Built on

E. J. Copeland, I. J. Grivell, and A. R. Liddle, Cosmological parameter estimation and the spectral index from inflation , Mon. Not. Roy. Astron. Soc. 298, 1233 (1998) [arXiv:astro-ph/9712028]
1998
Earlier work this paper cites.
M. Chevallier and D. Polarski, Accelerating Universes with Scaling Dark Matter , Int. J. Mod. Phys. D10, 213 (2001) [arXiv:gr-qc/0009008]
2001
Earlier work this paper cites.
D. Huterer and M. S. Turner, Probing the dark energy: methods and strategies , Phys. Rev. D64, 123527 (2001) [arXiv:astro-ph/0012510]
2001
Earlier work this paper cites.
R. R. Caldwell, A Phantom Menace? Cosmological consequences of a dark energy component with super-negative equation of state , Phys. Lett. B545, 23 (2002) [arXiv:astro-ph/9908168]
2002
Earlier work this paper cites.
E. V. Linder, Exploring the Expansion History of the Universe , Phys. Rev. Lett. 90, 091301 (2003) [arXiv:astro-ph/0208512]
2003
Earlier work this paper cites.
A. Vikman, Can dark energy evolve to the Phantom? , Phys. Rev. D71, 023515 (2005) [arXiv:astro-ph/0407107]
2005
Earlier work this paper cites.
W. Hu, Crossing the Phantom Divide: Dark Energy Internal Degrees of Freedom , Phys. Rev. D71, 047301 (2005), [arXiv:astro-ph/0410680]
2005
Earlier work this paper cites.
R. R. Caldwell and M. Doran, Dark-Energy Evolution Across the Cosmological-Constant Boundary , Phys. Rev. D72, 043527 (2005) [arXiv:astro-ph/0501104]
2005
Earlier work this paper cites.
E. J. Copeland, M. Sami, and S. Tsujikawa, Dynamics of dark energy , Int. J. Mod. Phys. D15, 1753 (2006) [arXiv:hep-th/0603057]
2006
Earlier work this paper cites.
A. Albrecht et al., Report of the Dark Energy Task Force , arXiv:astro-ph/0609591 (2006)
2006
Earlier work this paper cites.
E. V. Linder, Biased Cosmology: Pivots, Parameters, and Figures of Merit , Astropart. Phys. 26, 102 (2006) [arXiv:astro-ph/0604280]
2006
Earlier work this paper cites.
D. Martin and A. Albrecht, Talk about Pivots , [arXiv:astro-ph/0604401] (2006)
2006
Earlier work this paper cites.
S. Nesseris and L. Perivolaropoulos, Crossing the Phantom Divide: Theoretical Implications and Observational Status , JCAP 0701, 018 (2007) [arXiv:astro-ph/0610092]
2007
Earlier work this paper cites.

Similar

D. N. Spergel et al. (WMAP Collaboration), Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology , Astrophys. J. Suppl. 170, 377 (2007) [arXiv:astro-ph/0603449]
2007
Cited alongside, same era.
M. Cortês, A. R. Liddle, and P. Mukherjee, On what scale should inflationary observables be constrained? , Phys. Rev. D75, 083520 (2007) [arXiv:astro-ph/0702170]
2007
Cited alongside, same era.
S. Aiola et al., The Atacama Cosmology Telescope: DR4 maps and cosmological parameters , JCAP 2020, 647 (2020) [arXiv:2007.07288 [astro-ph.CO]]
Original
2007
Cited alongside, same era.
S. Alam et al. (eBOSS Collaboration), Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Apache Point Observatory , Phys. Rev. D103, 083533 (2021) [arXiv:2007.08991 [astro-ph.CO]]
Original
2007
Cited alongside, same era.

Then

Beyond the bibliography

alphaXiv searches the wider corpus for related work and actual follow-ups.

Open on alphaXiv

alphaXiv is searching for related work…

Reading the bibliography…

2024

Interpreting DESI's evidence for evolving dark energy

Cortês, Marina, Liddle, Andrew R

Understand

The latest results on baryon acoustic oscillations from DESI (Dark Energy Spectroscopic Instrument), when combined with cosmic microwave background and supernova data, show indications of a deviation from a cosmological constant in favour of evolving dark energy.

Use of a pivot scale for the equation of state $w$ shows that this evidence is concentrated in the derivative of $w$ rather than its mean offset from $-1$, indicating a new cosmic coincidence where the mean equation of state matches that of the $\Lambda$CDM model precisely in the region probed by the observations.
An equivalent way to express this is to say that the dark energy hits the maximum value that it will ever achieve within the observed window.
We argue that conclusions on dark energy evolution are strongly driven by the assumed parameter priors and that this coincidence, which we are naming the PhantomX coincidence (where X stands for crossing), may be a signature of this.