Constraints on the evolution of the relationship between HI mass and halo mass in the last 12 Gyr

Abstract

The neutral hydrogen (HI) content of dark matter haloes forms an intermediate state in the baryon cycle that connects the hot shock-heated gas and cold star-forming gas in haloes. Measurement of the relationship between HI mass and halo mass therefore puts important constraints on galaxy formation models. We combine radio observations of HI in emission at low redshift ($z\sim 0$) with optical/UV observations of HI in absorption at high redshift ($1<z<4$) to derive constraints on the evolution of the HI-mass halo-mass (HIHM) relation from redshift $z=4$ to $z=0$. We find that one can model the HIHM relation similar to the stellar-mass halo-mass (SHM) relation at $z\sim 0$. At $z=0$, haloes with mass $10^{11.7}$ M${}_{\odot }$ have the highest HI mass fraction ($\sim 1\%$), which is about four times smaller than their stellar mass fraction. We model the evolution of the HIHM relation in a manner similar to that of the SHM relation. Combining this parameterisation with a redshift- and mass-dependent modified Navarro-Frenk-White (NFW) profile for the HI density within a halo, we draw constraints on the evolution of the HIHM relation from the observed HI column density, incidence rate, and clustering bias at high redshift. We compare these findings with results from hydrodynamical simulations and other approaches in the literature, and find the models to be consistent with each other at the $68\%$ confidence level.

11 pages, 8 figures, 1 table; published in MNRAS. v3: minor typo corrected; results unchanged

References in corpus (23)

• The EAGLE project: Simulating the evolution and assembly of galaxies and their environments
• The EAGLE simulations of galaxy formation: calibration of subgrid physics and model variations
• The stellar mass assembly of galaxies from z=0 to z=4. Analysis of a sample selected in the rest-frame near-infrared with Spitzer
• COLD GASS, an IRAM legacy survey of molecular gas in massive galaxies: I. Relations between H2, HI, stellar content and structural properties
• COLD GASS, an IRAM Legacy Survey of Molecular Gas in Massive Galaxies: II. The non-universality of the Molecular Gas Depletion Timescale
• Measurement of 21 cm brightness fluctuations at z ~ 0.8 in cross-correlation
• On the (Non)Evolution of HI Disks over Cosmic Time
• Damped Lyman Alpha Systems in Galaxy Formation Simulations
• Canadian Hydrogen Intensity Mapping Experiment (CHIME) Pathfinder
• On the galaxy stellar mass function, the mass-metallicity relation, and the implied baryonic mass function
• The HI content of star-forming galaxies at z = 0.24
• The EAGLE simulations: atomic hydrogen associated with galaxies
• The Atomic to Molecular Transition and its Relation to the Scaling Properties of Galaxy Disks in the Local Universe
• Damped Lyman-alpha absorbers as a probe of stellar feedback
• The Rise of the First Stars: Supersonic Streaming, Radiative Feedback, and 21-cm Cosmology
• Reproducing the Kinematics of Damped Lyman-alpha Systems
• Evolution of the atomic and molecular gas content of galaxies in dark matter haloes
• The origin of the atomic and molecular gas contents of early-type galaxies. I. A new test of galaxy formation physics
• Theoretical and observational constraints on the HI intensity power spectrum
• Constraining a halo model for cosmological neutral hydrogen
• Modelling the post-reionization neutral Hydrogen (\HI) bias
• A consistent model for both the HI and stellar mass functions of galaxies
• Galactic outflows and the kinematics of damped Lyman alpha absorbers

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• Constraining the evolution of CII intensity through the end stages of reionization
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• Impact of Foregrounds on HI Intensity Mapping Cross-Correlations with Optical Surveys
• Strategies to Detect Dark-Matter Decays with Line-Intensity Mapping
• The physical drivers of the atomic hydrogen-halo mass relation
• From EMBER to FIRE: predicting high resolution baryon fields from dark matter simulations with Deep Learning
• The neutral hydrogen distribution in large-scale haloes from 21-cm intensity maps
• A scale dependent bias on linear scales: the case for HI intensity mapping at z=1
• HI Intensity Mapping for Clustering-Based Redshift Estimation
• Redshift space distortions of the {\rm HI} 21-cm intensity mapping signal due to the internal motions within galaxies
• Modelling the post-reionization neutral hydrogen ($\mathrm{HI}$) 21-cm bispectrum
• Halo models of HI selected galaxies
• The galaxy HI-(sub)halo connection and the HI spatial clustering of local galaxies
• New empirical constraints on the cosmological evolution of gas and stars in galaxies
• HI gas content of SDSS galaxies revealed by ALFALFA: implications for the mass-metallicity relation and the environmental dependence of HI in the local Universe
• Filament Hunting: Integrated HI 21cm Emission From Filaments Inferred by Galaxy Surveys
• Synergizing 21 cm and sub-millimetre surveys during reionization: new empirical insights
• HI intensity mapping correlation function from UNIT simulations: BAO and observationally induced anisotropy
• Extreme Spheres: Counts-in-cells for 21cm intensity mapping
• Disk galaxies are self-similar: the universality of the HI-to-Halo mass ratio for isolated disks
• The Population of Galaxies that Contribute to The HI Mass Function
• The GMRT archive atomic gas survey -- II. Mass modelling and dark matter halo properties across late-type spirals
• The Dark Matter Halos of HI Selected Galaxies
• A Multi-messenger view of Cosmic Dawn: Conquering the Final Frontier
• The bias from hydrodynamic simulations: mapping baryon physics onto dark matter fields
• The slingshot effect as a probe of transverse motions of galaxies
• Neutral hydrogen in the post-reionization universe
• The Baryon Budget of Galaxies across the First Billion Years