利用 DESI 2024 数据发布中经校准的 $E_p-E_{iso}$ 伽马射线暴关联给出的宇宙学约束
Cosmological constraints from calibrated $E_p-E_{iso}$ gamma-ray burst correlation by using DESI 2024 data release
AI总结：
本文利用 DESI 2024 数据和 Bézier 插值校准伽马射线暴 Amati 关联，并结合 MCMC 约束多种暗能量模型，发现曲率为零时偏好 ΛCDM，而演化暗能量可能仍存在于高红移。
摘要：
DESI 合作组的近期结果揭示了暗能量可能存在轻微演化，从而对标准 $Λ$CDM 范式提出挑战。为更好地理解暗能量的本质，诸如伽马射线暴数据等高红移观测对于描绘宇宙膨胀历史变得至关重要，前提是它们需与其他探针一起完成校准。为此，我们通过对更新后的哈勃率和新颖的 DESI 数据集进行模型无关的 Bézier 插值，校准了 $E_p-E_{iso}$（或称 Amati）关联。更具体地说，我们提供两种 Bézier 校准：i）处理完整 DESI 样本；ii）排除近期文献所质疑的 $z_{eff}=0.51$ 数据点。在这两种选择中，我们都允许拖拽时期的共动声视界 $r_d$ 在 $r_d \in [138,156]$ Mpc 范围内变化。为便于比较，我们也考察了 Planck 数值。借助由此校准的伽马射线暴，我们进而在空间平坦和非平坦宇宙中约束三种暗能量框架，即标准 $Λ$CDM、$ω_0$CDM 和 $ω_0ω_1$CDM 模型。为此，我们采用 Metropolis-Hastings 算法开展了 Monte Carlo Markov chain 分析。此外，我们采用模型选择准则来检验统计上更受偏好的宇宙学模型，结果发现只有在空间曲率为零时才倾向于 concordance（协和）范式。相反且相当有趣的是，平坦 $ω_0$CDM 以及平坦/非平坦两种情形下的 $ω_0ω_1$CDM 模型，显然保留了暗能量在更高红移处发生演化的可能性。
英文摘要：
Recent outcomes by the DESI Collaboration have shed light on a possible slightly evolving dark energy, challenging the standard $Λ$CDM paradigm. To better understand dark energy nature, high-redshift observations like gamma-ray burst data become essential for mapping the universe expansion history, provided they are calibrated with other probes. To this aim, we calibrate the $E_p-E_{iso}$ (or Amati) correlation through model-independent Bézier interpolations of the updated Hubble rate and the novel DESI data sets. More precisely, we provide two Bézier calibrations: i) handling the entire DESI sample, and ii) excluding the point at $z_{eff}=0.51$, criticized by the recent literature. In both the two options, we let the comoving sound horizon at the drag epoch, $r_d$, vary in the range $r_d \in [138, 156]$ Mpc. The Planck value is also explored for comparison. By means of the so-calibrated gamma-ray bursts, we thus constrain three dark energy frameworks, namely the standard $Λ$CDM, the $ω_0$CDM and the $ω_0ω_1$CDM models, in both spatially flat and non-flat universes. To do so, we worked out Monte Carlo Markov chain analyses, making use of the Metropolis-Hastings algorithm. Further, we adopt model selection criteria to check the statistically preferred cosmological model finding a preference towards the concordance paradigm only whether the spatial curvature is zero. Conversely, and quite interestingly, the flat $ω_0$CDM and both the cases, flat/non-flat, $ω_0ω_1$CDM model, leave evidently open the chance that dark energy evolves at higher redshifts.
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