Forecast and analysis of the cosmological redshift drift

Lazkoz, Ruth; Leanizbarrutia, Iker; Salzano, Vincenzo

doi:10.1140/epjc/s10052-017-5479-0

Cited by 13 publications

(8 citation statements)

References 85 publications

(117 reference statements)

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“…In the present work we further quantify this statement. Two other recent forecasts, with more optimistic assumptions on the ELT performance, can be found in (Jimenez et al 2018;Lazkoz et al 2018).…”

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confidence: 99%

Forecasts of redshift drift constraints on cosmological parameters

Alves

Leite

Martins

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Cosmological observations usually map our present-day past light cone. However, it is also possible to compare different past light cones. This is the concept behind the redshift drift, a model-independent probe of fundamental cosmology. In simple physical terms, this effectively allows us to watch the Universe expand in real time. While current facilities only allow sensitivities several orders of magnitude worse than the expected signal, it should be possible to detect it with forthcoming ones. Here we discuss the potential impact of measurements by three such facilities: the Extremely Large Telescope (the subject of most existing redshift drift forecasts), but also the Square Kilometre Array and intensity mapping experiments. For each of these we assume the measurement sensitivities estimated respectively in Liske et al. (2008), Klockner et al. (2015 and Yu et al. (2014). We focus on the role of these measurements in constraining dark energy scenarios, highlighting the fact that although on their own they yield comparatively weak constraints, they do probe regions of parameter space that are typically different from those probed by other experiments, as well as being redshift-dependent. Specifically, we quantify how combinations of several redshift drift measurements at different redshifts, or combinations of redshift drift measurements with those from other canonical cosmological probes, can constrain some representative dark energy models. Our conclusion is that a model-independent mapping of the expansion of the universe from redshift z = 0 to z = 4-a challenging but feasible goal for the next generation of astrophysical facilities-can have a significant impact on fundamental cosmology.

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confidence: 99%

Forecasts of redshift drift constraints on cosmological parameters

Alves

Leite

Martins

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Since then, and particularly in recent years, a lot of work has been done to investigate the measurability of the redshift drift in cosmology and the information gained, see e.g. references [47][48][49][50][51].…”

Section: The λCdm Modelmentioning

confidence: 99%

BiGONLight: light propagation with bilocal operators in numerical relativity

Grasso

Villa

2021

Class. Quantum Grav.

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BiGONLight, Bilocal Geodesic Operators framework for Numerical Light propagation, is a new tool for light propagation in Numerical Relativity. The package implements the Bi-local Geodesic Operators formalism, a new framework for light propagation in General Relativity. With BiGONLight it is possible to extract observables such as angular diameter distance, luminosity distance, magnification as well as new real-time observables like parallax and redshift drift within the same computation. As a test-bed for our code we consider two exact cosmological models, the ΛCDM and the inhomogeneous Szekeres model, and a simulated dust universe. All our tests show an excellent agreement with known results.

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“…In terms of the constraints on the equation of state of dark energy, the expected constraints in the year 2040 do not seem impressive if compared to the present-day constraints [22]. However, one should keep in mind that these are the constraints from the drift effects alone, without combining them with other cosmological probes available in the year 2040 [23]. In addition, if the flux stability is better than ∆F ν /F ν ∼ 10 −4 , then the constraints improve significantly.…”

Section: Redshift Drift and Flux Driftmentioning

confidence: 99%

Direct detection of the cosmic expansion: the redshift drift and the flux drift

Bolejko,

Wang,

Lewis

2019

Preprint

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The redshift drift, the change of cosmological redshift with time, is a direct consequence of the expansion of the Universe. Thus the measurement of the cosmological redshift drift will offer a direct test of our models of cosmology. The magnitude of the effect is very small, i.e. the spectral shift is of order of 10 −10 − 10 −9 over the period of a decade, but the next generation facilities such as ELT and SKA will be able to directly detect the expansion of our Universe by the year 2040. In this paper we focus on detectebility of this effect, including strategies of overcoming the kinematic contamination of the cosmological signal. We also show that the redshift drift directly impacts the change of flux. Thus apart from the redshift drift, measurements of the flux drift will provide an additional tool of detecting the expansion of the universe, including its acceleration. We discuss the strategies of detecting the flux drift and show that by including the flux drift signal to the redshift drift signal we boost the chances of a direct detection of the expansion of the Universe. We show that if only the stability of flux is at the level of ∆F/F ∼ 10 −6 then the SKA1-mid Array should be able to detect these effects, before the ETL and the full SKA. Thus, by including the flux drift into the SKA1-mid Array's analysis pipeline, we could be able to provide by mid-2030s a direct evidence of the expansion of the universe including its accelerating phase.

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Forecast and analysis of the cosmological redshift drift

Cited by 13 publications

References 85 publications

Forecasts of redshift drift constraints on cosmological parameters

Forecasts of redshift drift constraints on cosmological parameters

BiGONLight: light propagation with bilocal operators in numerical relativity

Direct detection of the cosmic expansion: the redshift drift and the flux drift

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