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Constraining the relation between the richness $N$ and the halo mass $M$ overa wide redshift range for optically-selected clusters is a key ingredient forcluster-related science in optical surveys, including the Subaru HyperSuprime-Cam (HSC) survey. We measure stacked weak lensing profiles around 1747HSC CAMIRA clusters over a redshift range of $0.1\leq z_{\rm cl}\leq 1.0$ with$N\geq 15$ using the HSC first-year shear catalog covering $\sim$$140$ ${\rmdeg^2}$. The exquisite depth and image quality of the HSC survey allow us tomeasure lensing signals around the high-redshift clusters at $0.7\leq z_{\rmcl}\leq 1.0$ with a signal-to-noise ratio of 19 in the comoving radius range$0.5\lesssim R\lesssim 15 h^{-1}{\rm Mpc}$. We constrain richness-massrelations $P(\ln N|M,z)$ of the HSC CAMIRA clusters assuming a log-normaldistribution without informative priors on model parameters, by jointly fittingto the lensing profiles and abundance measurements under both Planck and WMAPcosmological models. We show that our model gives acceptable $p$-values when weadd redshift dependent terms which are proportional to $\ln (1+z)$ and $[\ln(1+z)]^{2}$ into the mean and scatter relations of $P(\ln N|M,z)$. Such termspresumably originate from the variation of photometric redshift errors as afunction of the redshift. We show that the constraints on the mean relation$\langle M|N \rangle$ are consistent between the Planck and WMAP models,whereas the scatter values $\sigma_{\ln M|N}$ for the Planck model aresystematically larger than those for the WMAP model. We also show that thescatter values for the Planck model increase toward lower richness values,whereas those for the WMAP model are consistent with constant values as afunction of richness. This result highlights the importance of the scatter inthe mass-richness relation for cluster cosmology.

The mass-richness relation of optically-selected clusters from weak gravitational lensing and abundance with Subaru HSC first-year data