scholarly journals The neutral hydrogen distribution in large-scale haloes from 21-cm intensity maps

2020 ◽  
Vol 498 (4) ◽  
pp. 5916-5935
Author(s):  
Denis Tramonte ◽  
Yin-Zhe Ma
Keyword(s):  
Large Scale ◽  
Neutral Hydrogen ◽  
Principal Component ◽  
Theoretical Models ◽  
Mapping Data ◽  
Hydrogen Distribution ◽  
Intensity Mapping ◽  
Concentration Parameter ◽  
Functional Forms ◽  
First Time

ABSTRACT We detect the neutral hydrogen (H i) radial brightness temperature profile in large-scale haloes by stacking 48 430 galaxies selected from the 2dFGRS catalogue on to a set of 21-cm intensity maps obtained with the Parkes radio telescope, spanning a total area of ∼1300 deg2 on the sky and covering the redshift range 0.06 ≲ z ≲ 0.10. Maps are obtained by removing both 10 and 20 foreground modes in the principal component analysis. We perform the stack at the map level and extract the profile from a circularly symmetrized version of the halo emission. We detect the H i halo emission with the significance 12.5σ for the 10-mode and 13.5σ for the 20-mode removed maps at the profile peak. We jointly fit for the observed halo mass Mv and the normalization $c_{0,\rm H\, \small{I}}$ for the H i concentration parameter against the reconstructed profiles, using functional forms for the H i halo abundance proposed in the literature. We find $\log _{10}{(M_{\rm v}/\text{M}_{\odot })}= 16.1^{+0.1}_{-0.2}$, $c_{0,\rm H\, \small{I}}=3.5^{+0.7}_{-1.0}$ for the 10-mode and $\log _{10}{(M_{\rm v}/\text{M}_{\odot })}= 16.5^{+0.1}_{-0.2}$, $c_{0,\rm H\, \small{I}}=5.3^{+1.1}_{-1.7}$ for the 20-mode removed maps. These estimates show the detection of the integrated contribution from multiple galaxies located inside very massive haloes. We also consider subsamples of 13 979 central and 34 361 satellite 2dF galaxies separately, and obtain marginal differences suggesting satellite galaxies are H i-richer. This work shows for the first time the feasibility of testing theoretical models for the H i halo content directly on profiles extracted from 21-cm maps and opens future possibilities for exploiting upcoming H i intensity-mapping data.

scholarly journals Searching for H i imprints in cosmic web filaments with 21-cm intensity mapping

2019 ◽  
Vol 489 (1) ◽  
pp. 385-400 ◽  
Author(s):  
Denis Tramonte ◽  
Yin-Zhe Ma ◽  
Yi-Chao Li ◽  
Lister Staveley-Smith
Keyword(s):  
Principal Component Analysis ◽  
Confidence Level ◽  
Column Density ◽  
Neutral Hydrogen ◽  
Principal Component ◽  
Density Parameter ◽  
Common Reference ◽  
Intensity Mapping ◽  
Upper Limits ◽  
First Time

ABSTRACT We investigate the possible presence of neutral hydrogen (H i) in intergalactic filaments at very low redshift (z ∼ 0.08), by stacking a set of 274 712 2dFGRS galaxy pairs over 21-cm maps obtained with dedicated observations conducted with the Parkes radio telescope, over a total sky area of approximately 1300 deg2 covering two patches in the northern and in the southern Galactic hemispheres. The stacking is performed by combining local maps in which each pair is brought to a common reference frame; the resulting signal from the edge galaxies is then removed to extract the filament residual emission. We repeat the analysis on maps cleaned removing either 10 or 20 foreground modes in a principal component analysis. Our study does not reveal any clear H i excess in the considered filaments in either case; we determine upper limits on the total filament H i brightness temperature at $T_{\rm b} \lesssim 10.3 \, \mu \text{K}$ for the 10-mode and at $T_{\rm b} \lesssim 4.8 \, \mu \text{K}$ for the 20-mode removed maps at the 95 per cent confidence level. These estimates translate into upper limits for the local filament H i density parameter, $\Omega _{\rm HI}^{\rm (f)} \lesssim 7.0\times 10^{-5}$ and $\Omega _{\rm HI}^{\rm (f)} \lesssim 3.2\times 10^{-5}$, respectively, and for the H i column density, $N_{\rm HI} \lesssim 4.6\times 10^{15}\, \text{cm}^{-2}$ and $N_{\rm HI} \lesssim 2.1\times 10^{15}\, \text{cm}^{-2}$, respectively. These column density constraints are consistent with previous detections of H i in the warm-hot intergalactic medium obtained observing broad Ly α absorption systems. This work shows for the first time how such constraints can be achieved using the stacking of galaxy pairs on 21-cm maps.

scholarly journals Modeling the neutral hydrogen distribution in the post-reionization Universe: intensity mapping

2014 ◽  
Vol 2014 (09) ◽  
pp. 050-050 ◽  
Author(s):  
Francisco Villaescusa-Navarro ◽  
Matteo Viel ◽  
Kanan K. Datta ◽  
T. Roy Choudhury
Keyword(s):  
Neutral Hydrogen ◽  
Hydrogen Distribution ◽  
Intensity Mapping

scholarly journals Beyond ΛCDM with H i intensity mapping: robustness of cosmological constraints in the presence of astrophysics

2020 ◽  
Vol 496 (4) ◽  
pp. 4115-4126 ◽  
Author(s):  
Stefano Camera ◽  
Hamsa Padmanabhan
Keyword(s):  
Dark Matter ◽  
Modified Gravity ◽  
Cosmological Parameters ◽  
Neutral Hydrogen ◽  
Temperature Fluctuations ◽  
Dark Matter Halo ◽  
Cosmological Constraints ◽  
Intensity Mapping ◽  
Standard Cosmological Model ◽  
First Time

ABSTRACT Mapping the unresolved intensity of the 21-cm emission of neutral hydrogen (H i) is now regarded as one the most promising tools for cosmological investigation in the coming decades. Here, we investigate, for the first time, extensions of the standard cosmological model, such as modified gravity and primordial non-Gaussianity, taking self-consistently into account. The present constraints on the astrophysics of H i clustering in the treatment of the brightness temperature fluctuations. To understand the boundaries within which results thus obtained can be considered reliable, we examine the robustness of cosmological parameter estimation performed via studies of 21-cm intensity mapping, against our knowledge of the astrophysical processes leading to H i clustering. Modelling of astrophysical effects affects cosmological observables through the relation linking the overall H i mass in a bound object, to the mass of the underlying dark matter halo that hosts it. We quantify the biases in estimates of standard cosmological parameters and those describing modified gravity and primordial non-Gaussianity that are obtained if one misconceives the slope of the relation between H i mass and halo mass, or the lower virial velocity cut-off for a dark matter halo to be able to host H i. Remarkably, we find that astrophysical uncertainties will not affect searches for primordial non-Gaussianity – one of the strongest science cases for H i intensity mapping – despite the signal being deeply linked to the H i bias.

The Galactic Distribution and Kinematics of OH Stars (A Preliminary Discussion)

1975 ◽  
Vol 2 (6) ◽  
pp. 362-363
Author(s):  
P.F. Bowers
Keyword(s):  
Large Scale ◽  
Velocity Dispersion ◽  
Neutral Hydrogen ◽  
Late Type ◽  
Velocity Range ◽  
Hydrogen Distribution ◽  
Mira Variables ◽  
Sky Survey ◽  
Ir Stars ◽  
Galactic Distribution

The majority of OH/IR stars have been identified as M-type Mira variables, but there are a few cases where the stars have been identified as M supergiants or late-type semi-regular variables. A large number of OH sources have also been discovered with the 1612 MHz OH characteristics of OH/IR stars but no apparent optical or infrared counterparts. In several cases the velocities of these unidentified sources (OH stars) have been outside the velocity range of the neutral hydrogen distribution, suggesting that some of these sources may represent a population with a higher velocity dispersion than Population I objects (Kerr and Bowers 1974a, b). The lack of infrared and optical counterparts may indicate that the sources are quite distant, since identified OH/IR stars are often bright infrared objects. A large-scale 1612 MHz sky survey has therefore been initiated to study the galactic distribution and kinematics of the OH stars and to investigate the possibility that they may represent an older population of stars (Bowers et al. 1974).

scholarly journals Neutral hydrogen in the post-reionization universe

2017 ◽  
Vol 12 (S333) ◽  
pp. 216-221
Author(s):  
Hamsa Padmanabhan
Keyword(s):  
Galaxy Evolution ◽  
Large Scale ◽  
Neutral Hydrogen ◽  
Lyman Alpha ◽  
Intensity Mapping ◽  
Best Fitting ◽  
Hydrodynamical Simulations ◽  
Intermediate Redshift ◽  
Intermediate Redshifts ◽  
The Universe

AbstractThe evolution of neutral hydrogen (HI) across redshifts is a powerful probe of cosmology, large scale structure in the universe and the intergalactic medium. Using a data-driven halo model to describe the distribution of HI in the post-reionization universe (z ∼ 5 to 0), we obtain the best-fitting parameters from a rich sample of observational data: low redshift 21-cm emission line studies, intermediate redshift intensity mapping experiments, and higher redshift Damped Lyman Alpha (DLA) observations. Our model describes the abundance and clustering of neutral hydrogen across redshifts 0 - 5, and is useful for investigating different aspects of galaxy evolution and for comparison with hydrodynamical simulations. The framework can be applied for forecasting future observations with neutral hydrogen, and extended to the case of intensity mapping with molecular and other line transitions at intermediate redshifts.

scholarly journals HIR4: cosmology from a simulated neutral hydrogen full sky using Horizon Run 4

2020 ◽  
Vol 495 (2) ◽  
pp. 1788-1806
Author(s):  
Jacobo Asorey ◽  
David Parkinson ◽  
Feng Shi ◽  
Yong-Seon Song ◽  
Kyungjin Ahn ◽  
...  
Keyword(s):  
Large Scale ◽  
Cosmological Parameters ◽  
Line Emission ◽  
Neutral Hydrogen ◽  
Angular Power Spectrum ◽  
Intensity Mapping ◽  
Free Case ◽  
Foreground Removal ◽  
The Universe ◽  
Mapping Information

ABSTRACT The distribution of cosmological neutral hydrogen will provide a new window into the large-scale structure of the Universe with the next generation of radio telescopes and surveys. The observation of this material, through 21 cm line emission, will be confused by foreground emission in the same frequencies. Even after these foregrounds are removed, the reconstructed map may not exactly match the original cosmological signal, which will introduce systematic errors and offset into the measured correlations. In this paper, we simulate future surveys of neutral hydrogen using the Horizon Run 4 (HR4) cosmological N-body simulation. We generate H i intensity maps from the HR4 halo catalogue, and combine with foreground radio emission maps from the Global Sky Model, to create accurate simulations over the entire sky. We simulate the H i sky for the frequency range 700–800 MHz, matching the sensitivity of the Tianlai pathfinder. We test the accuracy of the fastICA, PCA, and log-polynomial fitting foreground removal methods to recover the input cosmological angular power spectrum and measure the parameters. We show the effect of survey noise levels and beam sizes on the recovered the cosmological constraints. We find that while the reconstruction removes power from the cosmological 21 cm distribution on large scales, we can correct for this and recover the input parameters in the noise-free case. However, the effect of noise and beam size of the Tianlai pathfinder prevents accurate recovery of the cosmological parameters when using only intensity mapping information.

scholarly journals Measuring ultralarge scale effects in the presence of 21 cm intensity mapping foregrounds

2021 ◽  
Vol 504 (1) ◽  
pp. 267-279
Author(s):  
José Fonseca ◽  
Michele Liguori
Keyword(s):  
High Precision ◽  
Large Scale ◽  
Scale Effects ◽  
Cosmological Parameters ◽  
Neutral Hydrogen ◽  
Joint Analysis ◽  
Forward Modelling ◽  
Intensity Mapping ◽  
Best Fitting ◽  
The Universe

ABSTRACT H i intensity mapping will provide maps of the large-scale distribution of neutral hydrogen (H i) in the universe. These are prime candidates to be used to constrain primordial non-Gaussianity using the large-scale structure of the Universe as well as to provide further tests of Einstein’s theory of Gravity (GR). But H i maps are contaminated by foregrounds, which can be several orders of magnitude above the cosmological signal. Here we quantify how degenerated are the large-scale effects (fNL and GR effects) with the residual foregrounds. We conclude that a joint analysis does not provide a catastrophic degradation of constraints and provides a framework to determine the marginal errors of large scale-effects in the presence of foregrounds. Similarly, we conclude that the macroscopical properties of the foregrounds can be measured with high precision. Notwithstanding, such results are highly dependent on accurate forward modelling of the foregrounds, which incorrectly done catastrophically bias the best-fitting values of cosmological parameters, foreground parametrizations, and large-scale effects.

Accelerating Parameterizaton of Large-Scale Dynamic Models Through the Use of Activity Analysis

2006 ◽  
Author(s):  
Bryon J. Sohns ◽  
James Allison ◽  
Hosam Fathy ◽  
Jeffrey L. Stein
Keyword(s):  
Physical Meaning ◽  
Large Scale ◽  
Dynamic Models ◽  
Principal Component ◽  
Activity Analysis ◽  
Reduction Technique ◽  
Space Reduction ◽  
Numerical Studies ◽  
Model Reduction Technique ◽  
First Time

Previous research presents both sensitivity-based and principal component-based techniques for improving the tractability of system identification. Both have proven viable, but the former may be computationally inefficient for large problems, and the latter require a change of realization that may compromise the physical meaning of the parameters to be identified. This paper proposes for the first time the use of activity analysis, an efficient and realization-preserving model reduction technique, for identification space reduction. Theoretical and numerical studies highlighting the viability of activity analysis versus the previous two methods are presented.

scholarly journals Constraints on the End of Reionization from the Density Fields Surrounding Two Highly Opaque Quasar Sightlines

2021 ◽  
Vol 923 (1) ◽  
pp. 87
Author(s):  
Holly M. Christenson ◽  
George D. Becker ◽  
Steven R. Furlanetto ◽  
Frederick B. Davies ◽  
Matthew A. Malkan ◽  
...  
Keyword(s):  
Large Scale ◽  
Intergalactic Medium ◽  
Neutral Hydrogen ◽  
Large Fluctuations ◽  
First Time ◽  
The Relationship

Abstract The observed large-scale scatter in Lyα opacity of the intergalactic medium at z < 6 implies large fluctuations in the neutral hydrogen fraction that are unexpected long after reionization has ended. A number of models have emerged to explain these fluctuations that make testable predictions for the relationship between Lyα opacity and density. We present selections of z = 5.7 Lyα-emitting galaxies (LAEs) in the fields surrounding two highly opaque quasar sightlines with long Lyα troughs. The fields lie toward the z = 6.0 quasar ULAS J0148+0600, for which we reanalyze previously published results using improved photometric selection, and toward the z = 6.15 quasar SDSS J1250+3130, for which results are presented here for the first time. In both fields, we report a deficit of LAEs within 20 h −1 Mpc of the quasar. The association of highly opaque sightlines with galaxy underdensities in these two fields is consistent with models in which the scatter in Lyα opacity is driven by large-scale fluctuations in the ionizing UV background or by an ultra-late reionization that has not yet concluded at z = 5.7.

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