center, GLAST will be able to detect dark matter annihilating to heavy quarks or gauge bosons over astrophysical backgrounds with 5sigma (3sigma) significance if they are lighter than approximately 320-500 GeV (500-750 GeV). If the angular window is broadened to study the dark matter halo profile's angular extension (while simultaneously reducing the astrophysical backgrounds), WIMPs as heavy as several TeV can be identified by GLAST with high significance. Only if the dark matter particles annihilate mostly to electrons or muons will GLAST be unable to identify the gamma ray spectrum associated with the WMAP Haze.
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