通过积分萨克斯-沃尔夫效应利用盖亚类星体探测暗能量演化
Probing dark energy evolution with Quaia quasars through the integrated Sachs-Wolfe effect
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中文总结 AI 辅助
研究利用积分萨克斯-沃尔夫效应，通过对盖亚类星体目录和普朗克CMB温度图的层析交叉相关分析，测量宽红移范围的ISW信号，检测到该效应，其振幅比ΛCDM预测稍强，为暗能量演化研究提供新约束。
中文摘要 AI 辅助
积分萨克斯-沃尔夫（ISW）效应探测引力势的晚期演化，并为暗能量的性质提供补充检验。我们研究ISW效应的红移演化是否能为暗能量的时间演化提供新的约束。考虑了标准ΛCDM宇宙学和近期DESI BAO及DES Y6约束支持的替代w0waCDM模型的理论预测。对盖亚类星体目录和普朗克CMB温度图进行层析交叉相关分析，以测量跨越约(10h−1 Gpc)3共动体积的宽红移范围内的ISW信号。评估了推断的ISW振幅对天空覆盖、多极范围和层析分箱变化的稳健性。以2.8σ的显著性检测到ISW效应，相对于普朗克ΛCDM预测，振幅AISW≃1.69±0.61。推断的信号在各种分析选择下保持稳定。测量的ISW振幅比基准ΛCDM宇宙学预测稍强，替代w0waCDM模型无法解释这种差异。未来利用盖亚改进的类星体目录以及即将进行的大面积星系巡天（如欧几里得和DESI）进行的层析ISW测量将有助于阐明这种差异的起源。
英文摘要
The Integrated Sachs--Wolfe (ISW) effect probes the late-time evolution of gravitational potentials and provides a complementary test of the nature of dark energy. We investigate whether the redshift evolution of the ISW effect can provide new constraints on the time evolution of dark energy. We consider theoretical predictions for the standard $Λ$CDM cosmology and alternative $w_0w_a$CDM models favoured by recent DESI BAO and DES Y6 constraints. We perform a tomographic cross-correlation analysis of the {\it Quaia} quasar catalogue and \textit{Planck} CMB temperature maps to measure the ISW signal over a broad redshift range, spanning about $(10h^{-1}~\mathrm{Gpc})^3$ comoving volume. We assess the robustness of the inferred ISW amplitude against variations in sky coverage, multipole range, and tomographic binning. We detect the ISW effect at a significance of $2.8 \, σ$, corresponding to an amplitude of $A_{\rm ISW}\simeq1.69\pm0.61$ relative to the \textit{Planck} $Λ$CDM prediction. The inferred signal remains stable against various analysis choices, including various CMB maps (SMICA, NILC, SEVEM), different choices of $\ell_{\rm max}$ and the number of multipole bins, and an alternative quasar bias model. The measured ISW amplitude is moderately stronger than predicted by the fiducial $Λ$CDM cosmology, and the alternative $w_0w_a$CDM models do not account for this discrepancy. Future tomographic ISW measurements with improved quasar catalogues from {\it Gaia} and forthcoming wide-area galaxy surveys such as {\it Euclid} and DESI will help clarify the origin of this difference.
