Cross-correlation between Subaru Hyper Suprime-Cam Galaxy Weak Lensing and Planck Cosmic Microwave Background Lensing

Abstract

Cross-correlations between galaxy weak lensing (WL) and cosmic microwave background (CMB) lensing are powerful tools to probe matter fluctuations at intermediate redshifts and to detect residual systematics in either probe. In this paper, we study the cross-correlation of galaxy WL from the Hyper Suprime-Cam Subaru Strategic Program (HSC) first data release and CMB lensing from the final Planck data release, for HSC source galaxies at 0.3 ≤ z ≤ 1.5. HSC is the deepest Stage-III galaxy WL survey, and provides a great opportunity to study the high-redshift universe. It also presents new challenges related to its exceptionally high source density, such as source blending. The cross-correlation signal is measured at a significance level of 3.1σ. The amplitude of our best-fit model with respect to the best-fit 2018 Planck cosmology is A = 0.81 ± 0.25, consistent with A = 1. Our result is also consistent with previous CMB lensing and galaxy WL cross-correlation studies using different surveys. We perform tests with respect to the WL B-modes, the point-spread-function, photometric redshift errors, and thermal Sunyaev–Zel’dovich leakage, and find no significant evidence of residual systematics.

The growth of density perturbations in the last $\sim$10 billion years from tomographic large-scale structure data

“…The map covers a sky fraction f sky = 0.671 and thus overlaps spatially with all surveys considered here. Various photometric redshift surveys have made use of cross-correlations with CMB lensing maps from different collaborations to extract cosmological constraints [7,19,28,[60][61][62][63].…”

Joint analysis of DES Year 3 data and CMB lensing from SPT and Planck II: Cross-correlation measurements and cosmological constraints

“…Similar analyses have recently been carried out using different galaxy imaging surveys and CMB data. [19] studied the cross-correlation of the galaxy weak lensing from the Hyper Suprime-Cam Subaru Strategic Program Survey [HSC-SSP, 20] and the Planck lensing map [21]; [22] used the same HSC galaxy weak lensing measurement to cross-correlate with CMB lensing from the PO-LARBEAR experiment [23]; [24] cross-correlated galaxy weak lensing from the Kilo-Degree Survey [KiDS,25] and the CMB lensing map from the Atacama Cosmology Telescope [ACT,26]; and [27] cross-correlated the galaxy density measured in unWISE data [28] with Planck CMB lensing. Compared to these previous studies, in addition to the new datasets, this paper is unique in that we combine δ g κ CMB and γ t κ CMB .…”

Strong detection of the CMB lensing and galaxy weak lensing cross-correlation from ACT-DR4,PlanckLegacy, and KiDS-1000

“…The first measurement of this kind combined the CMB lensing data from the Atacama Cosmology Telescope (ACT) with galaxy weak lensing data from the Canada-France-Hawaii Telescope Stripe 82 Survey (CS82, Hand et al 2015). There have been several subsequent measurements using the Canada-France Hawaii Telescope Lensing Survey, Red Cluster Survey Lensing, Kilo Degree Survey (KiDS), Dark Energy Survey, or Hyper Suprime-Cam galaxy weak lensing surveys combined with the Planck, ACT, South Pole Telescope or POLARBEAR CMB lensing data (Liu & Hill 2015;Kirk et al 2016;Harnois-Déraps et al 2016Miyatake et al 2017;Omori et al 2019b;Namikawa et al 2019;Marques et al 2020). Little improvement in the signal-to-noise ratio (S/N) has been observed between these measurements, mostly due either to the small overlapping area between the data sets or to the large residual noise in the CMB lensing maps; both considerations presently limit the achieved S/N.…”

“…For the current generation of low S/N measurements, it is common to compress the cross-correlation measurement into an estimation of a single amplitude parameter A, which is equal to unity if the data are consistent with a ΛCDM model at a chosen cosmology. For these previous measurements, the amplitude A was calibrated on the Planck best-fit cosmology, and while some were consistent with A = 1.0 (Kirk et al 2016;Marques et al 2020), others found an amplitude lower than expected (Hand et al 2015;Liu & Hill 2015;Harnois-Déraps et al 2016. There has been some discussion about whether this could be caused by the effect of intrinsic alignment of galaxies (Hall & Taylor 2014;Chisari et al 2015;Larsen & Challinor 2016), which can imitate and conceal the true lensing signal (see Kirk et al 2015, and references therein).…”