Cosmology on Ultralarge Scales with Intensity Mapping of the Neutral Hydrogen 21 cm Emission: Limits on Primordial Non-Gaussianity

Camera, Stefano; Santos, Mário G.; Ferreira, Pedro G.; Ferramacho, L.

doi:10.1103/physrevlett.111.171302

Cited by 104 publications

(97 citation statements)

References 46 publications

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“…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: 99%

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: Comparison With Theoretical Models and Implications For Intementioning

confidence: 99%

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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“…Therefore, in principle one can obtain a three-dimensional HI distribution that can provide more modes of fluctuation than the CMB two-dimensional sphere. There have been several works to forecast the detectability of PNG through the HI intensity mapping technique [31][32][33], but those forecasts are exclusively only for the local and equilateral type of PNG and limited experimental cases (SKA and Tianlai). In this work, we will calculate the scale-dependent bias of all four typical types of PNG by using the halo model and calculate their imprints on the power spectrum of HI .…”

Section: Introductionmentioning

confidence: 99%

Constraints on primordial non-Gaussianity from future Hi intensity mapping experiments

2017

Phys. Rev. D

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The primordial non-Gaussianity induces scale-dependent bias of the HI with respect to the underlying dark matter, which exhibits features on the very large scales of the 21-cm power spectrum potentially observable with HI intensity mapping observations. We forecast the prospective constraints on the four fundamental shapes of primordial non-Gaussianity (local, equilateral, orthogonal, and enfolded), with the current and future HI intensity mapping experiments, BINGO, FAST, and SKA-I. With the current configuration of the experiments and assumed one-year observation time, we find that the SKA-I will provide tighter constraints on the local shape of primoridal non-Gaussianity than Planck. The results are (σ f local NL

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“…It has been recently shown that the local and integrated relativistic contributions can become significant on very large scales [23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38]. Here we will investigate in detail the behaviour of the integrated terms for different cases, assuming a ΛCDM model.…”

Section: Introductionmentioning

confidence: 99%

“…The need to include geometrical and lightcone effects in the theoretical modeling has been long recognised (see the seminal works [16][17][18][19][20][21]). More recently, geometrical and relativistic effects have been intensively analyzed, as it becomes clear that future surveys will need very precise modeling [22][23][24][25][26][27][28][29][30][31][32][33][34][35][36][37][38].…”

Section: Introductionmentioning

confidence: 99%

Lensing and time-delay contributions to galaxy correlations

et al. 2016

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Galaxy clustering on very large scales can be probed via the 2-point correlation function in the general case of wide and deep separations, including all the lightcone and relativistic effects. Using our recently developed formalism, we analyze the behavior of the local and integrated contributions and how these depend on redshift range, linear and angular separations and luminosity function. Relativistic corrections to the local part of the correlation can be non-negligible but they remain generally sub-dominant. On the other hand, the additional correlations arising from lensing convergence and time-delay effects can become very important and even dominate the observed total correlation function. We investigate different configurations formed by the observer and the pair of galaxies, and we find that the case of near-radial large-scale separations is where these effects will be the most important.

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Cosmology on Ultralarge Scales with Intensity Mapping of the Neutral Hydrogen 21 cm Emission: Limits on Primordial Non-Gaussianity

Cited by 104 publications

References 46 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

Constraints on primordial non-Gaussianity from future Hi intensity mapping experiments

Lensing and time-delay contributions to galaxy correlations

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