Any successful model of galaxy formation needs to explain the low rate of
star formation in the small progenitors of today's normal galaxies. The low
efficiency of star formation is necessary for reproducing the low
stellar-to-halo mass fractions, as suggested by current abundance matching
models. We found that the main driver of this low efficiency is the radiation
pressure exerted by ionizing photons from massive and young stars. We model the
effect of radiation pressure in cosmological, zoom-in galaxy formation
simulations, as a non-thermal pressure that acts locally around dense and
optically thick star-forming regions. We also include the effect of
photoionization and photoheating on the gas cooling and heating rates. In some
conditions, the full photoionization of HI reduces the HI peak of the cooling
curve, effectively preventing cooling in the 10^4-10^4.5 K regime. We also
consider a simple model for the boosting of radiation pressure due to the
trapping of infrared radiation. The main effect of the local UV radiation is to
regulate and limit the high values of the gas density distribution and the
amount of gas available for star formation. Radiation pressure is the main
driver that regulates star formation, stellar and galaxy growth in halos of
masses around 10^11 Msun at high redshifts, z=3. Infrared trapping and
photoionization/photoheating processes are secondary effects in this mass
range. The typical galaxies residing in these halos contain only 0.6% of the
total virial mass in stars and form stars at a small rate of 1 Msun/yr at z=3,
roughly consistent with current abundance matching models. The effect of the
local UV radiation ultimately translates into a lighter and more extended
galaxy and it yields a raising circular velocity profile.
Description
[1307.0943] Radiative feedback and the low efficiency of galaxy formation in low-mass halos at high redshift
%0 Generic
%1 ceverino2013radiative
%A Ceverino, Daniel
%A Klypin, Anatoly
%A Klimek, Elizabeth
%A Trujillo-Gomez, Sebastian
%A Churchill, Christopher W.
%A Primack, Joel
%D 2013
%K feedback galaxy radiative simulation
%T Radiative feedback and the low efficiency of galaxy formation in
low-mass halos at high redshift
%U http://arxiv.org/abs/1307.0943
%X Any successful model of galaxy formation needs to explain the low rate of
star formation in the small progenitors of today's normal galaxies. The low
efficiency of star formation is necessary for reproducing the low
stellar-to-halo mass fractions, as suggested by current abundance matching
models. We found that the main driver of this low efficiency is the radiation
pressure exerted by ionizing photons from massive and young stars. We model the
effect of radiation pressure in cosmological, zoom-in galaxy formation
simulations, as a non-thermal pressure that acts locally around dense and
optically thick star-forming regions. We also include the effect of
photoionization and photoheating on the gas cooling and heating rates. In some
conditions, the full photoionization of HI reduces the HI peak of the cooling
curve, effectively preventing cooling in the 10^4-10^4.5 K regime. We also
consider a simple model for the boosting of radiation pressure due to the
trapping of infrared radiation. The main effect of the local UV radiation is to
regulate and limit the high values of the gas density distribution and the
amount of gas available for star formation. Radiation pressure is the main
driver that regulates star formation, stellar and galaxy growth in halos of
masses around 10^11 Msun at high redshifts, z=3. Infrared trapping and
photoionization/photoheating processes are secondary effects in this mass
range. The typical galaxies residing in these halos contain only 0.6% of the
total virial mass in stars and form stars at a small rate of 1 Msun/yr at z=3,
roughly consistent with current abundance matching models. The effect of the
local UV radiation ultimately translates into a lighter and more extended
galaxy and it yields a raising circular velocity profile.
@misc{ceverino2013radiative,
abstract = {Any successful model of galaxy formation needs to explain the low rate of
star formation in the small progenitors of today's normal galaxies. The low
efficiency of star formation is necessary for reproducing the low
stellar-to-halo mass fractions, as suggested by current abundance matching
models. We found that the main driver of this low efficiency is the radiation
pressure exerted by ionizing photons from massive and young stars. We model the
effect of radiation pressure in cosmological, zoom-in galaxy formation
simulations, as a non-thermal pressure that acts locally around dense and
optically thick star-forming regions. We also include the effect of
photoionization and photoheating on the gas cooling and heating rates. In some
conditions, the full photoionization of HI reduces the HI peak of the cooling
curve, effectively preventing cooling in the 10^4-10^4.5 K regime. We also
consider a simple model for the boosting of radiation pressure due to the
trapping of infrared radiation. The main effect of the local UV radiation is to
regulate and limit the high values of the gas density distribution and the
amount of gas available for star formation. Radiation pressure is the main
driver that regulates star formation, stellar and galaxy growth in halos of
masses around 10^11 Msun at high redshifts, z=3. Infrared trapping and
photoionization/photoheating processes are secondary effects in this mass
range. The typical galaxies residing in these halos contain only 0.6% of the
total virial mass in stars and form stars at a small rate of 1 Msun/yr at z=3,
roughly consistent with current abundance matching models. The effect of the
local UV radiation ultimately translates into a lighter and more extended
galaxy and it yields a raising circular velocity profile.},
added-at = {2013-07-04T07:42:13.000+0200},
author = {Ceverino, Daniel and Klypin, Anatoly and Klimek, Elizabeth and Trujillo-Gomez, Sebastian and Churchill, Christopher W. and Primack, Joel},
biburl = {https://www.bibsonomy.org/bibtex/21013de9fc23e382d1d4b8b9aaf72ea76/miki},
description = {[1307.0943] Radiative feedback and the low efficiency of galaxy formation in low-mass halos at high redshift},
interhash = {9b05dcea5f87cc93d89f50755f9854a7},
intrahash = {1013de9fc23e382d1d4b8b9aaf72ea76},
keywords = {feedback galaxy radiative simulation},
note = {cite arxiv:1307.0943Comment: 17 pages, 11 figures, submitted to MNRAS},
timestamp = {2013-07-04T07:42:14.000+0200},
title = {Radiative feedback and the low efficiency of galaxy formation in
low-mass halos at high redshift},
url = {http://arxiv.org/abs/1307.0943},
year = 2013
}