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We utilize the galaxy shape catalogue from the first-year data release of theSubaru Hyper Suprime-cam Survey (HSC) to study the dark matter content ofgalaxy groups in the Universe using weak lensing. We use galaxy groups from theGalaxy Mass and Assembly galaxy survey in approximately $100$ sq. degrees ofthe sky that overlap with the HSC survey as lenses. We restrict our analysis tothe $1587$ groups with at least five members. We divide these groups into sixbins each of group luminosity and group member velocity dispersion and measurethe lensing signal with a signal-to-noise ratio of $55$ and $51$ for these twodifferent selections, respectively. We use a Bayesian halo model framework toinfer the halo mass distribution of our groups binned in the two differentobservable properties and constrain the power-law scaling relation, and thescatter between mean halo masses and the two group observable properties. Weobtain a 5 percent constraint on the amplitude of the scaling relation betweenhalo mass and group luminosity with $\avg{M} = (0.81\pm0.04)\times10^{14}\hinvMsun$ for $L_{\rm grp}=10^{11.5}\hinvsqLsun$, and apower-law index of $\alpha=1.01\pm 0.07$. We constrain the amplitude of thescaling relation between halo mass and velocity dispersion to be$\avg{M}=(0.93\pm 0.05)\times10^{14}\hinvMsun$ for $\sigma=500 \kms$ and apower-law index to be $\alpha=1.52\pm0.10$. However, these scaling relationsare sensitive to the exact cuts applied to the number of group members.Comparisons with similar scaling relations from the literature show that ourresults are consistent and have significantly reduced errors.

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