A Cosmic Microwave Background Lensing Mass Map and Its Correlation with the Cosmic Infrared Background

• Published in: The Astrophysical Journal
• Main Authors: Holder, G. P., Viero, M. P., Bock, J., Lueker, M., Padin, S., Schulz, B., Vieira, J. D., Zemcov, M.
• Format: Article in Journal/Newspaper
• Language: unknown
• Published: American Astronomical Society 2013
• Subjects: cosmic background radiation; galaxies: structure; Canada; Hubble; Kavli; South Pole; South pole
• Online Access: https://doi.org/10.1088/2041-8205/771/1/L16

We use a temperature map of the cosmic microwave background (CMB) obtained using the South Pole Telescope at 150 GHz to construct a map of the gravitational convergence to z ~ 1100, revealing the fluctuations in the projected mass density. This map shows individual features that are significant at the ~4σ level, providing the first image of CMB lensing convergence. We cross-correlate this map with Herschel/SPIRE maps covering 90 deg2 at wavelengths of 500, 350, and 250 μm. We show that these submillimeter (submm) wavelength maps are strongly correlated with the lensing convergence map, with detection significances in each of the three submm bands ranging from 6.7σ to 8.8σ. We fit the measurement of the cross power spectrum assuming a simple constant bias model and infer bias factors of b = 1.3-1.8, with a statistical uncertainty of 15%, depending on the assumed model for the redshift distribution of the dusty galaxies that are contributing to the Herschel/SPIRE maps. © 2013 American Astronomical Society. Received 2013 March 28; accepted 2013 June 5; published 2013 June 19. The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support provided by NSF grant PHY-1125897, the Kavli Foundation, and the Gordon and Betty Moore Foundation. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. Work at Harvard is supported by grant AST-1009012. S. Bhattacharya acknowledges support from NSF grant AST-1009811, R.Keisler from NASA Hubble Fellowship grant HF-51275.01, B. Benson from a KICP Fellowship, M. Dobbs from an Alfred P. Sloan Research Fellowship, and O. Zahn from a BCCP fellowship. Published - 2041-8205_771_1_L16.pdf Submitted - 1303.5048v1.pdf