The stellar-to-halo mass relation of GAMA galaxies from 100 square degrees of KiDS weak lensing data

TL;DR

This study combines KiDS weak lensing data with GAMA survey information to precisely measure the stellar-to-halo mass relation of galaxies, exploring environmental effects and the reliability of group catalogues.

Contribution

It provides the first measurement of the stellar-to-halo mass relation in dense environments using combined lensing and group data, and demonstrates the robustness of the relation derived from satellite galaxies.

Findings

Stellar-to-halo mass relation follows M_h^0.25 for M_* > 5x10^10 h^-2 M_sun.

Minimum dark matter to stellar mass ratio occurs at M_h=8x10^11 h^-1 M_sun with ratio 56.

No significant difference in the relation between dense environments and the full sample.

Abstract

We study the stellar-to-halo mass relation of central galaxies in the range 9.7<log_10(M_*/h^-2 M_sun)<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 deg^2 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_sun>5x10^10 h^-2 M_sun, 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 8x10^11 h^-1 M_sun 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.