Journal article
Cross-correlation of CMB Polarization Lensing with High-z Submillimeter Herschel-ATLAS Galaxies
M Aguilar Faúndez, K Arnold, C Baccigalupi, D Barron, D Beck, F Bianchini, D Boettger, J Borrill, J Carron, K Cheung, Y Chinone, H El Bouhargani, T Elleflot, J Errard, G Fabbian, C Feng, N Galitzki, N Goeckner-Wald, M Hasegawa, M Hazumi Show all
The Astrophysical Journal | American Astronomical Society | Published : 2019
Abstract
We report a 4.8σ 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 galaxies of the Herschel-ATLAS survey. This is the first measurement of its kind.
Related Projects (2)
Grants
Awarded by Horizon 2020 Framework Programme
Funding Acknowledgements
The POLARBEAR project is funded by the National Science Foundation under Grants No. AST-0618398 and No. AST-1212230. The James Ax Observatory operates in the Parque Astronomico Atacama in Northern Chile under the auspices of the Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT). Work at the University of Melbourne is supported by an Australian Research Council's Future Fellowship (FT150100074). This research was supported in part by the RADIOFOREGROUNDS project, funded by the European Commissions H2020 Research Infrastructures under the Grant Agreement 687312, and by the ASI-COSMOS Network of the Italian Space Agency (cosmosnet.it). We also acknowledge support by the INDARK INFN Initiative. G.F. acknowledges the support of the CNES postdoctoral fellowship. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement No. [616170]. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC0205CH11231. M.A. acknowledges support from CONICYT UC Berkeley-Chile Seed Grant (CLAS fund) Number 77047, Fondecyt project 1130777 and 1171811, DFI postgraduate scholarship program and DFI Postgraduate Competitive Fund for Support in the Attendance to Scientific Events. B.K. acknowledges support from the Ax Center for Experimental Cosmology. Y.C. acknowledges the World Premier International Research Center Initiative (WPI), MEXT, Japan and support from the JSPS KAKENHI grant Nos. 18K13558, 18H04347. F.M. acknowledges the support by the World Premier International Research Center Initiative (WPI), MEXT, Japan and JSPS fellowship (Grant number JP17F17025). A.K. acknowledges the support by JSPS Leading Initiative for Excellent Young Researchers (LEADER) and by the JSPS KAKENHI grant No. JP16K21744. Work at LBNL is supported in part by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under contract No. DE-AC02-05CH11231. This work was supported by MEXT KAKENHI grant Nos. 21111002 and JP15H05891, JSPS KAKENHI grant Nos. JP26220709, JP26800125, and JP18H05539, and the JSPS Core-toCore Program. The APC group acknowledges travel support from Labex Univearths. We acknowledge the use of many python packages: IPYTHON (Perez and Granger 2007), MATPLOTLIB (Hunter 2007), SCIPY (Virtanen et al. 20019), SURVEYVISUALIZER.<SUP>31</SUP>