Indirect dark matter searches: towards a consistent top-bottom approach for studying the gamma-ray signals and associated backgrounds
Indirect dark matter searches: towards a consistent top-bottom approach for studying the gamma-ray signals and associated backgrounds
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间接暗物质搜索：采用一致的自上而下方法来研究伽马射线信号和相关背景
DOI：
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发表时间：
2012
期刊：
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通讯作者：
R. Teyssier
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作者：
E. Nezri;J. Lavalle;R. Teyssier
虽然暗物质（DM）是成功的结构形成理论的关键因素，但其微观性质仍然难以捉摸。间接检测可以为一些强动机的DM粒子模型提供强有力的测试。然而，天体物理背景通常预期具有与追踪信号类似的振幅和光谱特征。在银河系尺度上，这些背景来自宇宙射线（CR）与星际气体的相互作用，两者都很难从观测中详细推断和建模。此外，相关的预测必然伴随着理论误差，这是众所周知的。我们表明，一个值得信赖的指南，这种具有挑战性的搜索，可以通过利用宇宙学模拟的星系，现在包括重子气体动力学和星星形成的全部信息。我们进一步插入CR生产和运输从确定的超新星事件，并充分计算CR分布在一个模拟星系。我们专注于漫射伽马射线，并自洽地计算天体物理银河系的发射和暗物质信号。值得注意的是，绝热收缩并不一定会导致大的信号噪声比在银河系中心，无论如何，可以追溯到天体物理背景本身。最后，我们将讨论如何所有这一切可能被用来作为一个通用的诊断工具，星系的形成。
While dark matter (DM) is the key ingredient for a successful theory of structure formation, its microscopic nature remains elusive. Indirect detection may provide a powerful test for some strongly motivated DM particle models. Nevertheless, astrophysical backgrounds are usually expected with amplitudes and spectral features similar to the chased signals. On galactic scales, these backgrounds arise from interactions of cosmic rays (CRs) with the interstellar gas, both being difficult to infer and model in detail from observations. Moreover, the associated predictions unavoidably come with theoretical errors, which are known to be significant. We show that a trustworthy guide for such challenging searches can be obtained by exploiting the full information contained in cosmological simulations of galaxies, which now include baryonic gas dynamics and star formation. We further insert CR production and transport from the identified supernova events and fully calculate the CR distribution in a simulated galaxy. We focus on diffuse gamma-rays, and self-consistently calculate both the astrophysical galactic emission and the dark matter signal. We notably show that adiabatic contraction does not necessarily induce large signal-to-noise ratios in galactic centers, and could anyway be traced from the astrophysical background itself. We finally discuss how all this may be used as a generic diagnostic tool for galaxy formation.