Predictions for the Abundance of High-redshift Galaxies in a Fuzzy Dark Matter Universe. (arXiv:1904.01604v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ni_Y/0/1/0/all/0/1">Yueying Ni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_M/0/1/0/all/0/1">Mei-Yu Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Feng_Y/0/1/0/all/0/1">Yu Feng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matteo_T/0/1/0/all/0/1">Tiziana Di Matteo</a>
During the last decades, rapid progress has been made in measurements of the
rest-frame ultraviolet (UV) luminosity function (LF) for high-redshift galaxies
($z geq 6$). The faint-end of the galaxy LF at these redshifts provides
powerful constraints on different dark matter models that suppress small-scale
structure formation. In this work we perform full hydrodynamical cosmological
simulations of galaxy formation using an alternative DM model composed of
extremely light bosonic particles ($m sim 10^{-22}$ eV), also known as fuzzy
dark matter (FDM), and examine the predictions for the galaxy stellar mass
function and luminosity function at $z geq 6$ for a range of FDM masses. We
find that for FDM models with bosonic mass $m = 5times10^{-22}$ eV, the number
density of galaxies with stellar mass $rm M_* sim 10^7 M_{odot}$ is
suppressed by $sim 40%$ at z = 9, $sim 20%$ at z = 5, and the UV LFs within
magnitude range of -16 < $M_{rm UV}$ < -14 is suppressed by $sim 60%$ at $z
= 9$, $sim 20%$ at $z = 5$ comparing to the CDM counterpart simulation.
Comparing our predictions with current measurements of the faint-end LFs ($-18
leqslant M_{rm UV} leqslant -14$), we find that FDM models with $m_{22} <
5times10^{-22}$ are ruled out at $3sigma$ confidence level. We expect that
future LF measurements by James Webb Space Telescope (JWST), which will extend
down to $M_{rm UV} sim -13$ for $z lesssim 10$, with a survey volume that is
comparable to the Hubble Ultra Deep Field (HUDF) would have the capability to
constrain FDM models to $m; gtrsim 10^{-21}$ eV.
During the last decades, rapid progress has been made in measurements of the
rest-frame ultraviolet (UV) luminosity function (LF) for high-redshift galaxies
($z geq 6$). The faint-end of the galaxy LF at these redshifts provides
powerful constraints on different dark matter models that suppress small-scale
structure formation. In this work we perform full hydrodynamical cosmological
simulations of galaxy formation using an alternative DM model composed of
extremely light bosonic particles ($m sim 10^{-22}$ eV), also known as fuzzy
dark matter (FDM), and examine the predictions for the galaxy stellar mass
function and luminosity function at $z geq 6$ for a range of FDM masses. We
find that for FDM models with bosonic mass $m = 5times10^{-22}$ eV, the number
density of galaxies with stellar mass $rm M_* sim 10^7 M_{odot}$ is
suppressed by $sim 40%$ at z = 9, $sim 20%$ at z = 5, and the UV LFs within
magnitude range of -16 < $M_{rm UV}$ < -14 is suppressed by $sim 60%$ at $z
= 9$, $sim 20%$ at $z = 5$ comparing to the CDM counterpart simulation.
Comparing our predictions with current measurements of the faint-end LFs ($-18
leqslant M_{rm UV} leqslant -14$), we find that FDM models with $m_{22} <
5times10^{-22}$ are ruled out at $3sigma$ confidence level. We expect that
future LF measurements by James Webb Space Telescope (JWST), which will extend
down to $M_{rm UV} sim -13$ for $z lesssim 10$, with a survey volume that is
comparable to the Hubble Ultra Deep Field (HUDF) would have the capability to
constrain FDM models to $m; gtrsim 10^{-21}$ eV.
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