The ellipticity of galaxy cluster haloes from satellite galaxies and weak lensing

Shin, Tae-hyeon; Clampitt, Joseph; Jain, Bhuvnesh; Bernstein, Gary; Neil, Andrew; Rozo, Eduardo; Rykoff, Eli

doi:10.1093/mnras/stx3366

Title: The ellipticity of galaxy cluster haloes from satellite galaxies and weak lensing

Journal Article · Thu Jan 04 00:00:00 EST 2018 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stx3366· OSTI ID:1436107

^[1]; Clampitt, Joseph ^[1]; Jain, Bhuvnesh ^[1]; Bernstein, Gary ^[1]; Neil, Andrew ^[2]; Rozo, Eduardo ^[3]; Rykoff, Eli ^[4]

Univ. of Pennsylvania, Philadelphia, PA (United States)
Univ. of Pennsylvania, Philadelphia, PA (United States); Univ. of Chicago, Chicago, IL (United States)
Univ. of Arizona, Tucson, AZ (United States)
SLAC National Accelerator Lab., Menlo Park, CA (United States)

Here, we study the ellipticity of galaxy cluster haloes as characterized by the distribution of cluster galaxies and as measured with weak lensing. We use Monte Carlo simulations of elliptical cluster density profiles to estimate and correct for Poisson noise bias, edge bias and projection effects. We apply our methodology to 10 428 Sloan Digital Sky Survey clusters identified by the redMaPPer algorithm with richness above 20. We find a mean ellipticity =0.271 ± 0.002 (stat) ±0.031 (sys) corresponding to an axis ratio = 0.573 ± 0.002 (stat) ±0.039 (sys). We compare this ellipticity of the satellites to the halo shape, through a stacked lensing measurement using optimal estimators of the lensing quadrupole based on Clampitt and Jain (2016). We find a best-fitting axis ratio of 0.56 ± 0.09 (stat) ±0.03 (sys), consistent with the ellipticity of the satellite distribution. Thus, cluster galaxies trace the shape of the dark matter halo to within our estimated uncertainties. Finally, we restack the satellite and lensing ellipticity measurements along the major axis of the cluster central galaxy's light distribution. From the lensing measurements, we infer a misalignment angle with an root-mean-square of 30° ± 10° when stacking on the central galaxy. We discuss applications of halo shape measurements to test the effects of the baryonic gas and active galactic nucleus feedback, as well as dark matter and gravity. The major improvements in signal-to-noise ratio expected with the ongoing Dark Energy Survey and future surveys from Large Synoptic Survey Telescope, Euclid, and Wide Field Infrared Survey Telescope will make halo shapes a useful probe of these effects.

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Research Organization:: SLAC National Accelerator Lab., Menlo Park, CA (United States)

Sponsoring Organization:: USDOE

Grant/Contract Number:: AC02-76SF00515

OSTI ID:: 1436107

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 475, Issue 2; ISSN 0035-8711

Publisher:: Royal Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 29 works

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