Measuring cosmic filament spin with the kinetic Sunyaev-Zel’dovich effect

作     者：Zheng, Yi Cai, Yan-Chuan Zhu, Weishan Neyrinck, Mark Wang, Peng Li, Shaohong 

作者机构：School of Physics and Astronomy Sun Yat-sen University 2 Daxue Road Tangjia Zhuhai519082 China CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area SYSU China  Shanghai Key Laboratory for Particle Physics and Cosmology China Scottish Universities Physics Alliance Institute for Astronomy University of Edinburgh Blackford Hill United Kingdom Ikerbasque The Basque Foundation for Science Bilbao48009 Spain Department of Physics University of the Basque Country UPV/EHU Bilbao48080 Spain Donostia International Physics Center Paseo Manuel Lardizabal 3 San Sebastián20018 Spain Shanghai Astronomical Observatory CAS Nandan Road 80 Shanghai200030 China Key Laboratory for Research in Galaxies and Cosmology SHAO CAS Nandan Road 80 Shanghai200030 China 

出 版 物：《arXiv》 (arXiv)

年 卷 期：2022年

核心收录：

主　　题：Red Shift 

摘      要：The spin of intergalactic filaments has been predicted from simulations, and supported by tentative evidence from redshift-space filament shapes in a galaxy redshift survey: generally, a filament is redshifted on one side of its axis, and blueshifted on the other. Here, we investigate whether filament spins could have a measurable kinetic Sunyaev-Zel’dovich (kSZ) signal, from CMB photons being scattered by moving ionised gas;this pure velocity information is complementary to filament redshift-space shapes. We propose to measure the kSZ dipole by combining galaxy redshift surveys with CMB experiments. We base our S/N analyses first on an existing filament catalogue, and its combination with Planck data. We then investigate the detectability of the kSZ dipole using the combination of DESI or SKA-2 with next-stage CMB experiments. We find that the gas halos of filament galaxies co-rotating with filaments induce a stronger kSZ dipole signal than that from the diffuse filamentary gas, but both signals seem too small to be detected in near-term surveys such as DESI+future CMB experiments. But the combination of SKA-2 with future CMB experiments could give a more than 10σ detection. The gain comes mainly from an increased area overlap and an increased number of filaments, but also the low noise and high resolution in future CMB experiments are important to capture signals from filaments small on the sky. Successful detection of the signals may help to find the gravitomagnetic effect in large-scale structure and advance our understanding of baryons in the cosmic web. Copyright © 2022, The Authors. All rights reserved.