On the halo-mass and radial scale dependence of the lensing is low effect

• Published in: arXiv.org
• Main Authors: Lange, Johannes U, Leauthaud, Alexie, Singh, Sukhdeep, Guo, Hong, Zhou, Rongpu, Smith, Tristan L, Francis-Yan Cyr-Racine
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 26.01.2021
• Subjects: Amplitudes; Astronomical models; Baryons; Clustering; Constraints; Cosmic microwave background; Cosmology; Dependence; Galaxies; Physics - Astrophysics of Galaxies; Physics - Cosmology and Nongalactic Astrophysics; Red shift; Sky surveys (astronomy); Stellar mass
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2011.02377

The canonical \(\Lambda\)CDM cosmological model makes precise predictions for the clustering and lensing properties of galaxies. It has been shown that the lensing amplitude of galaxies in the Baryon Oscillation Spectroscopic Survey (BOSS) is lower than expected given their clustering properties. We present new measurements and modelling of galaxies in the BOSS LOWZ sample. We focus on the radial and stellar mass dependence of the lensing amplitude mis-match. We find an amplitude mis-match of around \(35\%\) when assuming \(\Lambda\)CDM with Planck Cosmological Microwave Background (CMB) constraints. This offset is independent of halo mass and radial scale in the range \(M_{\rm halo}\sim 10^{13.3} - 10^{13.9} h^{-1} M_\odot\) and \(r=0.1 - 60 \, h^{-1} \mathrm{Mpc}\) (\(k \approx 0.05 - 20 \, h \, {\rm Mpc}^{-1}\)). The observation that the offset is both mass and scale independent places important constraints on the degree to which astrophysical processes (baryonic effects, assembly bias) can fully explain the effect. This scale independence also suggests that the "lensing is low" effect on small and large radial scales probably have the same physical origin. Resolutions based on new physics require a nearly uniform suppression, relative to \(\Lambda\)CDM predictions, of the amplitude of matter fluctuations on these scales. The possible causes of this are tightly constrained by measurements of the CMB and of the low-redshift expansion history.