Journal
PHYSICAL REVIEW D
Volume 93, Issue 8, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.93.082002
Keywords
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Funding
- U.S. National Science Foundation (NSF) [AST-0408698, AST-0965625, PHY-0855887, PHY-1214379]
- Princeton University
- University of Pennsylvania
- Cornell University
- Canada Foundation for Innovation (CFI)
- Comision Nacional de Investigacion Cientifica y Tecnologica de Chile (CONICYT)
- CFI under the auspices of Compute Canada
- Government of Ontario
- Ontario Research Fund Research Excellence
- University of Toronto
- Mishrahi Fund
- Wilkinson Fund
- NSF [AST1311756, AST1517593, AST1412966, AST-1454881, AST-1517049]
- NASA [NNXI2AG72G, 12-EUCLID11-0004, NNX13AE56G, NNX14AB58G, NNX12AM32H, ATP NNX14AB57G]
- Government of Canada through Industry Canada
- Province of Ontario through the Ministry of Research and Innovation
- NSERC Discovery grant
- DOE-ASC [DOE-DESC001114]
- Lyman Spitzer fellowship
- ERC [259505]
- DOE [DE-SC0011114]
- NASA Space Technology research fellowships
- CONICYT [QUIMAL-120001, FONDECYT-1141113]
- Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]
- Alfred P. Sloan Foundation
- National Science Foundation
- U.S. Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Institute de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- [AST-1312991]
- NASA [69674, NNX12AM32H] Funding Source: Federal RePORTER
- ESRC [ES/N013956/1] Funding Source: UKRI
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1311756] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1312380, 1517049, 1440226] Funding Source: National Science Foundation
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We use microwave temperature maps from two seasons of data from the Atacama Cosmology Telescope at 146 GHz, together with the Constant Mass CMASS galaxy sample from the Baryon Oscillation Spectroscopic Survey to measure the kinematic Sunyaev-Zel'dovich (kSZ) effect over the redshift range z = 0.4-0.7. We use galaxy positions and the continuity equation to obtain a reconstruction of the line-of-sight velocity field. We stack the microwave temperature at the location of each halo, weighted by the corresponding reconstructed velocity. We vary the size of the aperture photometry filter used, thus probing the free electron profile of these halos from within the virial radius out to three virial radii, on the scales relevant for investigating the missing baryons problem. The resulting best fit kSZ model is preferred over the no-kSZ hypothesis at 3.3 and 2.9 sigma for two independent velocity reconstruction methods, using 25,537 galaxies over 660 square degrees. The data suggest that the baryon profile is shallower than the dark matter in the inner regions of the halos probed here, potentially due to energy injection from active galactic nucleus or supernovae. Thus, by constraining the gas profile on a wide range of scales, this technique will be useful for understanding the role of feedback in galaxy groups and clusters. The effect of foregrounds that are uncorrelated with the galaxy velocities is expected to be well below our signal, and residual thermal Sunyaev-Zel'dovich contamination is controlled by masking the most massive clusters. Finally, we discuss the systematics involved in converting our measurement of the kSZ amplitude into the mean free electron fraction of the halos in our sample.
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