A constant early dark energy (EDE) component contributing a fraction $f_{\mathrm{EDE}}(z_c)\sim 10\%$ of the energy density of the universe around $z_c\simeq 3500$ and diluting as or faster than radiation afterwards, can provide a simple resolution to the Hubble tension, the $\sim 5\sigma$ discrepancy—in the $\mathrm{\Lambda }\mathrm{CDM}$ context—between the $H_0$ value derived from early- and late-universe observations. However, it has been pointed out that including Large-Scale Structure (LSS) data, which are in $\sim 3\sigma$ tension with $\mathrm{\Lambda }\mathrm{CDM}$ and EDE cosmologies, might break some parameter degeneracy and alter these conclusions. We reassess the viability of the EDE against a host of high- and low-redshift measurements, by combining LSS observations from recent weak lensing (WL) surveys with CMB, baryon acoustic oscillation (BAO), growth function (FS) and Supernova Ia (SNIa) data. Introducing a model whose only parameter is $f_{\mathrm{EDE}}(z_c)$, we report in agreement with past work a $\sim 2\sigma$ preference for nonzero $f_{\mathrm{EDE}}(z_c)$ from Planck CMB data alone, while the tension with the local $H_0$ measurement from sh0es is reduced below $2\sigma$. Adding BAO, FS and SNIa does not affect this conclusion, while the inclusion of a prior on $H_0$ from sh0es increase the preference for EDE over $\mathrm{\Lambda }\mathrm{CDM}$ to the $\sim 3.6\sigma$ level. After checking the EDE nonlinear matter power spectrum as predicted by standard semi-analytical algorithms via a dedicated set of $N$-body simulations, we test the 1-parameter EDE cosmology against WL data. We find that it does not significantly worsen the fit to the $S_8$ measurement as compared to $\mathrm{\Lambda }\mathrm{CDM}$, and that current WL observations do not exclude the EDE resolution to the Hubble tension. We also caution against the interpretation of constraints obtained from combining statistically inconsistent datasets within the $\mathrm{\Lambda }\mathrm{CDM}$ cosmology. In light of the CMB lensing anomalies, we show that the lensing-marginalized CMB data also favor nonzero $f_{\mathrm{EDE}}(z_c)$ at $\sim 2\sigma$, predicts $H_0$ in $1.4\sigma$ agreement with sh0es and $S_8$ in $1.5\sigma$ and $0.8\sigma$ agreement with kids-viking and des respectively. There still exists however a $\sim 2.5\sigma$ tension with the joint results from kids-viking and des. With an eye on Occam’s razor, we finally discuss promising extensions of the EDE cosmology that could allow us to fully restore cosmological concordance.

中文翻译：

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鉴于弱镜头调查和镜头异常，早期的暗能量分辨率可解决哈勃张力问题

恒定的早期暗能量（EDE）成分贡献了一部分 $F_{\mathrm{电子数据交换}}（{ž}_C）〜10％$ 周围宇宙的能量密度 ${ž}_C\simeq 3500$ 然后稀释或辐射得比辐射快，可以为哈勃张力提供一个简单的解决方案， $〜5\sigma$ 差异-在 $\mathrm{\Lambda }\mathrm{清洁发展机制}$ 上下文之间 $H_0$从早期和晚期宇宙观测中得出的价值。但是，已经指出，包括大型结构（LSS）数据，这些数据位于$〜3\sigma$ 紧张 $\mathrm{\Lambda }\mathrm{清洁发展机制}$和EDE宇宙学，可能会破坏某些参数的简并性并改变这些结论。我们结合最近的弱透镜（WL）勘测的LSS观测值与CMB，重子声振荡（BAO），生长函数（FS）和超新星Ia（ SNIa）数据。引入唯一参数为的模型$F_{\mathrm{电子数据交换}}（{ž}_C）$，我们同意与过去的工作进行合作 $〜\mathrm{2个}\sigma$ 非零偏好 $F_{\mathrm{电子数据交换}}（{ž}_C）$仅从普朗克CMB数据来看，而与当地的紧张关系$H_0$从sh 0 es的测量值减少到以下$\mathrm{2个}\sigma$。添加BAO，FS和SNIa不会影响此结论，而将先前的$H_0$从sh 0 es开始增加对EDE的偏好$\mathrm{\Lambda }\mathrm{清洁发展机制}$ 到 $〜3.6\sigma$等级。在检查标准半解析算法预测的EDE非线性物质功率谱后，通过一组专用的$ñ$体仿真，我们针对WL数据测试了1参数EDE宇宙学。我们发现它并没有显着恶化与${\mathrm{小号}}_8$ 测量与 $\mathrm{\Lambda }\mathrm{清洁发展机制}$，并且当前的WL观测值并未排除针对哈勃张力的EDE分辨率。我们也告诫不要对通过组合统计内不一致的数据集而获得的约束进行解释。$\mathrm{\Lambda }\mathrm{清洁发展机制}$宇宙学。鉴于CMB镜头异常，我们显示镜头边缘CMB数据也倾向于非零$F_{\mathrm{电子数据交换}}（{ž}_C）$ 在 $〜\mathrm{2个}\sigma$，预测 $H_0$ 在 $1.4\sigma$与sh 0 es达成协议，并且${\mathrm{小号}}_8$ 在 $1.5\sigma$ 和 $0.8\sigma$与k i ds的协议-分别是维京人和des。但是仍然存在$〜2.5\sigma$张力与从关节结果ķ我DS -海盗和DES。最后，我们着眼于Occam的剃刀，讨论了EDE宇宙学的有希望的扩展，这些扩展可能使我们能够完全恢复宇宙学的一致性。