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We report a highly significant ($>10sigma$) spatial correlation between galaxies with $S_{350murm m}ge 30,$mJy detected in the equatorial fields of the textsl{Herschel} Astrophysical Terahertz Large Area Survey (H-ATLAS) with estimated redshifts $gtrsim 1.5$, and SDSS or GAMA galaxies at $0.2le zle 0.6$. The significance of the cross-correlation is much higher than those reported so far for samples with non-overlapping redshift distributions selected in other wavebands. Extensive, realistic simulations of clustered sub-mm galaxies amplified by foreground structures confirm that the cross-correlation is explained by weak gravitational lensing ($mu<2$). The simulations also show that the measured amplitude and range of angular scales of the signal are larger than can be accounted for by galaxy-galaxy weak lensing. However, for scales $lesssim 2,$arcmin, the signal can be reproduced if SDSS/GAMA galaxies act as signposts of galaxy groups/clusters with halo masses in the range $10^{13.2}$--$10^{14.5} M_{odot}$. The signal detected on larger scales appears to reflect the clustering of such halos.
We report a 4.8$sigma$ measurement of the cross-correlation signal between the cosmic microwave background (CMB) lensing convergence reconstructed from measurements of the CMB polarization made by the POLARBEAR experiment and the infrared-selected ga
We present the first measurement of the correlation between the map of the cosmic microwave background (CMB) lensing potential derived from the emph{Planck} nominal mission data and $zgtrsim 1.5$ galaxies detected by the emph{Herschel}-ATLAS (H-ATLAS
This is the first in a series of papers on the weak lensing effect caused by clusters of galaxies in Sloan Digital Sky Survey. The photometrically selected cluster sample, known as MaxBCG, includes ~130,000 objects between redshift 0.1 and 0.3, rangi
Recent studies have demonstrated that {em secondary} non-Gaussianity induced by gravity will be detected with a high signal-to-noise (S/N) by future and even by on-going weak lensing surveys. One way to characterise such non-Gaussianity is through th
We have constructed a sample of radio-loud objects with optical spectroscopy from the Galaxy and Mass Assembly (GAMA) project over the Herschel-ATLAS Phase 1 fields. Classifying the radio sources in terms of their optical spectra, we find that strong