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 ($z0$) 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 model the evolution of the HIHM relation in a
manner similar to that of the stellar-halo mass (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 find that the
peak HI mass fraction moderately increases from 1% at $z=0$ to about 3.1% at
$z=4$. The corresponding halo mass increases from $10^11.7$ M$_ødot$ to
$10^12.4$ M$_ødot$. The data do not suggest a strong evolution in the HI
density profile. Predictions of this model are in excellent agreement with the
observed column density distribution and incidence rate of high-column-density
HI absorption-line systems at high redshift, although the agreement is poor
with the column density distribution at $z=0$. The increase in the halo mass
with maximum HI mass fraction also enables the model predictions to
successfully match the measured clustering bias of high column density HI
systems at $z=2.3$. We discuss the resultant evolution of the HIHM relation and
its consequences for HI and galaxy evolution. Abridged Abstract
Description
[1608.00007] Constraints on the evolution of the relationship between HI mass and halo mass in the last 12 Gyr
%0 Generic
%1 padmanabhan2016constraints
%A Padmanabhan, Hamsa
%A Kulkarni, Girish
%D 2016
%K HI evolution halo mass
%T Constraints on the evolution of the relationship between HI mass and
halo mass in the last 12 Gyr
%U http://arxiv.org/abs/1608.00007
%X 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 ($z0$) 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 model the evolution of the HIHM relation in a
manner similar to that of the stellar-halo mass (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 find that the
peak HI mass fraction moderately increases from 1% at $z=0$ to about 3.1% at
$z=4$. The corresponding halo mass increases from $10^11.7$ M$_ødot$ to
$10^12.4$ M$_ødot$. The data do not suggest a strong evolution in the HI
density profile. Predictions of this model are in excellent agreement with the
observed column density distribution and incidence rate of high-column-density
HI absorption-line systems at high redshift, although the agreement is poor
with the column density distribution at $z=0$. The increase in the halo mass
with maximum HI mass fraction also enables the model predictions to
successfully match the measured clustering bias of high column density HI
systems at $z=2.3$. We discuss the resultant evolution of the HIHM relation and
its consequences for HI and galaxy evolution. Abridged Abstract
@misc{padmanabhan2016constraints,
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 model the evolution of the HIHM relation in a
manner similar to that of the stellar-halo mass (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 find that the
peak HI mass fraction moderately increases from 1% at $z=0$ to about 3.1% at
$z=4$. The corresponding halo mass increases from $10^{11.7}$ M$_\odot$ to
$10^{12.4}$ M$_\odot$. The data do not suggest a strong evolution in the HI
density profile. Predictions of this model are in excellent agreement with the
observed column density distribution and incidence rate of high-column-density
HI absorption-line systems at high redshift, although the agreement is poor
with the column density distribution at $z=0$. The increase in the halo mass
with maximum HI mass fraction also enables the model predictions to
successfully match the measured clustering bias of high column density HI
systems at $z=2.3$. We discuss the resultant evolution of the HIHM relation and
its consequences for HI and galaxy evolution. [Abridged Abstract]},
added-at = {2016-08-02T09:37:16.000+0200},
author = {Padmanabhan, Hamsa and Kulkarni, Girish},
biburl = {https://www.bibsonomy.org/bibtex/236cf114ba91d9a03e17aba0f06c9c75a/miki},
description = {[1608.00007] Constraints on the evolution of the relationship between HI mass and halo mass in the last 12 Gyr},
interhash = {0b8ede701b8825c3c3733a14de7b2e78},
intrahash = {36cf114ba91d9a03e17aba0f06c9c75a},
keywords = {HI evolution halo mass},
note = {cite arxiv:1608.00007Comment: 10 pages; 8 figures; 1 table},
timestamp = {2016-08-02T09:37:16.000+0200},
title = {Constraints on the evolution of the relationship between HI mass and
halo mass in the last 12 Gyr},
url = {http://arxiv.org/abs/1608.00007},
year = 2016
}