Constraining the H i–Halo Mass Relation from Galaxy Clustering

Guo, Hong; Cheng, Li; Zheng, Zheng; Mo, H. J.; Jing, Y. P.; Zu, Ying; Lim, Sangsoo; Xu, Haojie

doi:10.3847/1538-4357/aa85e7

Cited by 72 publications

(93 citation statements)

References 150 publications

(246 reference statements)

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“…At z=1, we find that depending on the halo mass considered, H I-rich halos can be more or less clustered than H I-poor halos. We note that Guo et al (2017) found that the clustering of H I galaxies from the ALFALFA survey at z∼0 shows a bias systematically lower than mass-selected halos, in agreement with our results for H I-rich halos.…”

Section: Secondary H I Biassupporting

confidence: 92%

Ingredients for 21 cm Intensity Mapping

Villaescusa-Navarro

Genel

Castorina

et al. 2018

ApJ

206

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: Secondary H I Biassupporting

confidence: 92%

Ingredients for 21 cm Intensity Mapping

Villaescusa-Navarro

Genel

Castorina

et al. 2018

ApJ

206

309

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“…If the average MHI − Mstar becomes a non-monotonic function of stellar mass and therefore halo mass, HI abundance matching techniques, used to obtain MHI −M halo relation (Khandai, et al 2011;Padmanabhan & Kulkarni 2017), will break down. The HI HOD models which also assume a step-like function (with the help of the error function) (Guo, et al 2017;Paul, Choudhury & Paranjape 2018) for the average occupation of centrals, may need to be revised. A log normal form for the mean occupation function for centrals was compared to the step-like parameterization in the context of describing quasar clustering (Shen, et al 2013), but it was found that the HOD parameters were not well constrained.…”

Section: Discussionmentioning

confidence: 99%

The population of galaxies that contribute to the H i mass function

Dutta

Khandai

Dey

2020

Monthly Notices of the Royal Astronomical Society

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We look at the contribution of different galaxy populations to the atomic hydrogen (HI) mass function (HIMF) and the HI density parameter, Ω HI , in the local Universe. Our analysis is based on a sample of 7857 HI-selected galaxies selected from a volume common to the SDSS and ALFALFA surveys (40% catalogα.40). We define different populations of galaxies in the color(u-r )-magnitude(M r ) plane and compute the HIMF for each of them. Additionally we compute the HIMF for dark galaxies; these are undetected in SDSS and represent ∼ 2% of the total sample. We find that the bright red population dominates the total HIMF for log 10 (M HI h 2 70 /M ) ≥ 10.4. The full red population -bright and faint -represents about ∼ 17% of the Ω HI budget, while that of the dark population is ∼ 3%. The HIMF about the knee, log 10 (M HI h 2 70 /M ) ∈ [8, 10.4], is dominated by the faint and bright blue populations, the latter dominating at larger masses in this interval. Their total contribution to Ω HI is ∼ 55 − 70%, the variation depending on the definition of population. The dominant populations at the low mass end, log 10 (M HI h 2 70 /M ) ≤ 8.0 are the faint blue and faint bluer populations, the latter's dominance being sensitive to its definition. The full blue (blue-bluer bright and faint) population represents ∼ 80% of Ω HI . A bimodal HIMF suggested by our results is however not seen since the amplitude of the HIMF of the bright red population is small compared to that of the bright blue population.

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“…We measure wp for 144 times leaving out one different sub-region at each time, and the covariance is calculated as 143 times the variance of the 144 measurements (e.g. Zehavi et al 2005bZehavi et al , 2011Guo et al 2015;Xu et al 2016;Zu & Mandelbaum 2016;Guo et al 2017).…”

Section: Galaxy Clustering Measurementsmentioning

confidence: 99%

The conditional colour–magnitude distribution – I. A comprehensive model of the colour–magnitude–halo mass distribution of present-day galaxies

Zheng

Guo

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We formulate a model of the conditional colour-magnitude distribution (CCMD) to describe the distribution of galaxy luminosity and colour as a function of halo mass. It consists of two populations of different colour distributions, dubbed pseudo-blue and pseudo-red, respectively, with each further separated into central and satellite galaxies. We define a global parameterization of these four colour-magnitude distributions and their dependence on halo mass, and we infer parameter values by simultaneously fitting the space densities and autocorrelation functions of 79 galaxy samples from the Sloan Digital Sky Survey defined by fine bins in the colour-magnitude diagram (CMD). The model deprojects the overall galaxy CMD, revealing its tomography along the halo mass direction. The bimodality of the colour distribution is driven by central galaxies at most luminosities, though at low luminosities it is driven by the difference between blue centrals and red satellites. For central galaxies, the two pseudocolour components are distinct and orthogonal to each other in the CCMD: at fixed halo mass, pseudo-blue galaxies have a narrow luminosity range and broad colour range, while pseudored galaxies have a narrow colour range and broad luminosity range. For pseudo-blue centrals, luminosity correlates tightly with halo mass, while for pseudo-red galaxies colour correlates more tightly (redder galaxies in more massive haloes). The satellite fraction is higher for redder and for fainter galaxies, with colour a stronger indicator than luminosity. We discuss the implications of the results and further applications of the CCMD model.

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Constraining the H i–Halo Mass Relation from Galaxy Clustering

Cited by 72 publications

References 150 publications

Ingredients for 21 cm Intensity Mapping

Ingredients for 21 cm Intensity Mapping

The population of galaxies that contribute to the H i mass function

The conditional colour–magnitude distribution – I. A comprehensive model of the colour–magnitude–halo mass distribution of present-day galaxies

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