The cross-correlation between 21 cm intensity mapping maps and the Lyα forest in the post-reionization era

Carucci, Isabella P.; Villaescusa-Navarro, Francisco; Viel, Matteo

doi:10.1088/1475-7516/2017/04/001

Cited by 32 publications

(30 citation statements)

References 81 publications

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“…Third, the amplitude of the signal depends only on the abundance and clustering of neutral hydrogen, and so cosmic H I can be traced from z=0 to z;50. 14 Current, upcoming, and future surveys such as the Giant Meterwave Radio Telescope (GMRT), 15 the Ooty Radio Telescope (ORT), 16 the Canadian Hydrogen Intensity Mapping Experiment (CHIME), 17 the Five-hundred-meter Aperture Spherical Telescope (FAST), 18 Tianlai, 19 BINGO (Baryon acoustic oscillations In Neutral Gas Observations), 20 ASKAP (The Australian Square Kilometer Array Pathfinder), 21 Meer-KAT (The South African Square Kilometer Array Pathfinder), 22 HIRAX (The Hydrogen Intensity and Real-time Analysis eXperiment), 23 and the SKA (The Square Kilometer Array) 24 will sample the large-scale structure of the universe in the post-reionization era by detecting 21 cm emission from cosmic neutral hydrogen (Choudhuri et al 2016;Carucci et al 2017b;Marthi et al 2017;Sarkar et al 2018aSarkar et al , 2018bSarkar et al , 2016b.…”

Section: Introductionmentioning

confidence: 99%

Ingredients for 21 cm Intensity Mapping

Villaescusa-Navarro

Genel

Castorina

et al. 2018

ApJ

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215

309

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Current and upcoming radio telescopes will map the spatial distribution of cosmic neutral hydrogen (H I) through its 21 cm emission. In order to extract the maximum information from these surveys, accurate theoretical predictions are needed. We study the abundance and clustering properties of H I at redshifts z5 using TNG100, a large state-of-the-art magnetohydrodynamic simulation of a 75h −1 Mpc box size, which is part of the IllustrisTNG Project. We show that most of the H I lies within dark matter halos, and we provide fits for the halo H I mass function, i.e.,the mean H I mass hosted by a halo of mass M at redshift z. We find that only halos with circular velocities larger than ;30km s −1 contain H I. While the density profiles of H I exhibit a large halo-to-halo scatter, the mean profiles are universal across mass and redshift. The H I in low-mass halos is mostly located in the central galaxy, while in massive halos the H I is concentrated in the satellites. Our simulation reproduces the bias value of damped Lyα systems from observations. We show that the H I and matter density probability distribution functions differ significantly. Our results point out that for small halos, the H I bulk velocity goes in the same direction and has the same magnitude as the halo peculiar velocity, while in large halos, differences show up. We find that halo H I velocity dispersion follows a power law with halo mass. We find a complicated H I bias, with H I already becoming nonlinear at k=0.3 h Mpc −1 at z3. The clustering of H I can, however, be accurately reproduced by perturbative methods. We find a new secondary bias by showing that the clustering of halos depends not only on mass but also on H I content. We compute the amplitude of the H I shot noise and find that it is small at all redshifts, verifying the robustness of BAO measurements with 21 cm intensity mapping. We study the clustering of H I in redshift space and show that linear theory can explain the ratio between the monopoles in redshift and real space down to 0.3, 0.5, and 1 h Mpc −1 at redshifts 3, 4, and 5, respectively. We find that the amplitude of the Fingers-of-God effect is larger for H I than for matter, since H I is found only in halos above a certain mass. We point out that 21 cm maps can be created from N-body simulations rather than full hydrodynamic simulations. Modeling the one-halo term is crucial for achieving percent accuracy with respect to a full hydrodynamic treatment. Although our results are not converged against resolution, they are, however, very useful as we work at the resolution where the model parameters have been calibrated to reproduce galaxy properties.

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Section: Introductionmentioning

confidence: 99%

Ingredients for 21 cm Intensity Mapping

Villaescusa-Navarro

Genel

Castorina

et al. 2018

ApJ

Self Cite

215

309

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“…By making use of the large-scale clustering present in the maps and the galaxy distribution, cross-correlation can extract information beyond what is derived from stacking spectra extracted at known galaxy positions. Cross-correlations between intensity maps and a broad range of other data sets have been explored as a tool for addressing numerous astrophysical and cosmological problems, including calibration of photometric redshifts (Cunnington et al 2019), characterizing feedback from active galactic nucleii (Breysse & Alexandroff 2019), determining physical properties of the interstellar medium (ISM; Sun et al 2019), exploring the Lyα forest (Carucci et al 2017), measuring baryon acoustic oscillations at high redshift (Cohn et al 2016), mitigating the effects of cosmic variance (Oxholm & Switzer 2021), and constraining models of primordial non-Gaussianity (Moradinezhad Dizgah & Keating 2019), among others.…”

Section: Introductionmentioning

confidence: 99%

An Intensity Mapping Constraint on the CO-Galaxy Cross Power Spectrum at Redshift ~ 3

Keenan,

Keating,

Marrone

2021

Preprint

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The abundance of cold molecular gas plays a crucial role in models of galaxy evolution. While deep spectroscopic surveys of CO emission lines have been a primary tool for measuring this abundance, the difficulty of these observations has motivated alternative approaches to studying molecular gas content. One technique, line intensity mapping, seeks to constrain the average molecular gas properties of large samples of individually undetectable galaxies through the CO brightness power spectrum.Here we present constraints on the cross-power spectrum between CO intensity maps and optical galaxy catalogs. This cross-measurement allows us to check for systematic problems in CO intensity mapping data, and validate the data analysis used the auto-power spectrum measurement of the CO Power Spectrum Survey. We place a 2σ upper limit on the band-averaged CO-galaxy cross-power of P × < 540 µK h −3 Mpc 3 . Our measurement favors a non-zero T CO at around 90% confidence and gives an upper limit on the mean molecular gas density at z ∼ 2.6 of 7.7 × 10 8 M Mpc −3 . We forecast the expected cross-power spectrum by applying a number of literature prescriptions for the CO luminosity to halo mass relation to a suite of mock light cones. Under the most optimistic forecasts the cross-spectrum could be detected with only moderate extensions of the data used here, while more conservative models could be detected with a factor of 10 increase in sensitivity. Ongoing CO intensity mapping experiments will target fields allowing extensive cross correlation analysis and should reach the sensitivity required to detect the cross-spectrum signal.

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“…estimated that observation of H I power spectrum at a redshift of z = 3.35 is possible for an angular scale of 11 ′ to 3 • with a three-sigma significance for an observation time of 1000 hours and bandwidth of 30 MHz with the ORT (henceforth ORT 2 ), Phase II. Guha Sarkar et al (2011); Carucci et al (2017) used the cross-correlation between 21-cm intensity mapping and Lyα forest in order to constraints the H I content in the galaxies in the post reionization universe.…”

Section: Introductionmentioning

confidence: 99%

Combined lensed estimator to probe the post reionization H I power spectrum

Arora,

Dutta

2021

Preprint

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In the post-reionization era, the baryons assembled into the protogalaxies and eventually the present population of the galaxies evolved through merger and evolution. In this work, we discuss a possible probe of the statistical distribution and evolution of the H I density in the post reionization era. We introduce an estimator of the H I power spectrum from the post reionization universe by observing it through the strong gravitational lenses by the nearby galaxy cluster. We also analytically calculate the uncertainties associated with the estimates of the post-EoR power spectrum for the discussed estimator. We access the efficacy of this estimator in the context of 19 galaxy clusters for which the lensing potential has been estimated earlier by various authors. We find that by combining the lensed power spectrum through eight of these cluster lenses, it is possible to estimate the post-reionization H I power spectrum at five-sigma significance for angular multipoles < 4000 for a uGMRT observation of 16 MHz bandwidth from redshifts of 1.25, 1.5 with a total of 400 hours of observation. With the same setup, for a redshift of 3.0, we need 200 hours of total observation time. The estimator also suppresses the diffused galactic foreground, though, the latter is still a dominant contributor to the overall signal and hence need to be estimated and mitigated. We discuss the merits and demerits of the estimator.

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The cross-correlation between 21 cm intensity mapping maps and the Lyα forest in the post-reionization era

Cited by 32 publications

References 81 publications

Ingredients for 21 cm Intensity Mapping

Ingredients for 21 cm Intensity Mapping

An Intensity Mapping Constraint on the CO-Galaxy Cross Power Spectrum at Redshift ~ 3

Combined lensed estimator to probe the post reionization H I power spectrum

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