Prospects of probing quintessence with H i 21-cm intensity mapping survey

Hussain, Azam; Thakur, Shruti; Sarkar, Tapomoy Guha; Sen, Anjan A.

doi:10.1093/mnras/stw2246

Cited by 11 publications

(15 citation statements)

References 85 publications

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“…Recent studies suggest that observations of 21-cm fluctuations on small scales, with SKA1, can constrain the sum of the neutrino masses (Villaescusa-Navarro et al 2015;Pal & Guha Sarkar 2016). Observations with SKA1-MID can also test different scalar field dark energy models (Hossain et al 2016). Ali & Bharadwaj (2014) and Bharadwaj et al (2015) present theoretical estimates for intensity mapping at z ∼ 3.35 with the Ooty Wide Field Array (OWFA), while Chatterjee et al (2016) and present similar estimates for the upcoming uGMRT and SKA2 respectively.…”

Section: Introductionmentioning

confidence: 80%

Modelling the post-reionization neutral hydrogen (H i ) bias

Sarkar

Bharadwaj

Anathpindika

2016

Mon. Not. R. Astron. Soc.

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Observations of the neutral Hydrogen (HI ) 21-cm signal hold the potential of allowing us to map out the cosmological large scale structures (LSS) across the entire postreionization era (z 6). Several experiments are planned to map the LSS over a large range of redshifts and angular scales, many of these targeting the Baryon Acoustic Oscillations. It is important to model the HI distribution in order to correctly predict the expected signal, and more so to correctly interpret the results after the signal is detected. In this paper we have carried out semi-numerical simulations to model the HI distribution and study the HI power spectrum P HI (k, z) across the redshift range 1 z 6. We have modelled the HI bias as a complex quantityb(k, z) whose modulus squared b 2 (k, z) relates P HI (k, z) to the matter power spectrum P (k, z), and whose real part b r (k, z) quantifies the cross-correlation between the HI and the matter distribution. We study the z and k dependence of the bias, and present polynomial fits which can be used to predict the bias across 0 z 6 and 0.01 k 10 Mpc −1 . We also present results for the stochasticity r = b r /b which is important for crosscorrelation studies.

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Section: Introductionmentioning

confidence: 80%

Modelling the post-reionization neutral hydrogen (H i ) bias

Sarkar

Bharadwaj

Anathpindika

2016

Mon. Not. R. Astron. Soc.

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“…The observable in 21 cm experiments is the excess brightness temperature. The power spectrum P 21 of this excess brightness temperature field is given by [36][37][38][39][40][41][42][43]…”

Section: Observed 21 CM Power Spectrummentioning

confidence: 99%

“…Forecasting the constraints on late time cosmology using 21cm intensity mapping experiments has been previously done by Bull et al [44] using ΛCDM and dark energy with CPL parametrization only. Prospects of probing quintessence 2D angular power spectra for intensity mapping has also been studied by Hussain et al [40]. The specifications for SKA configurations have been revised in recent past.…”

Section: Introductionmentioning

confidence: 99%

Dark energy constraints from the 21~cm intensity mapping surveys with SKA1

Dinda,

Sen,

Choudhury

2018

Preprint

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Understanding the nature of dark energy is one of the most outstanding problems in cosmology at present. In last twenty years, cosmological observations related to SNIa, Cosmic Microwave Background Radiation, Baryon Acoustic Oscillations etc, have put stringent constraints on the the dark energy evolution, still there is enough uncertainty in our knowledge about dark energy that demands new generation of cosmological observations. Post-reionization neutral hydrogen 21 cm intensity mapping surveys are one of the most promising future cosmological observations that have the potential to map the cosmological evolution from dark ages till present time with unprecedented accuracy and Square Kilometer Array (SKA) is one of the most sensitive instruments to measure the post-reionization 21 cm signal. In this work, we study the future dark energy constraints using postreionization 21 cm intensity mapping power spectra with SKA1-mid specifications. We use three different parametrizations for dark energy equation of state (EoS) including the widely used CPL one. To generate simulated data, we use to two fiducial models: the concordance ΛCDM and the best fit CPL model for Planck+SNIa+BAO+HST. Our study shows that SKA1-mid alone has the potential to reach the present accuracy for combined Planck+SNIa+BAO+HST to constrain the dark energy behaviour. Whether dark energy is phantom or non-phantom or whether it exhibits phantom crossing, we may potentially address such questions with SKA1-mid. We also show that it is crucial to choose the correct parametrization for dark energy equation of state as some parametrizations are better than others to constrain the dark energy behaviour. Specifically, as observed in this study, the widely used CPL parametrization may not give the best constraint for dark energy behaviour.

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“…We have assumed spatially flat cosmology in our entire analysis and not constrained radiation density, as only dark matter and dark energy are dominant in the late universe. The full relativistic treatment of perturbations for Quintessence dark energy has been studied Hussain et al (2016). Ignoring super-horizon effects, we note that on sub-horizon scales, ignoring the clustering of Quintessence field, the linearized equations governing the growth of matter fluctuations is given by the ODE (Amendola 2000(Amendola , 2004)…”

Section: Quintessence Cosmologymentioning

confidence: 99%

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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Prospects of probing quintessence with H i 21-cm intensity mapping survey

Cited by 11 publications

References 85 publications

Modelling the post-reionization neutral hydrogen (H i ) bias

Modelling the post-reionization neutral hydrogen (H i ) bias

Dark energy constraints from the 21~cm intensity mapping surveys with SKA1

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

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