Weak lensing clusters from HSC-SSP s16a data (Hamana, Shirasaki, and Yen-Ting, 2020)

  • Related paper: "An empirical method for mitigating an excess up-scattering mass bias on the weak lensing mass estimates for shear-selected cluster samples", Takashi Hamana (2022)
  • Updated cluster masses with correction for the excess up-scattering mass bias from Table 1 of Hamana 2022
  • A preprint with full resolution figures
  • HWL16a peak catalog
  • hscmap format csv file
  • [c200c, M200c, M500c] of HWL16a secure clusters from Table 3 of Hamana, Shirasaki, and Yen-Ting, 2020
  • A Fortran program to generate weak lensing mass maps from shear data
  • Public data products

    • Some details of individual peaks:
  • XMM field [ID=1-23]
  • GAMA09H field [ID=24-41]
  • WIDE12H field [ID=42-56]
  • GAMA15H field [ID=57-98]
  • HECTOMAP field [ID=99-103]
  • VVDS field [ID=104-124]
    • In the above links, plots shown are:
  • Top: 10 arcmin-side riz composite image, the yellow contour shows the weak lensing SN (the contour lines start from SN=2 with the interval of 1), and the cyan/magenta/red plus marks show the position of CAMIRA/NED/XXL clusters with label (CAMIRA-ID/redshift/richness)/(cluster-name from NED/redshift)/(XXL-id/redshift).
  • Bottom-left: Azimuthally averaged galaxy number density as a function of the angular separation from the SN peak position. Different colors show different z_min (black/red/gree/blue/cyan/magenta for z_min=0/0.2/0.3/0.4/0.5/0.6).
  • Bottom-right: Red line shows the weak lensing peak SN as a function of z_min.
    • Lists of matched known clusters:
    Clusters from CAMIRA (version s16a_wide_smnew), XXL (XXL 365 cluster catalogue) and NED matched within the angular separation of 5 arcmin from weak lensing SN peak positions are summarized in tables.

    Contact: Takashi Hamana


    Last update: 2022/10/18
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