Recent baryon acoustic oscillation (BAO) measurements by the Dark Energy Spectroscopic Instrument (DESI) provide evidence that dark energy (DE) evolves with time, as parameterized by a w ₀ w _a equation of state. Cosmologically coupled black holes (BHs) provide a DE source that naturally evolves with time, because BH production tracks cosmic star-formation. Using DESI BAO measurements and priors informed by Big Bang Nucleosynthesis, we measure the fraction of baryonic density converted into BHs, assuming that all DE is sourced by BH production. We find that the best-fit DE density tracks each DESI best-fit w ₀ w _a model within 1σ, except at redshifts z ≲ 0.2, highlighting limitations of the w ₀ w _a parameterization. Cosmologically coupled BHs produce H ₀ = (69.94 ± 0.81) km s^-1 Mpc^-1, with the same χ ² as ΛCDM, and with two fewer parameters than w ₀ w _a . This value reduces tension with SH0ES to 2.7σ and is in excellent agreement with recent measurements from the Chicago-Carnegie Hubble Program. Because cosmologically coupled BH production depletes the baryon density established by primordial nucleosynthesis, these BHs provide a physical explanation for the “missing baryon problem” and the anomalously low sum of neutrino masses preferred by DESI. The global evolution of DE is an orthogonal probe of cosmological coupling, complementing constraints on BH mass-growth from elliptical galaxies, stellar binaries, globular clusters, the LIGO-Virgo-KAGRA merging population, and X-ray binaries. A DE density that correlates with cosmic star-formation: 1) is a natural outcome of cosmological coupling in BH populations; 2) eases tension between early and late-time cosmological probes; and 3) produces time-evolution toward a late-time ΛCDM cosmology different from Cosmic Microwave Background projections.

中文翻译：

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DESI 暗能量时间演化被宇宙耦合黑洞恢复


暗能量光谱仪 （DESI） 最近进行的重子声学振荡 （BAO） 测量提供了暗能量 （DE） 随时间演变的证据，如_{状态方程 w 0}w 所参数化的那样。宇宙耦合黑洞 （BH） 提供了一个随时间自然演变的 DE 源，因为 BH 的产生跟踪宇宙恒星的形成。使用 DESI BAO 测量和大爆炸核合成提供的先验信息，我们测量转化为 BH 的重子密度的分数，假设所有 DE 都来自 BH 生产。我们发现最佳拟合 DE 密度跟踪 1σ 内的每个 DESI 最佳拟合 w₀w _a 模型，除了红移 z ≲ 0.2，突出了 w₀w _a 参数化的局限性。宇宙耦合的 BH 产生 H₀ = （69.94 ± 0.81） km ^{s-1 Mpc-1，χ 2} 与 ΛCDM 相同，但参数比 w₀w _a 少两个。该值将 SH0ES 的张力降低到 2.7σ，并且与芝加哥-卡内基哈勃计划最近的测量结果非常吻合。因为宇宙耦合的 BH 产生耗尽了原始核合成建立的重子密度，所以这些 BH 为“缺失重子问题”和 DESI 首选的异常低中微子质量总和提供了物理解释。DE 的全球演化是宇宙耦合的正交探测器，补充了椭圆星系、恒星双星、球状星团、LIGO-Virgo-KAGRA 合并种群和 X 射线双星对 BH 质量增长的限制。 与宇宙恒星形成相关的 DE 密度：1） 是 BH 种群中宇宙学耦合的自然结果;2） 缓解早期和晚期宇宙学探测器之间的紧张关系;3） 产生与宇宙微波背景投影不同的晚期 ΛCDM 宇宙学的时间演化。