Stacked phase-space density of galaxies around massive clusters: Comparison of dynamical and lensing masses
Affiliation
Steward Observatory, University of ArizonaIssue Date
2021Keywords
galaxies: clusters: generalgalaxies: kinematics and dynamics
large-scale structure of Universe
methods: observational
Metadata
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Oxford University PressCitation
Shirasaki, M., Egami, E., Okabe, N., & Miyazaki, S. (2021). Stacked phase-space density of galaxies around massive clusters: Comparison of dynamical and lensing masses. Monthly Notices of the Royal Astronomical Society, 506(3), 3385–3405.Rights
Copyright © 2021 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.Collection Information
This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.Abstract
We present a measurement of average histograms of line-of-sight velocities over pairs of galaxies and galaxy clusters. Since the histogram can be measured at different galaxy-cluster separations, this observable is commonly referred to as the stacked phase-space density. We formulate the stacked phase-space density based on a halo-model approach so that the model can be applied to real samples of galaxies and clusters. We examine our model by using an actual sample of massive clusters with known weak-lensing masses and spectroscopic observations of galaxies around the clusters. A likelihood analysis with our model enables us to infer the spherical-symmetric velocity dispersion of observed galaxies in massive clusters. We find the velocity dispersion of galaxies surrounding clusters with their lensing masses of 1.1 × 1015, h-1,M⊙ to be 1180+83-70, km s-1 at the 68 per cent confidence level. Our constraint confirms that the relation between the galaxy velocity dispersion and the host cluster mass in our sample is consistent with the prediction in dark-matter-only N-body simulations under General Relativity. Assuming that the Poisson equation in clusters can be altered by an effective gravitational constant of Geff, our measurement of the velocity dispersion can place a tight constraint of 0.88 < Geff/GN < 1.29, (68 per cent) at length-scales of a few Mpc about 2.5 Giga years ago, where GN is the Newton's constant. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.Note
Immediate accessISSN
0035-8711Version
Final published versionae974a485f413a2113503eed53cd6c53
10.1093/mnras/stab1961