Constraining dark energy using the cross correlations of weak lensing with post-reionization probes of neutral hydrogen

Dash, Chandrachud B. V.; Sarkar, Tapomoy Guha

doi:10.1088/1475-7516/2021/02/016

Cited by 9 publications

(7 citation statements)

References 127 publications

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“…Specific studied models are f (R) [218,219], generalised scalar-tensor theories [496], early DE [497,498], interacting DE [499,500], among others [408,501]. Recently, several studies have focused on the cross-correlation between IM and other LSS probes, such as WL, GWs, and galaxy clustering [502][503][504][505]. The constraining power on DE of other lines is still mostly uncharted [506].…”

Section: Radio Surveys: Continuum and Intensity Mappingmentioning

confidence: 99%

Cosmological Probes of Structure Growth and Tests of Gravity

et al. 2023

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The current standard cosmological model is constructed within the framework of general relativity with a cosmological constant Λ, which is often associated with dark energy, and phenomenologically explains the accelerated cosmic expansion. Understanding the nature of dark energy is one of the most appealing questions in achieving a self-consistent physical model at cosmological scales. Modification of general relativity could potentially provide a more natural and physical solution to the accelerated expansion. The growth of the cosmic structure is sensitive in constraining gravity models. In this paper, we aim to provide a concise introductory review of modified gravity models from an observational point of view. We will discuss various mainstream cosmological observables, and their potential advantages and limitations as probes of gravity models.

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Section: Radio Surveys: Continuum and Intensity Mappingmentioning

confidence: 99%

Cosmological Probes of Structure Growth and Tests of Gravity

et al. 2023

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“…The post reionization HI signal has been studied extensively Wyithe & Loeb 2007;Loeb & Wyithe 2008;Visbal et al 2009;Bharadwaj & Pandey 2003;Padmanabhan et al 2015;Bharadwaj & Srikant 2004). We follow the general formalism for the cross-correlation of the 21-cm signal with other cosmological fields given in (Dash & Guha Sarkar (2021)). Usually for the investigations involving the 21-cm signal the the radial information is retained for tomographic study.…”

Section: The Cross-correlation Signalmentioning

confidence: 99%

“…where C κ and C T are the convergence and 21-cm auto-correlation angular power spectra respectively and N κ and N T are the corresponding noise power spectra. The auto-correlation power spectra are given by (Dash & Guha Sarkar (2021))…”

Section: The Baryon Acoustic Oscillation In the Angular Power Spectrummentioning

confidence: 99%

“…Further, the foregrounds and contaminants of individual surveys are, in most cases, uncorrelated and hence do not bias the cross-correlation signal (Sarkar 2010;Vallinotto et al 2009). The cross-correlation of the post-reionization HI 21 cm signal has been extensively studied (Sarkar et al 2009;Guha Sarkar et al 2010;Sarkar 2010;Sarkar et al 2019;Dash & Guha Sarkar 2021).…”

Section: Introductionmentioning

confidence: 99%

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Probing Quintessence using BAO imprint on the cross-correlation of weak lensing and post-reionization HI 21 cm signal

Dash¹,

Sarkar²

2022

Preprint

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In this work we investigate the possibility of constraining a thawing Quintessence scalar field model for dark energy. We propose using the imprint of baryon acoustic oscillation (BAO) on the cross-correlation of post-reionization 21-cm signal and galaxy weak lensing convergence field to tomographically measure the angular diameter distance D A (z) and the Hubble parameter H(z). The projected errors in these quantities are then used to constrain the Quintessence model parameters. We find that independent 600hrs radio interferometric observation at four observing frequencies 916MHz, 650 MHz, 520 MHz and 430MHz with a SKA-1-Mid like radio telescope in cross-correlation with a deep weak lensing survey covering half the sky may measure the binned D A and H at a few percent level of sensitivity. The Monte Carlo analysis for a power law thawing Quientessence model gives the 1 − σ marginalized bounds on the initial slope λ i , dark energy density parameter Ω φ0 and the shape of the potential Γ at 8.63%, 10.08% and 9.75% respectively. The constraints improve to 7.66%, 4.39% and 5.86% respectively when a joint analysis with SN and other probes is performed.

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“…In addition to P3D, large volumes enable cross-correlating Lyα and other tracers of matter fluctuations. Because the forest power spectrum is sensitive to the small-scale matter fluctuation, whereas CMB lensing convergence measures the total matter fluctuation along the line of sight, combining the two (Vallinotto et al 2009(Vallinotto et al , 2011Chiang & Slosar 2018;Dash & Guha Sarkar 2021) allows us to probe the nonlinear structure formation at large scales in a redshift range still poorly tested. Correlating galaxy positions and their Lyα environments is another promising research avenue (Font-Ribera et al 2013;Bielby et al 2017;Mukae et al 2017;Momose et al 2021bMomose et al , 2021a for tracing matter fluctuations, as galaxy formation occurs in preferentially more dense environments, while the forest mostly comes from less dense regions.…”

Section: Introductionmentioning

confidence: 99%

Reconstructing Lyα Fields from Low-resolution Hydrodynamical Simulations with Deep Learning

Jacobus,

Harrington,

Lukić

2023

ApJ

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Hydrodynamical cosmological simulations are a powerful tool for accurately predicting the properties of the intergalactic medium (IGM) and for producing mock skies that can be compared against observational data. However, the need to resolve density fluctuation in the IGM puts a stringent requirement on the resolution of such simulations, which in turn limits the volumes that can be modeled, even on the most powerful supercomputers. In this work, we present a novel modeling method that combines physics-driven simulations with data-driven generative neural networks to produce outputs that are qualitatively and statistically close to the outputs of hydrodynamical simulations employing eight times higher resolution. We show that the Lyα flux field, as well as the underlying hydrodynamic fields, have greatly improved statistical fidelity over a low-resolution simulation. Importantly, the design of our neural network allows for sampling multiple realizations from a given input, enabling us to quantify the model uncertainty. Using test data, we demonstrate that this model uncertainty correlates well with the true error of the Lyα flux prediction. Ultimately, our approach allows for training on small simulation volumes and applying it to much larger ones, opening the door to producing accurate Lyα mock skies in volumes of Hubble size, as will be probed with DESI and future spectroscopic sky surveys.

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Constraining dark energy using the cross correlations of weak lensing with post-reionization probes of neutral hydrogen

Cited by 9 publications

References 127 publications

Cosmological Probes of Structure Growth and Tests of Gravity

Cosmological Probes of Structure Growth and Tests of Gravity

Probing Quintessence using BAO imprint on the cross-correlation of weak lensing and post-reionization HI 21 cm signal

Reconstructing Lyα Fields from Low-resolution Hydrodynamical Simulations with Deep Learning

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