TY - JOUR
T1 - The Galaxy–Halo Connection for 1.5\lesssim z\lesssim 5 as Revealed by the Spitzer Matching Survey of the UltraVISTA Ultra-deep Stripes
AU - Cowley, William I.
AU - Caputi, Karina I.
AU - Deshmukh, Smaran
AU - Ashby, Matthew L. N.
AU - Fazio, Giovanni G.
AU - Le Fèvre, Olivier
AU - Fynbo, Johan P. U.
AU - Ilbert, Olivier
AU - McCracken, Henry J.
AU - Milvang-Jensen, Bo
AU - Somerville, Rachel S.
PY - 2018/1/24
Y1 - 2018/1/24
N2 - The Spitzer Matching Survey of the UltraVISTA ultra-deep Stripes (SMUVS)
provides unparalleled depth at 3.6 and 4.5 μm over ∼0.66
deg2 of the COSMOS field, allowing precise photometric
determinations of redshift and stellar mass. From this unique data set
we can connect galaxy samples, selected by stellar mass, to their host
dark matter halos for 1.5<z<5.0, filling in a large hitherto
unexplored region of the parameter space. To interpret the observed
galaxy clustering, we use a phenomenological halo model, combined with a
novel method to account for uncertainties arising from the use of
photometric redshifts. We find that the satellite fraction decreases
with increasing redshift and that the clustering amplitude (e.g.,
comoving correlation length/large-scale bias) displays monotonic trends
with redshift and stellar mass. Applying ΛCDM halo mass accretion
histories and cumulative abundance arguments for the evolution of
stellar mass content, we propose pathways for the coevolution of dark
matter and stellar mass assembly. Additionally, we are able to estimate
that the halo mass at which the ratio of stellar-to-halo mass is
maximized is {10}{12.5-0.08+0.10}
{M}ȯ at z∼ 2.5. This peak halo mass is here
inferred for the first time from stellar mass-selected clustering
measurements at z≳ 2, and it implies a mild evolution of this
quantity for z≲ 3, consistent with constraints from
abundance-matching techniques.
AB - The Spitzer Matching Survey of the UltraVISTA ultra-deep Stripes (SMUVS)
provides unparalleled depth at 3.6 and 4.5 μm over ∼0.66
deg2 of the COSMOS field, allowing precise photometric
determinations of redshift and stellar mass. From this unique data set
we can connect galaxy samples, selected by stellar mass, to their host
dark matter halos for 1.5<z<5.0, filling in a large hitherto
unexplored region of the parameter space. To interpret the observed
galaxy clustering, we use a phenomenological halo model, combined with a
novel method to account for uncertainties arising from the use of
photometric redshifts. We find that the satellite fraction decreases
with increasing redshift and that the clustering amplitude (e.g.,
comoving correlation length/large-scale bias) displays monotonic trends
with redshift and stellar mass. Applying ΛCDM halo mass accretion
histories and cumulative abundance arguments for the evolution of
stellar mass content, we propose pathways for the coevolution of dark
matter and stellar mass assembly. Additionally, we are able to estimate
that the halo mass at which the ratio of stellar-to-halo mass is
maximized is {10}{12.5-0.08+0.10}
{M}ȯ at z∼ 2.5. This peak halo mass is here
inferred for the first time from stellar mass-selected clustering
measurements at z≳ 2, and it implies a mild evolution of this
quantity for z≲ 3, consistent with constraints from
abundance-matching techniques.
KW - galaxies: evolution
KW - galaxies: formation
KW - galaxies: high-redshift
KW - large-scale structure of universe
KW - methods: statistical
U2 - 10.3847/1538-4357/aaa41d
DO - 10.3847/1538-4357/aaa41d
M3 - Article
VL - 853
JO - The Astrophysical Journal
JF - The Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 69
ER -