論文

2019年4月16日

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

  • Ryoma Murata
  • ,
  • Masamune Oguri
  • ,
  • Takahiro Nishimichi
  • ,
  • Masahiro Takada
  • ,
  • Rachel Mandelbaum
  • ,
  • Surhud More
  • ,
  • Masato Shirasaki
  • ,
  • Atsushi J. Nishizawa
  • ,
  • Ken Osato

記述言語
掲載種別
研究論文(学術雑誌)

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

リンク情報
arXiv
http://arxiv.org/abs/arXiv:1904.07524
URL
http://arxiv.org/abs/1904.07524v1

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