TY - JOUR
T1 - The stellar-to-halo mass relation of GAMA galaxies from 100 deg2 of KiDS weak lensing data
AU - van Uitert, Edo
AU - Cacciato, Marcello
AU - Hoekstra, Henk
AU - Brouwer, Margot
AU - Sifón, Cristóbal
AU - Viola, Massimo
AU - Baldry, Ivan
AU - Bland-Hawthorn, Joss
AU - Brough, Sarah
AU - Brown, M. J. I.
AU - Choi, Ami
AU - Driver, Simon P.
AU - Erben, Thomas
AU - Heymans, Catherine
AU - Hildebrandt, Hendrik
AU - Joachimi, Benjamin
AU - Kuijken, Konrad
AU - Liske, Jochen
AU - Loveday, Jon
AU - McFarland, John
AU - Miller, Lance
AU - Nakajima, Reiko
AU - Peacock, John
AU - Radovich, Mario
AU - Robotham, A. S. G.
AU - Schneider, Peter
AU - Sikkema, Gert
AU - Taylor, Edward N.
AU - Verdoes Kleijn, Gijs
PY - 2016/7/1
Y1 - 2016/7/1
N2 - We study the stellar-to-halo mass relation of central galaxies in the
range 9.7 <log 10(M*/h- 2
M⊙) <11.7 and z <0.4, obtained from a combined
analysis of the Kilo Degree Survey (KiDS) and the Galaxy And Mass
Assembly (GAMA) survey. We use ˜100 deg2 of KiDS data
to study the lensing signal around galaxies for which spectroscopic
redshifts and stellar masses were determined by GAMA. We show that
lensing alone results in poor constraints on the stellar-to-halo mass
relation due to a degeneracy between the satellite fraction and the halo
mass, which is lifted when we simultaneously fit the stellar mass
function. At M* > 5 × 1010 h-
2 M⊙, the stellar mass increases with halo mass as
{˜ }M_h^{0.25}. The ratio of dark matter to stellar mass has a
minimum at a halo mass of 8 × 1011 h-1
M⊙ with a value of M_h/M_{*}=56_{-10}^{+16} [h]. We also
use the GAMA group catalogue to select centrals and satellites in groups
with five or more members, which trace regions in space where the local
matter density is higher than average, and determine for the first time
the stellar-to-halo mass relation in these denser environments. We find
no significant differences compared to the relation from the full
sample, which suggests that the stellar-to-halo mass relation does not
vary strongly with local density. Furthermore, we find that the
stellar-to-halo mass relation of central galaxies can also be obtained
by modelling the lensing signal and stellar mass function of satellite
galaxies only, which shows that the assumptions to model the satellite
contribution in the halo model do not significantly bias the
stellar-to-halo mass relation. Finally, we show that the combination of
weak lensing with the stellar mass function can be used to test the
purity of group catalogues.
AB - We study the stellar-to-halo mass relation of central galaxies in the
range 9.7 <log 10(M*/h- 2
M⊙) <11.7 and z <0.4, obtained from a combined
analysis of the Kilo Degree Survey (KiDS) and the Galaxy And Mass
Assembly (GAMA) survey. We use ˜100 deg2 of KiDS data
to study the lensing signal around galaxies for which spectroscopic
redshifts and stellar masses were determined by GAMA. We show that
lensing alone results in poor constraints on the stellar-to-halo mass
relation due to a degeneracy between the satellite fraction and the halo
mass, which is lifted when we simultaneously fit the stellar mass
function. At M* > 5 × 1010 h-
2 M⊙, the stellar mass increases with halo mass as
{˜ }M_h^{0.25}. The ratio of dark matter to stellar mass has a
minimum at a halo mass of 8 × 1011 h-1
M⊙ with a value of M_h/M_{*}=56_{-10}^{+16} [h]. We also
use the GAMA group catalogue to select centrals and satellites in groups
with five or more members, which trace regions in space where the local
matter density is higher than average, and determine for the first time
the stellar-to-halo mass relation in these denser environments. We find
no significant differences compared to the relation from the full
sample, which suggests that the stellar-to-halo mass relation does not
vary strongly with local density. Furthermore, we find that the
stellar-to-halo mass relation of central galaxies can also be obtained
by modelling the lensing signal and stellar mass function of satellite
galaxies only, which shows that the assumptions to model the satellite
contribution in the halo model do not significantly bias the
stellar-to-halo mass relation. Finally, we show that the combination of
weak lensing with the stellar mass function can be used to test the
purity of group catalogues.
KW - gravitational lensing: weak
KW - methods: observational
KW - galaxies: groups: general
KW - galaxies: haloes
KW - galaxies: luminosity function
KW - mass function
U2 - 10.1093/mnras/stw747
DO - 10.1093/mnras/stw747
M3 - Article
VL - 459
SP - 3251
EP - 3270
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 3
ER -