Journal
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
Volume 70, Issue -, Pages -Publisher
OXFORD UNIV PRESS
DOI: 10.1093/pasj/psx128
Keywords
cosmology: observations; dark matter; galaxies: clusters: general; gravitational lensing: weak; large-scale structure of universe
Categories
Funding
- FIRST program from Japanese Cabinet Office
- Japan Society for the Promotion of Science (JSPS)
- Japan Science and Technology Agency (JST)
- Toray Science Foundation
- NAOJ
- Kavli IPMU
- KEK
- ASIAA
- Princeton University
- National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]
- National Science Foundation [AST-1238877]
- Princeton Institute for Computational Science and Engineering
- Princeton University Office of Information Technology's Research Computing department
- Lyman Spitzer Jr. Fellowship
- Jet Propulsion Laboratory, California Institute of Technology
- National Aeronautics and Space Administration
- World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan
- JSPS KAKENHI [26800093, 15H05892]
- Ministry of Science and Technology of Taiwan [MOST 103-2112-M-001-030-MY3]
- Ministry of Education, Culture, Sports, Science and Technology (MEXT)
- Grants-in-Aid for Scientific Research [15K21733, 26800093, 17H06600] Funding Source: KAKEN
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Using similar to 140 deg(2) Subaru Hyper Suprime-Cam (HSC) survey data, we stack the weak lensing (WL) signal around five Planck clusters found within the footprint. This yields a 15 sigma detection of the mean Planck cluster mass density profile. The five Planck clusters span a relatively wide mass range, M-WL,M-500c = (2-30) x 10(14) M-circle dot with a mean mass of M-WL,M-500c = (4.15 +/- 0.61) x 10(14) M-circle dot. The ratio of the stacked Planck Sunyaev-Zel'dovich (SZ) mass to the stacked WL mass is < M-SZ > / < M-WL > = 1 - b = 0.80 +/- 0.14. This mass bias is consistent with previous WL mass calibrations of Planck clusters within the errors. We discuss the implications of our findings for the calibration of SZ cluster counts and the much discussed tension between Planck SZ cluster counts and Planck Lambda CDM cosmology.
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