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Reconstructing Dark Energy
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abstract
This review summarizes recent attempts to reconstruct the expansion history of the Universe and to probe the nature of dark energy. Reconstruction methods can be broadly classified into parametric and non-parametric approaches. It is encouraging that, even with the limited observational data currently available, different approaches give consistent results for the reconstruction of the Hubble parameter $H(z)$ and the effective equation of state $w(z)$ of dark energy. Model independent reconstruction using current data allows for modest evolution of dark energy density with redshift. However, a cosmological constant (= dark energy with a constant energy density) remains an excellent fit to the data. Some pitfalls to be guarded against during cosmological reconstruction are summarized and future directions for the model independent reconstruction of dark energy are explored.
Forward citations
Cited by 4 Pith papers
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Evolving Dark Energy from the Back-Reaction of Cosmological Perturbations
Back-reaction of cosmological inhomogeneities can make an effective dark energy with a time-dependent equation of state and no phantom crossing, even for a global average.
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Entropic Chaplygin-Gas cosmology and late-universe tension diagnostics
An entropic Chaplygin-gas dark sector can shift fitted H0 values, but the shift and any tension relief depend on supernova calibration and vanish with DES-Dovekie data.
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Constraints on Dark Energy Models Using Late Universe Probes
Using late-universe probes only, the authors find all dark energy models remain within 1-2 sigma of Lambda CDM, which wins the Bayesian model comparison, and confirm that DESI's LRG1 and LRG2 points drive the dynamica...
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Effective Phantom Dark Energy: What Cosmological Reconstruction Does and Does Not Imply
Effective phantom dark energy is a background-level reconstruction that does not imply fundamental pathologies such as ghost instabilities or null energy condition violation by the underlying stress tensor.
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