LATE-TIME COSMOLOGY WITH 21 cm INTENSITY MAPPING EXPERIMENTS

Bull, Philip; Ferreira, Pedro G.; Patel, Prina; Santos, Mário G.

doi:10.1088/0004-637x/803/1/21

Cited by 366 publications

(448 citation statements)

References 96 publications

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“…It has been recently pointed out that using an instrument like the future SKA, the constraints on the cosmological parameters will be much tighter if the intensity mapping technique is employed (see Bull et al 2015). In order to extract the maximum information from these surveys, an exquisite knowledge of the spatial distribution of neutral hydrogen is needed from the theoretical side.…”

Section: Summary and Discussionmentioning

confidence: 99%

“…As discussed in the introduction, the shape and amplitude of the function MHI(M, z) is of primary importance for future surveys that aim at putting constraints on the cosmological parameters using intensity mapping. We now compare our findings with the theoretical model of Bagla et al (2010), which has been commonly used in the literature to perform forecasts (Camera et al 2013;Bull et al 2015;Villaescusa-Navarro et al 2014, 2015bCarucci et al 2015;Villaescusa-Navarro et al 2015a) and to create mock 21cm intensity mapping maps (Seehars et al 2015). Bagla et al (2010) proposed a functional form for the MHI(M, z) function as follows…”

Section: Comparison With Theoretical Models and Implications For Intementioning

confidence: 97%

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Neutral hydrogen in galaxy clusters: impact of AGN feedback and implications for intensity mapping

Villaescusa-Navarro¹,

Planelles²,

Borgani³

et al. 2016

Mon. Not. R. Astron. Soc.

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By means of zoom-in hydrodynamic simulations we quantify the amount of neutral hydrogen (HI) hosted by groups and clusters of galaxies. Our simulations, which are based on an improved formulation of smoothed particle hydrodynamics (SPH), include radiative cooling, star formation, metal enrichment and supernova feedback, and can be split in two different groups, depending on whether feedback from active galactic nuclei (AGN) is turned on or off. Simulations are analyzed to account for HI self-shielding and the presence of molecular hydrogen. We find that the mass in neutral hydrogen of dark matter halos monotonically increases with the halo mass and can be well described by a power-law of the form M HI (M, z) ∝ M 3/4 . Our results point out that AGN feedback reduces both the total halo mass and its HI mass, although it is more efficient in removing HI. We conclude that AGN feedback reduces the neutral hydrogen mass of a given halo by ∼ 50%, with a weak dependence on halo mass and redshift. The spatial distribution of neutral hydrogen within halos is also affected by AGN feedback, whose effect is to decrease the fraction of HI that resides in the halo inner regions. By extrapolating our results to halos not resolved in our simulations we derive astrophysical implications from the measurements of Ω HI (z): halos with circular velocities larger than ∼ 25 km/s are needed to host HI in order to reproduce observations. We find that only the model with AGN feedback is capable of reproducing the value of Ω HI b HI derived from available 21cm intensity mapping observations.

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Section: Summary and Discussionmentioning

confidence: 99%

Section: Comparison With Theoretical Models and Implications For Intementioning

confidence: 97%

Neutral hydrogen in galaxy clusters: impact of AGN feedback and implications for intensity mapping

Villaescusa-Navarro¹,

Planelles²,

Borgani³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The collective emission from the clouds, however form a diffuse background in all radio observations at observing frequencies less than 1420 MHz. Tomographic imaging using the low resolution intensity mapping of this diffuse background radiation is a potentially rich probe of cosmology (Bharadwaj & Sethi 2001;Chang et al 2008;Wyithe 2008;Bharadwaj et al 2009;Wyithe & Loeb 2009;Camera et al 2013;Bull et al 2015).…”

Section: Cross Correlation Signal and Estimation Of Neutrino Massmentioning

confidence: 99%

Constraining neutrino mass using the large-scale H i distribution in the post-reionization epoch

Pal¹,

Sarkar²

2016

Mon. Not. R. Astron. Soc.

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The neutral intergalactic medium in the post reionization epoch allows us to study cosmological structure formation through the observation of the redshifted 21 cm signal and the Lymanalpha forest. We investigate the possibility of measuring the total neutrino mass through the suppression of power in the matter power spectrum. We investigate the possibility of measuring the neutrino mass through its imprint on the cross-correlation power spectrum of the 21-cm signal and the Lyman-alpha forest. We consider a radio-interferometric measurement of the 21 cm signal with a SKA1-mid like radio telescope and a BOSS like Lyman-alpha forest survey. A Fisher matrix analysis shows that at the fiducial redshift z = 2.5, a 10,000 hrs 21-cm observation distributed equally over 25 radio pointings and a Lyman-alpha forest survey with 30 quasars lines of sights in 1deg 2 , allows us to measure Ω ν at a 3.25% level. A total of 25,000 hrs radio-interferometric observation distributed equally over 25 radio pointings and a Lyman-alpha survey withn = 60deg −2 will allow Ω ν to be measured at a 2.26% level. This corresponds to an idealized measurement of m ν at the precision of (100 ± 2.26)meV and f ν = Ω ν /Ω m at 2.49% level.

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“…The suitable choice of the w i takes care of the fact that the pixel noise for each of the QSO spectra are in principle different. We have, in Fourier space, 10) whereρ is the Fourier transform of ρ, ⊗ denotes a convolution and ∆ N F (k) denotes a noise term. We define the cross-correlation estimatorÊ aŝ…”

Section: Cross-correlation Power Spectrummentioning

confidence: 99%

On using large scale correlation of the Ly-α forest and redshifted 21-cm signal to probe HI distribution during the post reionization era

Sarkar

Datta

2015

J. Cosmol. Astropart. Phys.

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Abstract. We investigate the possibility of detecting the 3D cross correlation power spectrum of the Ly-α forest and HI 21 cm signal from the post reionization epoch. The crosscorrelation signal is directly dependent on the dark matter power spectrum and is sensitive to the 21-cm brightness temperature and Ly-α forest biases. These bias parameters dictate the strength of anisotropy in redshift space. We find that the cross-correlation power spectrum can be detected using 400 hrs observation with SKA-mid (phase 1) and a futuristic BOSS like experiment with a quasar (QSO) density of 30 deg −2 at a peak SNR of 15 for a single field experiment at redshift z = 2.5. We also study the possibility of constraining various bias parameters using the cross power spectrum. We find that with the same experiment 1σ conditional errors on the 21-cm linear redshift space distortion parameter β T and β F corresponding to the Ly-α forest are ∼ 2.7% and ∼ 1.4% respectively for 10 independent pointings of the SKA-mid (phase 1). This prediction indicates a significant improvement over existing measurements. We claim that the detection of the 3D cross correlation power spectrum will not only ascertain the cosmological origin of the signal in presence of astrophysical foregrounds but will also provide stringent constraints on large scale HI biases. This provides an independent probe towards understanding cosmological structure formation.

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LATE-TIME COSMOLOGY WITH 21 cm INTENSITY MAPPING EXPERIMENTS

Cited by 366 publications

References 96 publications

Neutral hydrogen in galaxy clusters: impact of AGN feedback and implications for intensity mapping

Neutral hydrogen in galaxy clusters: impact of AGN feedback and implications for intensity mapping

Constraining neutrino mass using the large-scale H i distribution in the post-reionization epoch

On using large scale correlation of the Ly-α forest and redshifted 21-cm signal to probe HI distribution during the post reionization era

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