The Subaru HSC weak lensing mass-observable scaling relations of spectroscopic galaxy groups from the GAMA survey

TL;DR

This study uses Subaru HSC weak lensing data to precisely measure the mass-observable scaling relations of galaxy groups from the GAMA survey, improving constraints on dark matter content and halo properties.

Contribution

It presents the first detailed weak lensing analysis of GAMA galaxy groups using Subaru HSC data, providing tight constraints on mass-luminosity and mass-velocity dispersion relations.

Findings

Measured the halo mass-luminosity relation with 5% precision.

Constrained the halo mass-velocity dispersion relation with improved accuracy.

Found that scaling relations are sensitive to group member count cuts.

Abstract

We utilize the galaxy shape catalogue from the first-year data release of the Subaru Hyper Suprime-cam Survey (HSC) to study the dark matter content of galaxy groups in the Universe using weak lensing. We use galaxy groups from the Galaxy Mass and Assembly galaxy survey in approximately $100$ sq. degrees of the sky that overlap with the HSC survey as lenses. We restrict our analysis to the $1587$ groups with at least five members. We divide these groups into six bins each of group luminosity and group member velocity dispersion and measure the lensing signal with a signal-to-noise ratio of $55$ and $51$ for these two different selections, respectively. We use a Bayesian halo model framework to infer the halo mass distribution of our groups binned in the two different observable properties and constrain the power-law scaling relation, and the scatter between mean halo masses and the two group observable properties. We obtain a 5 percent constraint on the amplitude of the scaling relation between halo mass and group luminosity with $\avg{M} = (0.81\pm 0.04)\times10^{14}\hinvMsun$ for $L_{\rm grp}=10^{11.5}\hinvsqLsun$, and a power-law index of $\alpha=1.01\pm 0.07$. We constrain the amplitude of the scaling relation between halo mass and velocity dispersion to be $\avg{M}=(0.93\pm 0.05)\times10^{14}\hinvMsun$ for $\sigma=500 \kms$ and a power-law index to be $\alpha=1.52\pm0.10$. However, these scaling relations are sensitive to the exact cuts applied to the number of group members. Comparisons with similar scaling relations from the literature show that our results are consistent and have significantly reduced errors.