2024-03-29T10:11:29Z
https://nagoya.repo.nii.ac.jp/oai
oai:nagoya.repo.nii.ac.jp:00028388
2023-01-16T04:29:20Z
2026:2027:2028
Weak-lensing Mass Calibration of ACTPol Sunyaev–Zel’dovich Clusters with the Hyper Suprime-Cam Survey
Miyatake, Hironao
Battaglia, Nicholas
Hilton, Matt
Medezinski, Elinor
Nishizawa, Atsushi J.
More, Surhud
Aiola, Simone
Bahcall, Neta
Bond, J. Richard
Calabrese, Erminia
Choi, Steve K.
Devlin, Mark J.
Dunkley, Joanna
Dunner, Rolando
Fuzia, Brittany
Gallardo, Patricio
Gralla, Megan
Hasselfield, Matthew
Halpern, Mark
Hikage, Chiaki
Hill, J. Colin
Hincks, Adam D.
Hložek, Renée
Huffenberger, Kevin
Hughes, John P.
Koopman, Brian
Kosowsky, Arthur
Louis, Thibaut
Madhavacheril, Mathew S.
McMahon, Jeff
Mandelbaum, Rachel
Marriage, Tobias A.
Maurin, Loïc
Miyazaki, Satoshi
Moodley, Kavilan
Murata, Ryoma
Naess, Sigurd
Newburgh, Laura
Niemack, Michael D.
Nishimichi, Takahiro
Okabe, Nobuhiro
Oguri, Masamune
Osato, Ken
Page, Lyman
Partridge, Bruce
Robertson, Naomi
Sehgal, Neelima
Sherwin, Blake
Shirasaki, Masato
Sievers, Jonathan
Sifón, Cristóbal
Simon, Sara
Spergel, David N.
Staggs, Suzanne T.
Stein, George
Takada, Masahiro
Trac, Hy
Umetsu, Keiichi
Engelen, Alex van
Wollack, Edward J.
open access
© 2019. The American Astronomical Society
cosmology: observations
galaxies: clusters: general
gravitational lensing: weak
We present weak-lensing measurements using the first-year data from the Hyper Suprime-Cam Strategic Survey Program on the Subaru telescope for eight galaxy clusters selected through their thermal Sunyaev–Zel'dovich (SZ) signal measured at 148 GHz with the Atacama Cosmology Telescope Polarimeter experiment. The overlap between the two surveys in this work is 33.8 square degrees, before masking bright stars. The signal-to-noise ratio of individual cluster lensing measurements ranges from 2.2 to 8.7, with a total of 11.1 for the stacked cluster weak-lensing signal. We fit for an average weak-lensing mass distribution using three different profiles, a Navarro–Frenk–White profile, a dark-matter-only emulated profile, and a full cosmological hydrodynamic emulated profile. We interpret the differences among the masses inferred by these models as a systematic error of 10%, which is currently smaller than the statistical error. We obtain the ratio of the SZ-estimated mass to the lensing-estimated mass (the so-called hydrostatic mass bias 1−b) of ${0.74}_{-0.12}^{+0.13}$, which is comparable to previous SZ-selected clusters from the Atacama Cosmology Telescope and from the Planck Satellite. We conclude with a discussion of the implications for cosmological parameters inferred from cluster abundances compared to cosmic microwave background primary anisotropy measurements.
IOP publishing
2019-04
eng
journal article
VoR
http://hdl.handle.net/2237/00030581
https://nagoya.repo.nii.ac.jp/records/28388
https://doi.org/10.3847/1538-4357/ab0af0
1538-4357
The Astrophysical Journal
875
1
63
https://nagoya.repo.nii.ac.jp/record/28388/files/Miyatake_2019_ApJ_875_63.pdf
application/pdf
2.0 MB
2019-08-08