Constraining dark energy through the stability of cosmic structures

Pavlidou, V.; Tetradis, N.; Tomaras, T.N.

doi:10.1088/1475-7516/2014/05/017

Cited by 55 publications

(128 citation statements)

References 37 publications

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“…On the other hand, the greater the value of the cosmological constant, the earlier structure formation stops. Similar predictions can be made [32] for a dark energy equation of state different from w = −1 or for the quintessence model. We have chosen to concentrate on the simpler, currently consistent with data ΛCDM model.…”

Section: Discussionsupporting

confidence: 73%

Testing ΛCDM cosmology at turnaround:whereto look for violations of the bound?

Tanoglidis

Pavlidou

Tomaras

2015

J. Cosmol. Astropart. Phys.

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Abstract. In ΛCDM cosmology, structure formation is halted shortly after dark energy dominates the mass/energy budget of the Universe. A manifestation of this effect is that in such a cosmology the turnaround radius -the non-expanding mass shell furthest away from the center of a structure-has an upper bound. Recently, a new, local, test for the existence of dark energy in the form of a cosmological constant was proposed based on this turnaround bound. Before designing an experiment that, through high-precision determination of masses and -independentlyturnaround radii, will challenge ΛCDM cosmology, we have to answer two important questions: First, when turnaround-scale structures are predicted to be close enough to their maximum size, so that a possible violation of the bound may be observable. Second, which is the best mass scale to target for possible violations of the bound. These are the questions we address in the present work. Using the Press-Schechter formalism, we find that turnaround structures have in practice already stopped forming, and consequently, the turnaround radius of structures must be very close to the maximum value today. We also find that the mass scale of ∼ 10 13 M ⊙ characterizes the turnaround structures that start to form in a statistically important number density today -and even at an infinite time in the future, since structure formation has almost stopped. This mass scale also separates turnaround structures with qualitative different cosmological evolution: smaller structures are no longer readjusting their mass distribution inside the turnaround scale, they asymptotically approach their ultimate abundance from higher values, and they are common enough to have, at some epoch, experienced major mergers with structures of comparable mass; larger structures exhibit the opposite behavior. We call this mass scale the transitional mass scale and we argue that it is the optimal for the purpose outlined above. As a corollary result, we explain the different accretion behavior of small and larger structures observed in already conducted numerical simulations.

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Section: Discussionsupporting

confidence: 73%

Testing ΛCDM cosmology at turnaround:whereto look for violations of the bound?

Tanoglidis

Pavlidou

Tomaras

2015

J. Cosmol. Astropart. Phys.

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“…It was suggested recently that the turnaround radius is a possible probe of dark energy or modified gravity scenarios [3,4,5,6] but the concept of turnaround radius is older [7].…”

Section: Turnaround Radius With Hawking Mass In Grmentioning

confidence: 99%

“…and it is suggested implicitly in [5] that M (r) is the Lemaître mass (2.6), from which one obtains the turnaround radius [5] …”

Section: (27)mentioning

confidence: 99%

“…Our new criterion identifies the turnaround radius by equating the two contributions to the quasilocal mass, which yields a (3w+4)/3 . For comparison, the ratio of the turnaround radius (2.14) to that of [5] is…”

Section: Pos(eps-hep2017)037mentioning

confidence: 99%

“…The turnaround radius may provide a way to constrain the equation of state parameter w of dark energy. One can express it as a function of redshift R c (z) and obtain [5] …”

Section: Pos(eps-hep2017)037mentioning

confidence: 99%

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The turnaround radius as a probe of dark energy and modified gravity

Faraoni¹

2018

Proceedings of the European Physical Society Conference on High Energy Physics — PoS(EPS-HEP2017)

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Does the Corona Borealis Supercluster form a giant binary-like system?

Pillastrini¹

2016

Astrophys Space Sci

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The distribution of local gravitational potentials generated by a complete volume-limited sample of galaxy groups and clusters filling the Corona Borealis region has been derived to search for new gravitational hints in the context of clustering analysis unrevealed by alternative methodologies. Mapping such a distribution as a function of spatial positions, the deepest potential wells in the sample trace unambiguously the locations of the densest galaxy cluster clumps providing the physical keys to bring out gravitational features connected to the formation, composition and evolution of the major clustered structures filling that region. As expected, the three deepest potential wells found at Equatorial coordinates: (~ 230°, ~ 28°, z ~ 0.075), (~ 240°, ~ 27°, z ~ 0.09) and, (227°, 5.8°, z ~ 0.0788) correspond to massive superclusters of galaxy groups and clusters identified as the Corona Borealis, A2142 and Virgo-Serpent, respectively. However, the deepest isopotential contours around the Corona Borealis and A2142 superclusters seem to suggest a gravitational feature similar to a giant binary-like system connected by a filamentary structure. To a first approximation, it seems unlikely that this hypothesized system could be gravitationally bound.

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Constraining dark energy through the stability of cosmic structures

Cited by 55 publications

References 37 publications

Testing ΛCDM cosmology at turnaround:whereto look for violations of the bound?

Testing ΛCDM cosmology at turnaround:whereto look for violations of the bound?

The turnaround radius as a probe of dark energy and modified gravity

Does the Corona Borealis Supercluster form a giant binary-like system?

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