arXiv 2112.032932021-12astro-ph.CO

亚星系尺度上的原始物质功率谱

The primordial matter power spectrum on sub-galactic scales

Daniel Gilman, Andrew Benson, Jo Bovy, Simon Birrer, Tommaso Treu, Anna Nierenberg

备注：: accepted to MNRAS; includes expanded discussion of results, tests with simulated data, and additional references
DOI：: 10.1093/mnras/stac670

摘要：

原始物质功率谱量化了紧接着暴胀之后暗物质分布的波动。随着宇宙时间的推移，太初密度场的过密区域生长并坍缩成暗物质晕，其丰度和密度分布保留着初始条件的记忆。通过分析11个强透镜和四倍像类星体的像放大率，我们推断了低质量晕的丰度和浓度，并将测量结果与原始物质功率谱的振幅联系起来。我们锚定大尺度上的功率谱，隔离的影响，小尺度偏差的$Λ$ CDM预测。假设一个功率谱的分析模型，并考虑几个潜在的系统不确定性的来源，包括晕质量函数的三个不同模型，我们得到了$\log_{10}\left(P / P_{Λ\rm{CDM}}\right)$的相关推论，功率谱振幅相对于协调宇宙学模型的预测，$0.0_{-0.4}^{+0.5}$，$0.1_{-0.6}^{+0.7}$，和$0.2_{-0.9}^{+1.0}$在k = 10，25和50 $\rm{Mpc^{-1}}$在$68 \%$置信度，与冷暗物质和单场慢卷暴胀相一致。

英文摘要：

The primordial matter power spectrum quantifies fluctuations in the distribution of dark matter immediately following inflation. Over cosmic time, over-dense regions of the primordial density field grow and collapse into dark matter halos, whose abundance and density profiles retain memory of the initial conditions. By analyzing the image magnifications in eleven strongly-lensed and quadruply-imaged quasars, we infer the abundance and concentrations of low-mass halos, and cast the measurement in terms of the amplitude of the primordial matter power spectrum. We anchor the power spectrum on large scales, isolating the effect of small-scale deviations from the $Λ$CDM prediction. Assuming an analytic model for the power spectrum and accounting for several sources of potential systematic uncertainty, including three different models for the halo mass function, we obtain correlated inferences of $\log_{10}\left(P / P_{Λ\rm{CDM}}\right)$, the power spectrum amplitude relative to the predictions of the concordance cosmological model, of $0.0_{-0.4}^{+0.5}$, $0.1_{-0.6}^{+0.7}$, and $0.2_{-0.9}^{+1.0}$ at k = 10, 25 and 50 $\rm{Mpc^{-1}}$ at $68 \%$ confidence, consistent with cold dark matter and single-field slow-roll inflation.

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