Constraints on the Cosmological Parameters with Three-Parameter Correlation of Gamma-Ray Bursts
Constraints on the Cosmological Parameters with Three-Parameter Correlation of Gamma-Ray Bursts
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DOI：
10.3847/1538-4357/ace107
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发表时间：
2023-06
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通讯作者：
Jia-Lun Li;Yupeng Yang;S. Yi;Jian-Ping Hu;Fayin Wang;Y. Qu
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作者：
Jia-Lun Li;Yupeng Yang;S. Yi;Jian-Ping Hu;Fayin Wang;Y. Qu
伽玛射线暴（GRB）是宇宙中能量最高、亮度最大的事件之一，是研究高红移宇宙的重要手段。与Ia型超新星类似，具有相同物理起源的伽玛暴可以被视为标准烛光。我们选取了具有相同物理起源的伽玛暴样品，将其分为两组。第一组由31个伽玛暴组成，具有恒定亮度的平台相位特征，在X射线余辉光变曲线中的衰减指数约为-2，第二组有50个伽玛暴，在光学光变曲线中具有浅衰减相位。对于所选的GRB样品，我们证实了平台光度L0、平台结束时间t B和各向同性能量释放E γ，iso之间存在紧密的相关性。我们还发现，L0-t B − E γ，iso关联对宇宙学参数不敏感，并且利用这种关联不能得到对宇宙学参数的有效限制.我们探索了一个新的三参数关联L0，t B和静止坐标系Ep，i（L0-t B -Ep，i）中的谱峰能量，发现这个关联可以作为标准烛光来约束宇宙学参数.通过仅使用光学样本，我们发现了平坦ΛCDM模型的约束Ωm=0.697−0.278+0.402（1σ）。对于非平坦ΛCDM模型，最佳拟合结果为Ωm=0.713−0.278+0.346，ΩΛ=0.981−0.580+0.379（1σ）.对于X射线和光学样品的组合，我们发现对于平坦的ΛCDM模型，Ωm=0.313−0.125+0.179（1σ），对于非平坦的Λ CDM模型，Ωm=0.344−0.112+0.176，ΩΛ=0.770−0.416+0.366（1σ）。
As one of the most energetic and brightest events, gamma-ray bursts (GRBs) can be treated as a promising probe of the high-redshift universe. Similar to type Ia supernovae, GRBs with the same physical origin could be treated as standard candles. We select GRB samples with the same physical origin, which are divided into two groups. The first group consists of 31 GRBs with a plateau phase feature of a constant luminosity followed by a decay index of about −2 in the X-ray afterglow light curves, and the second group has 50 GRBs with a shallow decay phase in the optical light curves. For the selected GRB samples, we confirm that there is a tight correlation between the plateau luminosity L 0, the end time of plateau t b , and the isotropic energy release E γ,iso. We also find that the L 0–t b − E γ,iso correlation is insensitive to the cosmological parameters and that no valid limitations on the cosmological parameters can be obtained using this correlation. We explore a new three-parameter correlation L 0, t b , and the spectral peak energy in the rest-frame E p,i (L 0–t b –E p,i ), and find that this correlation can be used as a standard candle to constrain the cosmological parameters. By employing the optical sample only, we find the constraints of Ωm=0.697−0.278+0.402(1σ) for a flat ΛCDM model. For the non-flat ΛCDM model, the best-fitting results are Ωm=0.713−0.278+0.346 , ΩΛ=0.981−0.580+0.379(1σ) . For the combination of the X-ray and optical samples, we find Ωm=0.313−0.125+0.179(1σ) for a flat ΛCDM model, and Ωm=0.344−0.112+0.176 , ΩΛ=0.770−0.416+0.366(1σ) for a non-flat ΛCDM model.