The observed values of the cosmological constant {\it and} the abundance ofDark Matter (DM) can be successfully understood, using certain measures, byimposing the anthropic requirement that density perturbations go non-linear andvirialize to form halos. This requires a probability distribution favoring lowamounts of DM, i.e. low values of the PQ scale $f$ for the QCD axion and lowvalues of the superpartner mass scale $\tilde{m}$ for LSP thermal relics. Intheories with independent scanning of multiple DM components, there is a highprobability for DM to be dominated by a single component. For example, withindependent scanning of $f$ and $\tilde{m}$, TeV-scale LSP DM and an axionsolution to the strong CP problem are unlikely to coexist. With thermal LSP DM,the scheme allows an understanding of a Little SUSY Hierarchy with multi-TeVsuperpartners. Alternatively, with axion DM, PQ breaking before (after)inflation leads to $f$ typically below (below) the projected range of thecurrent ADMX experiment of $f = (3 - 30) \times 10^{11}$ GeV, providing strongmotivation to develop experimental techniques for probing lower $f$.
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机译：通过使用某些措施，通过人类要求密度扰动变为非线性并虚拟化以形成光晕，可以使用某些措施成功地理解宇宙常数{\ it和}的观测值。这需要有利于DM含量低的概率分布，即QCD轴的PQ标度$ f $的低值和LSP热文物的超级伙伴质量标度$ \ tilde {m} $的低值。在具有独立扫描多个DM组件的理论中，DM极有可能由单个组件控制。例如，$ f $和$ \ tilde {m} $的独立扫描，TeV级LSP DM和针对强CP问题的轴距解决方案不太可能共存。使用热LSP DM，该方案可以了解具有多个TeVsuperpartners的Little SUSY层次结构。或者，对于axion DM，在通货膨胀之前（之后）PQ破裂会导致$ f $通常低于（以下）当前ADMX实验的预计范围$ f =（3-30）\ times 10 ^ {11} $ GeV，从而提供开发用于探测较低$ f $的实验技术的强烈动机。
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