Clustering and halo abundances in early dark energy cosmological models
Clustering and halo abundances in early dark energy cosmological models
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DOI：
10.1093/mnras/stab769
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发表时间：
2021-04-21
影响因子：
4.8
通讯作者：
Smith, Tristan L.
中科院分区：
文献类型：
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作者：
Klypin, Anatoly;Poulin, Vivian;Smith, Tristan L.
具有早期暗能量（EDE）的冷暗物质（Lambda CDM）宇宙学模型已经被提出，以解决哈勃常数km (-1)Mpc（-1）之间的紧张关系，使h近似于0.73，而从普朗克宇宙微波背景（CMB）和其他早期宇宙测量中推断出的h -0加上Lambda CDM，使h近似于0.67。EDE模型通过增加一个标量场来实现这一点，该标量场暂时增加了暗能量，相当于辐射主导时代结束时宇宙能量密度的10%，红移z类似于3500。在这里，我们比较了包括EDE （h = 0.728）在内的普朗克归一化Lambda CDM模型的线性和非线性预测与h = 0.678的标准普朗克归一化Lambda CDM模型的预测。我们发现非线性演化减小了低红移时波动功率谱之间的差异。因此，在z = 0时，星系尺度上的光晕质量函数几乎相同，只有1- 2%的差异。然而，在高红移处，差异显著增加。EDE模型预测，在z = 1处，大质量星团会增加50%，在z = 4处，星系质量晕会增加两倍。在更高的红移处，星系质量晕的丰度增加得更大，可能更容易用EDE再电离宇宙。詹姆斯·韦伯太空望远镜（JWST）的观测将很快验证预测的星系丰度和群集。重子声学振荡（BAOs）和相关函数的位置在两个模型之间相差约2%——这种影响不会被非线性所消除。这里研究的标准Lambda CDM和EDE模型都与目前可用的声学尺度观测结果非常吻合，但暗能量光谱仪器和欧几里得测量将提供严格的新测试。
Cold Dark Matter with cosmological constant (Lambda CDM) cosmological models with early dark energy (EDE) have been proposed to resolve tensions between the Hubble constant kms(-1)Mpc(-1) measured locally, giving h approximate to 0.73, and H-0 deduced from Planck cosmic microwave background (CMB) and other early-Universe measurements plus Lambda CDM, giving h approximate to 0.67. EDE models do this by adding a scalar field that temporarily adds dark energy equal to about 10percent of the cosmological energy density at the end of the radiation-dominated era at redshift z similar to 3500. Here, we compare linear and non-linear predictions of a Planck-normalized Lambda CDM model including EDE giving h = 0.728 with those of standard Planck-normalized Lambda CDM with h = 0.678. We find that non-linear evolution reduces the differences between power spectra of fluctuations at low redshifts. As a result, at z = 0 the halo mass functions on galactic scales are nearly the same, with differences only 1-2percent. However, the differences dramatically increase at high redshifts. The EDE model predicts 50percent more massive clusters at z = 1 and twice more galaxy-mass haloes at z = 4. Even greater increases in abundances of galaxy-mass haloes at higher redshifts may make it easier to reionize the universe with EDE. Predicted galaxy abundances and clustering will soon be tested by the James Webb Space Telescope (JWST) observations. Positions of baryonic acoustic oscillations (BAOs) and correlation functions differ by about 2percent between the models - an effect that is not washed out by non-linearities. Both standard Lambda CDM and the EDE model studied here agree well with presently available acoustic-scale observations, but the Dark Energy Spectroscopic Instrument and Euclid measurements will provide stringent new tests.